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Sample records for intrinsic ellipticity correlation

  1. SELF-CALIBRATION OF GRAVITATIONAL SHEAR-GALAXY INTRINSIC ELLIPTICITY CORRELATION IN WEAK LENSING SURVEYS

    SciTech Connect

    Zhang Pengjie

    2010-09-10

    The galaxy intrinsic alignment is a severe challenge to precision cosmic shear measurement. We propose self-calibrating the induced gravitational shear-galaxy intrinsic ellipticity correlation (the GI correlation) in weak lensing surveys with photometric redshift measurements. (1) We propose a method to extract the intrinsic ellipticity-galaxy density cross-correlation (I-g) from the galaxy ellipticity-density measurement in the same redshift bin. (2) We also find a generic scaling relation to convert the extracted I-g correlation to the necessary GI correlation. We perform a concept study under simplified conditions and demonstrate its capability to significantly reduce GI contamination. We discuss the impact of various complexities on the two key ingredients of the self-calibration technique, namely the method for extracting the I-g correlation and the scaling relation between the I-g and the GI correlation. We expect that none of them will likely be able to completely invalidate the proposed self-calibration technique.

  2. The correlation function of galaxy ellipticities produced by gravitational lensing

    NASA Technical Reports Server (NTRS)

    Miralda-Escude, Jordi

    1991-01-01

    The correlation of galaxy ellipticities produced by gravitational lensing is calculated as a function of the power spectrum of density fluctuations in the universe by generalizing an analytical method developed by Gunn (1967). The method is applied to a model where identical objects with spherically symmetric density profiles are randomly laid down in space, and to the cold dark matter model. The possibility of detecting this correlation is discussed. Although an ellipticity correlation can also be caused by an intrinsic alignment of the axes of galaxies belonging to a cluster or a supercluster, a method is suggested by which one type of correlation can be distinguished from another. The advantage of this ellipticity correlation is that it is one of the few astronomical observations that can directly probe large-scale mass fluctuations in the universe.

  3. Intrinsic galaxy shapes and alignments - I. Measuring and modelling COSMOS intrinsic galaxy ellipticities

    NASA Astrophysics Data System (ADS)

    Joachimi, B.; Semboloni, E.; Bett, P. E.; Hartlap, J.; Hilbert, S.; Hoekstra, H.; Schneider, P.; Schrabback, T.

    2013-05-01

    The statistical properties of the ellipticities of galaxy images depend on how galaxies form and evolve, and therefore constrain models of galaxy morphology, which are key to the removal of the intrinsic alignment contamination of cosmological weak lensing surveys, as well as to the calibration of weak lensing shape measurements. We construct such models based on the halo properties of the Millennium Simulation and confront them with a sample of 90 000 galaxies from the COSMOS Survey, covering three decades in luminosity and redshifts out to z = 2. The ellipticity measurements are corrected for effects of point spread function smearing, spurious image distortions and measurement noise. Dividing galaxies into early, late and irregular types, we find that early-type galaxies have up to a factor of 2 lower intrinsic ellipticity dispersion than late-type galaxies. None of the samples shows evidence for redshift evolution, while the ellipticity dispersion for late-type galaxies scales strongly with absolute magnitude at the bright end. The simulation-based models reproduce the main characteristics of the intrinsic ellipticity distributions although which model fares best depends on the selection criteria of the galaxy sample. We observe fewer close-to-circular late-type galaxy images in COSMOS than expected for a sample of randomly oriented circular thick discs and discuss possible explanations for this deficit.

  4. Elliptical Laguerre-Gaussian correlated Schell-model beam.

    PubMed

    Chen, Yahong; Liu, Lin; Wang, Fei; Zhao, Chengliang; Cai, Yangjian

    2014-06-02

    A new kind of partially coherent beam with non-conventional correlation function named elliptical Laguerre-Gaussian correlated Schell-model (LGCSM) beam is introduced. Analytical propagation formula for an elliptical LGCSM beam passing through a stigmatic ABCD optical system is derived. The elliptical LGCSM beam exhibits unique features on propagation, e.g., its intensity in the far field (or in the focal plane) displays an elliptical ring-shaped beam profile, being qualitatively different from the circular ring-shaped beam profile of the circular LGCSM beam. Furthermore, we carry out experimental generation of an elliptical LGCSM beam with controllable ellipticity, and measure its focusing properties. Our experimental results are consistent with the theoretical predictions. The elliptical LGCSM beam will be useful in atomic optics.

  5. A theoretical estimate of intrinsic ellipticity bispectra induced by angular momenta alignments

    NASA Astrophysics Data System (ADS)

    Merkel, Philipp M.; Schäfer, Björn Malte

    2014-12-01

    Intrinsically aligned galaxy shapes are one of the most important systematics in cosmic shear measurements. So far, theoretical studies of intrinsic alignments almost exclusively focus on their statistics at the two-point level. Results from numerical simulations, however, suggest that third-order measures might be even stronger affected. We therefore investigate the (angular) bispectrum of intrinsic alignments. In our fully analytical study, we describe intrinsic galaxy ellipticities by a physical alignment model, which makes use of tidal torque theory. We derive expressions for the various combinations of intrinsic and gravitationally induced ellipticities, i.e. III-, GII- and GGI-alignments, and compare our results to the shear bispectrum, the GGG-term. The latter is computed using hyperextended perturbation theory. Considering equilateral and squeezed configurations, we find that for a Euclid-like survey intrinsic alignments (III-alignments) start to dominate on angular scales smaller than 20 and 13 arcmin, respectively. This sensitivity to the configuration-space geometry may allow us to exploit the cosmological information contained in both the intrinsic and gravitationally induced ellipticity field. On smallest scales (ℓ ˜ 3000), III-alignments exceed the lensing signal by at least one order of magnitude. The amplitude of the GGI-alignments is the weakest. It stays below that of the shear field on all angular scales irrespective of the wavevector configuration.

  6. Intrinsic alignment contamination to CMB lensing-galaxy weak lensing correlations from tidal torquing

    NASA Astrophysics Data System (ADS)

    Larsen, Patricia; Challinor, Anthony

    2016-10-01

    Correlations of galaxy ellipticities with large-scale structure, due to galactic tidal interactions, provide a potentially significant contaminant to measurements of cosmic shear. However, these intrinsic alignments are still poorly understood for galaxies at the redshifts typically used in cosmic shear analyses. For spiral galaxies, it is thought that tidal torquing is significant in determining alignments resulting in zero correlation between the intrinsic ellipticity and the gravitational potential in linear theory. Here, we calculate the leading-order correction to this result in the tidal-torque model from non-linear evolution, using second-order perturbation theory, and relate this to the contamination from intrinsic alignments to the recently measured cross-correlation between galaxy ellipticities and the cosmic microwave background (CMB) lensing potential. On the scales relevant for CMB lensing observations, the squeezed limit of the gravitational bispectrum dominates the correlation. Physically, the large-scale mode that sources CMB lensing modulates the small-scale power and hence the intrinsic ellipticity, due to non-linear evolution. We find that the angular cross-correlation from tidal torquing has a very similar scale dependence as in the linear alignment model, believed to be appropriate for elliptical galaxies. The amplitude of the cross-correlation is predicted to depend strongly on the formation redshift, being smaller for galaxies that formed at higher redshift when the bispectrum of the gravitational potential was smaller. Finally, we make simple forecasts for constraints on intrinsic alignments from the correlation of forthcoming cosmic shear measurements with current CMB lensing measurements. We note that cosmic variance can be significantly reduced in measurements of the difference in the intrinsic alignments for elliptical and spiral galaxies if these types can be separated (e.g. using colour).

  7. Properties of Ellipticity Correlation with Atmospheric Structure from Gemini South

    SciTech Connect

    Asztalos, S J; Treadway, T; de Vries, W H; Rosenberg, L J; Burke, D; Claver, C; Saha, A; Puxley, P

    2006-12-21

    Cosmic shear holds great promise for a precision independent measurement of {Omega}{sub m}, the mass density of the universe relative to the critical density. The signal is expected to be weak, so a thorough understanding of systematic effects is crucial. An important systematic effect is the atmosphere: shear power introduced by the atmosphere is larger than the expected signal. Algorithms exist to extract the cosmic shear from the atmospheric component, though a measure of their success applied to a range of seeing conditions is lacking. To gain insight into atmospheric shear, Gemini South imaging in conjunction with ground condition and satellite wind data were obtained. We find that under good seeing conditions Point-Spread-Function (PSF) correlations persist well beyond the separation typical of high-latitude stars. Under these conditions, ellipticity residuals based on a simple PSF interpolation can be reduced to within a factor of a few of the shot-noise induced ellipticity floor. We also find that the ellipticity residuals are highly correlated with wind direction. Finally, we correct stellar shapes using a more sophisticated procedure and generate shear statistics from stars. Under all seeing conditions in our data set the residual correlations lie everywhere below the target signal level. For good seeing we find that the systematic error attributable to atmospheric turbulence is comparable in magnitude to the statistical error (shape noise) over angular scales relevant to present lensing surveys.

  8. Properties of Ellipticity Correlation with Atmospheric Structure From Gemini South

    SciTech Connect

    Asztalos, Stephen J.; de Vries, W.H.; Rosenberg, L.J; Treadway, T.; Burke, D.; Claver, C.; Saha, A.; Puxley, P.; /Gemini Observ., La Serena

    2007-01-17

    Cosmic shear holds great promise for a precision independent measurement of {Omega}{sub m}, the mass density of the universe relative to the critical density. The signal is expected to be weak, so a thorough understanding of systematic effects is crucial. An important systematic effect is the atmosphere: shear power introduced by the atmosphere is larger than the expected signal. Algorithms exist to extract the cosmic shear from the atmospheric component, though a measure of their success applied to a range of seeing conditions is lacking. To gain insight into atmospheric shear, Gemini South imaging in conjunction with ground condition and satellite wind data were obtained. We find that under good seeing conditions Point-Spread-Function (PSF) correlations persist well beyond the separation typical of high-latitude stars. Under these conditions, ellipticity residuals based on a simple PSF interpolation can be reduced to within a factor of a few of the shot-noise induced ellipticity floor. We also find that the ellipticity residuals are highly correlated with wind direction. Finally, we correct stellar shapes using a more sophisticated procedure and generate shear statistics from stars. Under all seeing conditions in our data set the residual correlations lie everywhere below the target signal level. For good seeing we find that the systematic error attributable to atmospheric turbulence is comparable in magnitude to the statistical error (shape noise) over angular scales relevant to present lensing surveys.

  9. Intrinsic Correlations for Flaring Blazars Detected by Fermi

    NASA Astrophysics Data System (ADS)

    Fan, J. H.; Yang, J. H.; Xiao, H. B.; Lin, C.; Constantin, D.; Luo, G. Y.; Pei, Z. Y.; Hao, J. M.; Mao, Y. W.

    2017-02-01

    Blazars are an extreme subclass of active galactic nuclei. Their rapid variability, luminous brightness, superluminal motion, and high and variable polarization are probably due to a beaming effect. However, this beaming factor (or Doppler factor) is very difficult to measure. Currently, a good way to estimate it is to use the timescale of their radio flares. In this Letter, we use multiwavelength data and Doppler factors reported in the literature for a sample of 86 flaring blazars detected by Fermi to compute their intrinsic multiwavelength data and intrinsic spectral energy distributions and investigate the correlations among observed and intrinsic data. Quite interestingly, intrinsic data show a positive correlation between luminosity and peak frequency, in contrast with the behavior of observed data, and a tighter correlation between γ-ray luminosity and the lower-energy ones. For flaring blazars detected by Fermi, we conclude that (1) observed emissions are strongly beamed; (2) the anti-correlation between luminosity and peak frequency from the observed data is an apparent result, the correlation between intrinsic data being positive; and (3) intrinsic γ-ray luminosity is strongly correlated with other intrinsic luminosities.

  10. The anisotropic Ising correlations as elliptic integrals: duality and differential equations

    NASA Astrophysics Data System (ADS)

    McCoy, B. M.; Maillard, J.-M.

    2016-10-01

    We present the reduction of the correlation functions of the Ising model on the anisotropic square lattice to complete elliptic integrals of the first, second and third kind, the extension of Kramers-Wannier duality to anisotropic correlation functions, and the linear differential equations for these anisotropic correlations. More precisely, we show that the anisotropic correlation functions are homogeneous polynomials of the complete elliptic integrals of the first, second and third kind. We give the exact dual transformation matching the correlation functions and the dual correlation functions. We show that the linear differential operators annihilating the general two-point correlation functions are factorized in a very simple way, in operators of decreasing orders. Dedicated to A J Guttmann, for his 70th birthday.

  11. Characterizing the intrinsic correlations of scale-free networks

    NASA Astrophysics Data System (ADS)

    de Brito, J. B.; Sampaio Filho, C. I. N.; Moreira, A. A.; Andrade, J. S.

    2016-08-01

    When studying topological or dynamical properties of random scale-free networks, it is tacitly assumed that degree-degree correlations are not present. However, simple constraints, such as the absence of multiple edges and self-loops, can give rise to intrinsic correlations in these structures. In the same way that Fermionic correlations in thermodynamic systems are relevant only in the limit of low temperature, the intrinsic correlations in scale-free networks are relevant only when the extreme values for the degrees grow faster than the square root of the network size. In this situation, these correlations can significantly affect the dependence of the average degree of the nearest neighbors of a given vertex on this vertices degree. Here, we introduce an analytical approach that is capable to predict the functional form of this property. Moreover, our results indicate that random scale-free network models are not self-averaging, that is, the second moment of their degree distribution may vary orders of magnitude among different realizations. Finally, we argue that the intrinsic correlations investigated here may have profound impact on the critical properties of random scale-free networks.

  12. Inhibitory control of correlated intrinsic variability in cortical networks

    PubMed Central

    Stringer, Carsen; Pachitariu, Marius; Steinmetz, Nicholas A; Okun, Michael; Bartho, Peter; Harris, Kenneth D; Sahani, Maneesh; Lesica, Nicholas A

    2016-01-01

    Cortical networks exhibit intrinsic dynamics that drive coordinated, large-scale fluctuations across neuronal populations and create noise correlations that impact sensory coding. To investigate the network-level mechanisms that underlie these dynamics, we developed novel computational techniques to fit a deterministic spiking network model directly to multi-neuron recordings from different rodent species, sensory modalities, and behavioral states. The model generated correlated variability without external noise and accurately reproduced the diverse activity patterns in our recordings. Analysis of the model parameters suggested that differences in noise correlations across recordings were due primarily to differences in the strength of feedback inhibition. Further analysis of our recordings confirmed that putative inhibitory neurons were indeed more active during desynchronized cortical states with weak noise correlations. Our results demonstrate that network models with intrinsically-generated variability can accurately reproduce the activity patterns observed in multi-neuron recordings and suggest that inhibition modulates the interactions between intrinsic dynamics and sensory inputs to control the strength of noise correlations. DOI: http://dx.doi.org/10.7554/eLife.19695.001 PMID:27926356

  13. Clique topology reveals intrinsic geometric structure in neural correlations.

    PubMed

    Giusti, Chad; Pastalkova, Eva; Curto, Carina; Itskov, Vladimir

    2015-11-03

    Detecting meaningful structure in neural activity and connectivity data is challenging in the presence of hidden nonlinearities, where traditional eigenvalue-based methods may be misleading. We introduce a novel approach to matrix analysis, called clique topology, that extracts features of the data invariant under nonlinear monotone transformations. These features can be used to detect both random and geometric structure, and depend only on the relative ordering of matrix entries. We then analyzed the activity of pyramidal neurons in rat hippocampus, recorded while the animal was exploring a 2D environment, and confirmed that our method is able to detect geometric organization using only the intrinsic pattern of neural correlations. Remarkably, we found similar results during nonspatial behaviors such as wheel running and rapid eye movement (REM) sleep. This suggests that the geometric structure of correlations is shaped by the underlying hippocampal circuits and is not merely a consequence of position coding. We propose that clique topology is a powerful new tool for matrix analysis in biological settings, where the relationship of observed quantities to more meaningful variables is often nonlinear and unknown.

  14. Modelling the impact of intrinsic size and luminosity correlations on magnification estimation

    NASA Astrophysics Data System (ADS)

    Ciarlariello, Sandro; Crittenden, Robert

    2016-11-01

    Spatial correlations of the observed sizes and luminosities of galaxies can be used to estimate the magnification that arises through weak gravitational lensing. However, the intrinsic properties of galaxies can be similarly correlated through local physical effects, and these present a possible contamination to the weak lensing estimation. In an earlier paper we modelled the intrinsic size correlations using the halo model, assuming the galaxy sizes reflect the mass in the associated halo. Here we extend this work to consider galaxy magnitudes and show that these may be even more affected by intrinsic correlations than galaxy sizes, making this a bigger systematic for measurements of the weak lensing signal. We also quantify how these intrinsic correlations are affected by sample selection criteria based on sizes and magnitudes.

  15. Opposing Effects of Intrinsic Conductance and Correlated Synaptic Input on Vm-Fluctuations during Network Activity

    PubMed Central

    Kolind, Jens; Hounsgaard, Jørn; Berg, Rune W.

    2012-01-01

    Neurons often receive massive concurrent bombardment of synaptic inhibition and excitation during functional network activity. This increases membrane conductance and causes fluctuations in membrane potential (Vm) and spike timing. The conductance increase is commonly attributed to synaptic conductance, but also includes the intrinsic conductances recruited during network activity. These two sources of conductance have contrasting dynamic properties at sub-threshold membrane potentials. Synaptic transmitter gated conductance changes abruptly and briefly with each presynaptic action potential. If the spikes arrive at random times the changes in synaptic conductance are therefore stochastic and rapid during intense network activity. In comparison, sub-threshold intrinsic conductances vary smoothly in time. In the present study this discrepancy is investigated using two conductance-based models: a (1) compartment model and a (2) compartment with realistic slow intrinsic conductances. We examine the effects of varying the relative contributions of non-fluctuating intrinsic conductance with fluctuating concurrent inhibitory and excitatory synaptic conductance. For given levels of correlation in the synaptic input we find that the magnitude of the membrane fluctuations uniquely determines the relative contribution of synaptic and intrinsic conductance. We also quantify how Vm-fluctuations vary with synaptic correlations for fixed ratios of synaptic and intrinsic conductance. Interestingly, the levels of Vm -fluctuations and conductance observed experimentally during functional network activity leave little room for intrinsic conductance to contribute. Even without intrinsic conductances the variance in Vm -fluctuations can only be explained by a high degree of correlated firing among presynaptic neurons. PMID:22783184

  16. THE L{proportional_to}{sigma}{sup 8} CORRELATION FOR ELLIPTICAL GALAXIES WITH CORES: RELATION WITH BLACK HOLE MASS

    SciTech Connect

    Kormendy, John; Bender, Ralf E-mail: bender@mpe.mpg.de

    2013-05-20

    We construct the Faber-Jackson correlation between velocity dispersion {sigma} and total galaxy luminosity L{sub V} separately for elliptical galaxies with and without cores. The coreless ellipticals show the well-known, steep relationship dlog {sigma}/dlog L{sub V} = 0.268 or L{sub V} {proportional_to}{sigma}{sup 3.74}. This corresponds to dlog {sigma}/dlog M = 0.203, where M is the stellar mass and we use M/L{proportional_to}L {sup 0.32}. In contrast, the velocity dispersions of core ellipticals increase much more slowly with L{sub V} and M: dlog {sigma}/dlog L{sub V} = 0.120, L{sub V} {proportional_to}{sigma}{sup 8.33}, and dlog {sigma}/dlog M = 0.091. Dissipationless major galaxy mergers are expected to preserve {sigma} according to the simplest virial-theorem arguments. However, numerical simulations show that {sigma} increases slowly in dry major mergers, with dlog {sigma}/dlog M {approx_equal} +0.15. In contrast, minor mergers cause {sigma} to decrease, with dlog {sigma}/dlog M {approx_equal} -0.05. Thus, the observed relation argues for dry major mergers as the dominant growth mode of the most massive ellipticals. This is consistent with what we know about the formation of cores. We know no viable way to explain galaxy cores except through dissipationless mergers of approximately equal-mass galaxies followed by core scouring by binary supermassive black holes. The observed, shallow {sigma}{proportional_to}L{sub V}{sup +0.12} relation for core ellipticals provides further evidence that they formed in dissipationless and predominantly major mergers. Also, it explains the observation that the correlation of supermassive black hole mass with velocity dispersion, M{sub .}{proportional_to}{sigma}{sup 4}, ''saturates'' at high M{sub .} such that M{sub .} becomes almost independent of {sigma}.

  17. Ellipticities of Elliptical Galaxies in Different Environments

    NASA Astrophysics Data System (ADS)

    Chen, Cheng-Yu; Hwang, Chorng-Yuan; Ko, Chung-Ming

    2016-10-01

    We studied the ellipticity distributions of elliptical galaxies in different environments. From the ninth data release of the Sloan Digital Sky Survey, we selected galaxies with absolute {r}\\prime -band magnitudes between -21 and -22. We used the volume number densities of galaxies as the criterion for selecting the environments of the galaxies. Our samples were divided into three groups with different volume number densities. The ellipticity distributions of the elliptical galaxies differed considerably in these three groups of different density regions. We deprojected the observed 2D ellipticity distributions into intrinsic 3D shape distributions, and the result showed that the shapes of the elliptical galaxies were relatively spherically symmetric in the high density region (HDR) and that relatively more flat galaxies were present in the low density region (LDR). This suggests that the ellipticals in the HDRs and LDRs have different origins or that different mechanisms might be involved. The elliptical galaxies in the LDR are likely to have evolved from mergers in relatively anisotropic structures, such as filaments and webs, and might contain information on the anisotropic spatial distribution of their parent mergers. By contrast, elliptical galaxies in the HDR might be formed in more isotropic structures, such as galaxy clusters, or they might encounter more torqueing effects compared with galaxies in LDRs, thereby becoming rounder.

  18. Variation in and correlation between intrinsic rate of increase and carrying capacity.

    PubMed

    Underwood, Nora

    2007-01-01

    Intrinsic population growth rate and density dependence are fundamental components of population dynamics. Theory suggests that variation in and correlations between these parameters among patches within a population can influence overall population size, but data on the degree of variation and correlation are rare. Replicate populations of a specialist aphid (Chaetosiphon fragaefolii) were followed on 11 genotypes of host plant (Fragaria chiloensis) in the greenhouse. Population models fit to these census data provide estimates of intrinsic growth rate and carrying capacity for aphid populations on each plant genotype. Growth rate and carrying capacity varied substantially among plant genotypes, and these two parameters were not significantly correlated. These results support the existence of spatial variation in population dynamic parameters; data on frequency distributions and correlations of these parameters in natural populations are needed for evaluation of the importance of variation in growth rate and density dependence for population dynamics in the field.

  19. Correlation between Intrinsic Patellofemoral Pain Syndrome in Young Adults and Lower Extremity Biomechanics.

    PubMed

    Kwon, Ohjeoung; Yun, Mijung; Lee, Wanhee

    2014-07-01

    [Purpose] The purpose of this study was to evaluate the correlation between intrinsic patellofemoral pain syndrome (PFPS) in young adults and lower extremity biomechanics. [Subjects] This experiment was carried out with sixty (24 men and 32 women), who are normal university students as subjects. [Methods] All subjects underwent 3 clinical evaluations. For distinguishing the intrinsic PFPS from controls, we used the Modified Functional Index Questionnaire (MFIQ), Clarke's test and the Eccentric step test. Based on the results of the tests, subjects who were classified as positive for 2 more tests were allocated to the bilateral or unilateral intrinsic PFPS group (n=14), and the others were allocated to the control group (n=42). These two groups were tested for hamstring tightness, foot overpronation, and static Q-angle and dynamic Q-angle. These are the four lower extremity biomechanic, cited as risk factors of patellofemoral pain syndrome. [Results] The over pronation, static Q-angle and the dynamic Q-angle were not significantly different between the two groups. However, the hamstring tightness of the PFPS group was significantly greater than that of the controls. [Conclusion] We examined individuals for intrinsic patellofemoral pain syndrome in young adults and lower extremity biomechanics. We found a strong correlation between intrinsic PFPS and hamstring tightness.

  20. Image patch analysis of sunspots and active regions. I. Intrinsic dimension and correlation analysis

    NASA Astrophysics Data System (ADS)

    Moon, Kevin R.; Li, Jimmy J.; Delouille, Véronique; De Visscher, Ruben; Watson, Fraser; Hero, Alfred O.

    2016-01-01

    Context. The flare productivity of an active region is observed to be related to its spatial complexity. Mount Wilson or McIntosh sunspot classifications measure such complexity but in a categorical way, and may therefore not use all the information present in the observations. Moreover, such categorical schemes hinder a systematic study of an active region's evolution for example. Aims: We propose fine-scale quantitative descriptors for an active region's complexity and relate them to the Mount Wilson classification. We analyze the local correlation structure within continuum and magnetogram data, as well as the cross-correlation between continuum and magnetogram data. Methods: We compute the intrinsic dimension, partial correlation, and canonical correlation analysis (CCA) of image patches of continuum and magnetogram active region images taken from the SOHO-MDI instrument. We use masks of sunspots derived from continuum as well as larger masks of magnetic active regions derived from magnetogram to analyze separately the core part of an active region from its surrounding part. Results: We find relationships between the complexity of an active region as measured by its Mount Wilson classification and the intrinsic dimension of its image patches. Partial correlation patterns exhibit approximately a third-order Markov structure. CCA reveals different patterns of correlation between continuum and magnetogram within the sunspots and in the region surrounding the sunspots. Conclusions: Intrinsic dimension has the potential to distinguish simple from complex active regions. These results also pave the way for patch-based dictionary learning with a view toward automatic clustering of active regions.

  1. Systematic differences between the field and cluster elliptical galaxies

    NASA Technical Reports Server (NTRS)

    De Carvalho, R. R.; Djorgovski, S.

    1992-01-01

    Multivariate statistical techniques and fundamental plane fits are used here to study possible systematic differences between field ellipticals (FEs) and cluster ellipticals (CEs). The FEs show more intrinsic scatter in their properties, especially when stellar population variables are included. Pairwise correlations for the two samples are different; the correlations are systematically better for the cluster sample, meaning that ellipticals in the two samples populate their fundamental planes in different ways. Bivariate correlations are different for the two samples, implying that they have different fundamental planes. This is especially true for the correlations which include the population variables Mg2 and (B-V), which are sensitive both to the enrichment history and the storm formation history.

  2. Brain correlates of the intrinsic subjective cost of effort in sedentary volunteers.

    PubMed

    Bernacer, J; Martinez-Valbuena, I; Martinez, M; Pujol, N; Luis, E; Ramirez-Castillo, D; Pastor, M A

    2016-01-01

    One key aspect of motivation is the ability of agents to overcome excessive weighting of intrinsic subjective costs. This contribution aims to analyze the subjective cost of effort and assess its neural correlates in sedentary volunteers. We recruited a sample of 57 subjects who underwent a decision-making task using a prospective, moderate, and sustained physical effort as devaluating factor. Effort discounting followed a hyperbolic function, and individual discounting constants correlated with an indicator of sedentary lifestyle (global physical activity questionnaire; R=-0.302, P=0.033). A subsample of 24 sedentary volunteers received a functional magnetic resonance imaging scan while performing a similar effort-discounting task. BOLD signal of a cluster located in the dorsomedial prefrontal cortex correlated with the subjective value of the pair of options under consideration (Z>2.3, P<0.05; cluster corrected for multiple comparisons for the whole brain). Furthermore, effort-related discounting of reward correlated with the signal of a cluster in the ventrolateral prefrontal cortex (Z>2.3, P<0.05; small volume cluster corrected for a region of interest including the ventral prefrontal cortex and striatum). This study offers empirical data about the intrinsic subjective cost of effort and its neural correlates in sedentary individuals.

  3. Correlated impurities and intrinsic spin-liquid physics in the kagome material herbertsmithite

    NASA Astrophysics Data System (ADS)

    Han, Tian-Heng; Norman, M. R.; Wen, J.-J.; Rodriguez-Rivera, Jose A.; Helton, Joel S.; Broholm, Collin; Lee, Young S.

    2016-08-01

    Low energy inelastic neutron scattering on single crystals of the kagome spin-liquid compound ZnCu3(OD) 6Cl2 (herbertsmithite) reveals antiferromagnetic correlations between impurity spins for energy transfers ℏ ω <0.8 meV (˜J /20 ). The momentum dependence differs significantly from higher energy scattering which arises from the intrinsic kagome spins. The low energy fluctuations are characterized by diffuse scattering near wave vectors (100) and (00 3/2 ), which is consistent with antiferromagnetic correlations between pairs of nearest-neighbor Cu impurities on adjacent triangular (Zn) interlayers. The corresponding impurity lattice resembles a simple cubic lattice in the dilute limit below the percolation threshold. Such an impurity model can describe prior neutron, NMR, and specific heat data. The low energy neutron data are consistent with the presence of a small spin gap (Δ ˜0.7 meV ) in the kagome layers, similar to that recently observed by NMR. The ability to distinguish the scattering due to Cu impurities from that of the planar kagome Cu spins provides an important avenue for probing intrinsic spin-liquid physics.

  4. Mechanical properties of structural amorphous steels: Intrinsic correlations, conflicts, and optimizing strategies

    SciTech Connect

    Liu, Z. Q. Zhang, Z. F.

    2013-12-28

    Amorphous steels have demonstrated superior properties and great potentials for structural applications since their emergence, yet it still remains unclear about how and why their mechanical properties are correlated with other factors and how to achieve intended properties by designing their compositions. Here, the intrinsic interdependences among the mechanical, thermal, and elastic properties of various amorphous steels are systematically elucidated and a general trade-off relation is exposed between the strength and ductility/toughness. Encouragingly, a breakthrough is achievable that the strength and ductility/toughness can be simultaneously improved by tuning the compositions. The composition dependences of the properties and alloying effects are further analyzed thoroughly and interpreted from the fundamental plastic flow and atomic bonding characters. Most importantly, systematic strategies are outlined for optimizing the mechanical properties of the amorphous steels. The study may help establish the intrinsic correlations among the compositions, atomic structures, and properties of the amorphous steels, and provide useful guidance for their alloy design and property optimization. Thus, it is believed to have implications for the development and applications of the structural amorphous steels.

  5. THE COSMIC RATE, LUMINOSITY FUNCTION, AND INTRINSIC CORRELATIONS OF LONG GAMMA-RAY BURSTS

    SciTech Connect

    Butler, Nathaniel R.; Bloom, Joshua S.; Poznanski, Dovi

    2010-03-01

    We calculate durations and spectral parameters for 207 Swift bursts detected by the Burst Alert Telescope from 2007 April to 2009 August, including 67 events with measured redshifts. This is the first supplement to our catalog of 425 Swift gamma-ray bursts (GRBs; 147 with redshifts) starting from GRB 041220. This complete and extensive data set, analyzed with a unified methodology, allows us to conduct an accurate census of intrinsic GRB energetics, hardnesses, durations, and redshifts. The GRB world model we derive reproduces well the observables from both Swift and pre-Swift satellites. Comparing to the cosmic star formation rate, we estimate that only about 0.1% of massive stars explode as bright GRBs. There is strong evidence for evolution in the Swift population at intermediate and high-z, and we can rule out (at the 5sigma level) that this is due to evolution in the luminosity function of GRBs. Instead, the Swift sample suggests a modest propensity for low metallicity, evidenced by an increase in the rate density with redshift. Treating the multivariate data and selection effects rigorously, we find a real, intrinsic correlation between E{sub iso} and E{sub pk} (and possibly also T{sub r45,z}); however, the correlation is not a narrow log-log relation and its observed appearance is strongly detector-dependent. We also estimate the high-z rate (3%-9% of GRBs at z beyond 5) and discuss the extent of a large missing population of low-E{sub pk,obs} X-ray flashes as well as a potentially large missing population of short-duration GRBs that will be probed by EXIST.

  6. Behavioral Correlates of Primates Conservation Status: Intrinsic Vulnerability to Anthropogenic Threats

    PubMed Central

    Lootvoet, Amélie Christelle; Philippon, Justine; Bessa-Gomes, Carmen

    2015-01-01

    Behavioral traits are likely to influence species vulnerability to anthropogenic threats and in consequence, their risk of extinction. Several studies have addressed this question and have highlighted a correlation between reproductive strategies and different viability proxies, such as introduction success and local extinction risk. Yet, very few studies have investigated the effective impact of social behaviour, and evidence regarding global extinction risk remains scant. Here we examined the effects of three main behavioral factors: the group size, the social and reproductive system, and the strength of sexual selection on global extinction risk. Using Primates as biological model, we performed comparative analysis on 93 species. The conservation status as described by the IUCN Red List was considered as a proxy for extinction risk. In addition, we added previously identified intrinsic factors of vulnerability to extinction, and a measure of the strength of the human impact for each species, described by the human footprint. Our analysis highlighted a significant effect of two of the three studied behavioral traits, group size and social and reproductive system. Extinction risk is negatively correlated with mean group size, which may be due to an Allee effect resulting from the difficulties for solitary and monogamous species to find a partner at low densities. Our results also indicate that species with a flexible mating system are less vulnerable. Taking into account these behavioral variables is thus of high importance when establishing conservation plans, particularly when assessing species relative vulnerability. PMID:26444966

  7. The properties of radio ellipticals

    NASA Astrophysics Data System (ADS)

    Sparks, W. B.; Disney, M. J.; Wall, J. V.; Rodgers, A. W.

    1984-03-01

    The authors present optical and additional radio data for the bright galaxies of the Disney & Wall survey. These data form the basis of a statistical comparison of the properties of radio elliptical galaxies to radio-quiet ellipticals. The correlations may be explained by the depth of the gravitational potential well in which the galaxy resides governing the circumstances under which an elliptical galaxy rids itself of internally produced gas.

  8. Intrinsic transverse momentum and parton correlations from dynamical chiral symmetry breaking

    SciTech Connect

    Peter Schweitzer, Mark Strikman, Christian Weiss

    2013-01-01

    The dynamical breaking of chiral symmetry in QCD is caused by nonperturbative interactions on a distance scale rho ~ 0.3 fm, much smaller than the typical hadronic size R ~ 1 fm. These short-distance interactions influence the intrinsic transverse momentum distributions of partons and their correlations at a low normalization point. We study this phenomenon in an effective description of the low-energy dynamics in terms of chiral constituent quark degrees of freedom, which refers to the large-N_c limit of QCD. The nucleon is obtained as a system of constituent quarks and antiquarks moving in a self-consistent classical chiral field (relativistic mean-field approximation, or chiral quark-soliton model). The calculated transverse momentum distributions of constituent quarks and antiquarks are matched with QCD quarks, antiquarks and gluons at the chiral symmetry--breaking scale rho^{-2}. We find that the transverse momentum distribution of valence quarks is localized at p_T^2 ~ R^{-2} and roughly of Gaussian shape. The distribution of unpolarized sea quarks exhibits a would-be power-like tail ~1/p_T^2 extending up to the chiral symmetry-breaking scale. Similar behavior is observed in the flavor-nonsinglet polarized sea. The high-momentum tails are the result of short-range correlations between sea quarks in the nucleon's light-cone wave function, which are analogous to short-range NN correlations in nuclei. We show that the nucleon's light-cone wave function contains correlated pairs of transverse size rho << R with scalar-isoscalar (Sigma) and pseudoscalar-isovector (Pi) quantum numbers, whose internal wave functions have a distinctive spin structure and become identical at p_T^2 ~ rho^{-2} (restoration of chiral symmetry). These features are model-independent and represent an effect of dynamical chiral symmetry breaking on the nucleon's partonic structure. Our results have numerous implications for the transverse momentum distributions of particles produced in hard

  9. Testing the tidal alignment model of galaxy intrinsic alignment

    SciTech Connect

    Blazek, Jonathan; Seljak, Uroš; McQuinn, Matthew E-mail: mmcquinn@berkeley.edu

    2011-05-01

    Weak gravitational lensing has become a powerful probe of large-scale structure and cosmological parameters. Precision weak lensing measurements require an understanding of the intrinsic alignment of galaxy ellipticities, which can in turn inform models of galaxy formation. It is hypothesized that elliptical galaxies align with the background tidal field and that this alignment mechanism dominates the correlation between ellipticities on cosmological scales (in the absence of lensing). We use recent large-scale structure measurements from the Sloan Digital Sky Survey to test this picture with several statistics: (1) the correlation between ellipticity and galaxy overdensity, w{sub g+}; (2) the intrinsic alignment auto-correlation functions; (3) the correlation functions of curl-free, E, and divergence-free, B, modes, the latter of which is zero in the linear tidal alignment theory; (4) the alignment correlation function, w{sub g}(r{sub p},θ), a recently developed statistic that generalizes the galaxy correlation function to account for the angle between the galaxy separation vector and the principle axis of ellipticity. We show that recent measurements are largely consistent with the tidal alignment model and discuss dependence on galaxy luminosity. In addition, we show that at linear order the tidal alignment model predicts that the angular dependence of w{sub g}(r{sub p},θ) is simply w{sub g+}(r{sub p})cos (2θ) and that this dependence is consistent with recent measurements. We also study how stochastic nonlinear contributions to galaxy ellipticity impact these statistics. We find that a significant fraction of the observed LRG ellipticity can be explained by alignment with the tidal field on scales ∼> 10 \\hMpc. These considerations are relevant to galaxy formation and evolution.

  10. Correlation between nitrate concentration in groundwater and parameters affecting aquifer intrinsic vulnerability

    NASA Astrophysics Data System (ADS)

    Debernardi, Laura; de Luca, Domenico Antonio; Lasagna, Manuela

    2008-08-01

    This paper is the result of a study which was carried out in order to verify if the traditional methods to evaluate the intrinsic vulnerability or vulnerability related parameters, are able to clarify the problem of nitrate pollution in groundwater. In particular, the aim was to evaluate limitations and problems connected to aquifer vulnerability methods applied to nitrate contamination prevision in groundwater. The investigation was carried out by comparing NO3 - concentrations, measured in March and November 2004 in the shallow aquifer, and the vulnerability classes, obtained by using GOD and TOT methods. Moreover, it deals with a comparison between NO3 - concentrations and single parameters (depth to water table, land use and nitrogen input). The study area is the plain sector of Piemonte (Northern Italy), where an unconfined aquifer nitrate contamination exists. In this area the anthropogenic presence is remarkable and the input of N-fertilizers and zootechnical effluents to the soil cause a growing amount of nitrates in groundwater. This approach, used in a large area (about 10,000 km2) and in several monitoring wells (about 500), allowed to compare the efficiency of different vulnerability methods and to verify the importance of every parameter on the nitrate concentrations in the aquifer. Furthermore it allowed to obtain interesting correlations in different hydrogeological situations. Correlations between depth to water table, land use and nitrogen input to the soil with nitrate concentrations in groundwater show unclear situations: in fact these comparisons describe the phenomenon trend and highlight the maximum nitrate concentrations for each circumstance but often show wide ranges of possible nitrate concentrations. The same situation could be observed by comparing vulnerability indexes and nitrate concentrations in groundwater. These results suggest that neither single parameters nor vulnerability methods (GOD and TOT) are able to describe individually

  11. Effects of intrinsic decoherence on various correlations and quantum dense coding in a two superconducting charge qubit system

    NASA Astrophysics Data System (ADS)

    Wang, Fei; Maimaitiyiming-Tusun; Parouke-Paerhati; Ahmad-Abliz

    2015-09-01

    The influence of intrinsic decoherence on various correlations and dense coding in a model which consists of two identical superconducting charge qubits coupled by a fixed capacitor is investigated. The results show that, despite the intrinsic decoherence, the correlations as well as the dense coding channel capacity can be effectively increased via the combination of system parameters, i.e., the mutual coupling energy between the two charge qubits is larger than the Josephson energy of the qubit. The bigger the difference between them is, the better the effect is. Project supported by the Project to Develop Outstanding Young Scientific Talents of China (Grant No. 2013711019), the Natural Science Foundation of Xinjiang Province, China (Grant No. 2012211A052), the Foundation for Key Program of Ministry of Education of China (Grant No. 212193), and the Innovative Foundation for Graduate Students Granted by the Key Subjects of Theoretical Physics of Xinjiang Province, China (Grant No. LLWLL201301).

  12. The brain correlates of the effects of monetary and verbal rewards on intrinsic motivation

    PubMed Central

    Albrecht, Konstanze; Abeler, Johannes; Weber, Bernd; Falk, Armin

    2014-01-01

    Apart from everyday duties, such as doing the laundry or cleaning the house, there are tasks we do for pleasure and enjoyment. We do such tasks, like solving crossword puzzles or reading novels, without any external pressure or force; instead, we are intrinsically motivated: we do the tasks because we enjoy doing them. Previous studies suggest that external rewards, i.e., rewards from the outside, affect the intrinsic motivation to engage in a task: while performance-based monetary rewards are perceived as controlling and induce a business-contract framing, verbal rewards praising one's competence can enhance the perceived self-determination. Accordingly, the former have been shown to decrease intrinsic motivation, whereas the latter have been shown to increase intrinsic motivation. The present study investigated the neural processes underlying the effects of monetary and verbal rewards on intrinsic motivation in a group of 64 subjects applying functional magnetic resonance imaging (fMRI). We found that, when participants received positive performance feedback, activation in the anterior striatum and midbrain was affected by the nature of the reward; compared to a non-rewarded control group, activation was higher while monetary rewards were administered. However, we did not find a decrease in activation after reward withdrawal. In contrast, we found an increase in activation for verbal rewards: after verbal rewards had been withdrawn, participants showed a higher activation in the aforementioned brain areas when they received success compared to failure feedback. We further found that, while participants worked on the task, activation in the lateral prefrontal cortex was enhanced after the verbal rewards were administered and withdrawn. PMID:25278834

  13. The brain correlates of the effects of monetary and verbal rewards on intrinsic motivation.

    PubMed

    Albrecht, Konstanze; Abeler, Johannes; Weber, Bernd; Falk, Armin

    2014-01-01

    Apart from everyday duties, such as doing the laundry or cleaning the house, there are tasks we do for pleasure and enjoyment. We do such tasks, like solving crossword puzzles or reading novels, without any external pressure or force; instead, we are intrinsically motivated: we do the tasks because we enjoy doing them. Previous studies suggest that external rewards, i.e., rewards from the outside, affect the intrinsic motivation to engage in a task: while performance-based monetary rewards are perceived as controlling and induce a business-contract framing, verbal rewards praising one's competence can enhance the perceived self-determination. Accordingly, the former have been shown to decrease intrinsic motivation, whereas the latter have been shown to increase intrinsic motivation. The present study investigated the neural processes underlying the effects of monetary and verbal rewards on intrinsic motivation in a group of 64 subjects applying functional magnetic resonance imaging (fMRI). We found that, when participants received positive performance feedback, activation in the anterior striatum and midbrain was affected by the nature of the reward; compared to a non-rewarded control group, activation was higher while monetary rewards were administered. However, we did not find a decrease in activation after reward withdrawal. In contrast, we found an increase in activation for verbal rewards: after verbal rewards had been withdrawn, participants showed a higher activation in the aforementioned brain areas when they received success compared to failure feedback. We further found that, while participants worked on the task, activation in the lateral prefrontal cortex was enhanced after the verbal rewards were administered and withdrawn.

  14. Recent Development in Determining Spontaneous Heating Susceptibility of Indian Coals and Its Correlation with Intrinsic Parameters of Coal

    NASA Astrophysics Data System (ADS)

    Ray, Santosh Kumar; Panigrahi, Durga Charan

    2015-10-01

    The paper describes a new electro-chemical method called wet oxidation potential technique for determining the susceptibility of coal to spontaneous combustion. Altogether 78 coal samples collected from thirteen different mining companies spreading over most of the Indian coalfields have been used for this experimental investigation. Experiments have also been carried out for proximate and ultimate analyses of coal. Susceptibility index obtained from wet oxidation potential was correlated with intrinsic parameters of coal. It has been found that susceptibility index bears a good correlation with moisture content, volatile matter, oxygen, hydrogen and carbon content of coal.

  15. Translational diffusion of hydration water correlates with functional motions in folded and intrinsically disordered proteins

    PubMed Central

    Schirò, Giorgio; Fichou, Yann; Gallat, Francois-Xavier; Wood, Kathleen; Gabel, Frank; Moulin, Martine; Härtlein, Michael; Heyden, Matthias; Colletier, Jacques-Philippe; Orecchini, Andrea; Paciaroni, Alessandro; Wuttke, Joachim; Tobias, Douglas J.; Weik, Martin

    2015-01-01

    Hydration water is the natural matrix of biological macromolecules and is essential for their activity in cells. The coupling between water and protein dynamics has been intensively studied, yet it remains controversial. Here we combine protein perdeuteration, neutron scattering and molecular dynamics simulations to explore the nature of hydration water motions at temperatures between 200 and 300 K, across the so-called protein dynamical transition, in the intrinsically disordered human protein tau and the globular maltose binding protein. Quasi-elastic broadening is fitted with a model of translating, rotating and immobile water molecules. In both experiment and simulation, the translational component markedly increases at the protein dynamical transition (around 240 K), regardless of whether the protein is intrinsically disordered or folded. Thus, we generalize the notion that the translational diffusion of water molecules on a protein surface promotes the large-amplitude motions of proteins that are required for their biological activity. PMID:25774711

  16. Translational diffusion of hydration water correlates with functional motions in folded and intrinsically disordered proteins.

    PubMed

    Schirò, Giorgio; Fichou, Yann; Gallat, Francois-Xavier; Wood, Kathleen; Gabel, Frank; Moulin, Martine; Härtlein, Michael; Heyden, Matthias; Colletier, Jacques-Philippe; Orecchini, Andrea; Paciaroni, Alessandro; Wuttke, Joachim; Tobias, Douglas J; Weik, Martin

    2015-03-16

    Hydration water is the natural matrix of biological macromolecules and is essential for their activity in cells. The coupling between water and protein dynamics has been intensively studied, yet it remains controversial. Here we combine protein perdeuteration, neutron scattering and molecular dynamics simulations to explore the nature of hydration water motions at temperatures between 200 and 300 K, across the so-called protein dynamical transition, in the intrinsically disordered human protein tau and the globular maltose binding protein. Quasi-elastic broadening is fitted with a model of translating, rotating and immobile water molecules. In both experiment and simulation, the translational component markedly increases at the protein dynamical transition (around 240 K), regardless of whether the protein is intrinsically disordered or folded. Thus, we generalize the notion that the translational diffusion of water molecules on a protein surface promotes the large-amplitude motions of proteins that are required for their biological activity.

  17. Short-range correlations in carbon-12, oxygen-16, and neon-20: Intrinsic properties

    NASA Technical Reports Server (NTRS)

    Braley, R. C.; Ford, W. F.; Becker, R. L.; Patterson, M. R.

    1972-01-01

    The Brueckner-Hartree-Fock (BHF) method has been applied to nuclei whose intrinsic structure is nonspherical. Reaction matrix elements were calculated as functions of starting energy for the Hamada-Johnston interaction using the Pauli operator appropriate to O-16 and a shifted oscillator spectrum for virtual excited states. Binding energies, single particle energies, radii, and shape deformations of the intrinsic state, in ordinary as well as renormalized BHF, are discussed and compared with previous HF studies and with experiment when possible. Results are presented for C-12, 0-16 and Ne-20. It is found that the binding energies and radii are too small, but that separation energies are well reproduced when the renormalized theory is used.

  18. Translational diffusion of hydration water correlates with functional motions in folded and intrinsically disordered proteins

    NASA Astrophysics Data System (ADS)

    Schirò, Giorgio; Fichou, Yann; Gallat, Francois-Xavier; Wood, Kathleen; Gabel, Frank; Moulin, Martine; Härtlein, Michael; Heyden, Matthias; Colletier, Jacques-Philippe; Orecchini, Andrea; Paciaroni, Alessandro; Wuttke, Joachim; Tobias, Douglas J.; Weik, Martin

    2015-03-01

    Hydration water is the natural matrix of biological macromolecules and is essential for their activity in cells. The coupling between water and protein dynamics has been intensively studied, yet it remains controversial. Here we combine protein perdeuteration, neutron scattering and molecular dynamics simulations to explore the nature of hydration water motions at temperatures between 200 and 300 K, across the so-called protein dynamical transition, in the intrinsically disordered human protein tau and the globular maltose binding protein. Quasi-elastic broadening is fitted with a model of translating, rotating and immobile water molecules. In both experiment and simulation, the translational component markedly increases at the protein dynamical transition (around 240 K), regardless of whether the protein is intrinsically disordered or folded. Thus, we generalize the notion that the translational diffusion of water molecules on a protein surface promotes the large-amplitude motions of proteins that are required for their biological activity.

  19. A Correlation Between Intrinsic Brightness and Average Decay Rate of Swift UVOT GRB Optical/UV Light Curves

    NASA Technical Reports Server (NTRS)

    Oates, S. R.; Page, M. J.; De Pasquale, M.; Schady, P.; Breeveld, A. A.; Holland, S. T.; Kuin, N. P. M.; Marshall, F. E.

    2012-01-01

    We examine a sample of 48 Swift/UVOT long Gamma-ray Burst light curves and find a correlation between the logarithmic luminosity at 200s and average decay rate determined from 200s onwards, with a Spearman rank coefficient of -0.58 at a significance of 99.998% (4.2 sigma ). We discuss the causes of the log L200s - alpha (greater than) 200s correlation, finding it to be an intrinsic property of long GRBs, and not resulting from the selection criteria. We find two ways to produce the correlation. One possibility is that there is some property of the central engine, outflow or external medium that affects the rate of energy release so that the bright afterglows release their energy more quickly and decay faster than the fainter afterglows. Alternatively, the correlation may be produced by variation of the observers viewing angle, with observers at large viewing angles observing fainter and slower decaying light curves.

  20. First order reversal curves and intrinsic parameter determination for magnetic materials; limitations of hysteron-based approaches in correlated systems

    NASA Astrophysics Data System (ADS)

    Ruta, Sergiu; Hovorka, Ondrej; Huang, Pin-Wei; Wang, Kangkang; Ju, Ganping; Chantrell, Roy

    2017-03-01

    The generic problem of extracting information on intrinsic particle properties from the whole class of interacting magnetic fine particle systems is a long standing and difficult inverse problem. As an example, the Switching Field Distribution (SFD) is an important quantity in the characterization of magnetic systems, and its determination in many technological applications, such as recording media, is especially challenging. Techniques such as the first order reversal curve (FORC) methods, were developed to extract the SFD from macroscopic measurements. However, all methods rely on separating the contributions to the measurements of the intrinsic SFD and the extrinsic effects of magnetostatic and exchange interactions. We investigate the underlying physics of the FORC method by applying it to the output predictions of a kinetic Monte-Carlo model with known input parameters. We show that the FORC method is valid only in cases of weak spatial correlation of the magnetisation and suggest a more general approach.

  1. First order reversal curves and intrinsic parameter determination for magnetic materials; limitations of hysteron-based approaches in correlated systems

    PubMed Central

    Ruta, Sergiu; Hovorka, Ondrej; Huang, Pin-Wei; Wang, Kangkang; Ju, Ganping; Chantrell, Roy

    2017-01-01

    The generic problem of extracting information on intrinsic particle properties from the whole class of interacting magnetic fine particle systems is a long standing and difficult inverse problem. As an example, the Switching Field Distribution (SFD) is an important quantity in the characterization of magnetic systems, and its determination in many technological applications, such as recording media, is especially challenging. Techniques such as the first order reversal curve (FORC) methods, were developed to extract the SFD from macroscopic measurements. However, all methods rely on separating the contributions to the measurements of the intrinsic SFD and the extrinsic effects of magnetostatic and exchange interactions. We investigate the underlying physics of the FORC method by applying it to the output predictions of a kinetic Monte-Carlo model with known input parameters. We show that the FORC method is valid only in cases of weak spatial correlation of the magnetisation and suggest a more general approach. PMID:28338056

  2. Actinidia DRM1--an intrinsically disordered protein whose mRNA expression is inversely correlated with spring budbreak in kiwifruit.

    PubMed

    Wood, Marion; Rae, Georgina M; Wu, Rong-Mei; Walton, Eric F; Xue, Bin; Hellens, Roger P; Uversky, Vladimir N

    2013-01-01

    Intrinsically disordered proteins (IDPs) are a relatively recently defined class of proteins which, under native conditions, lack a unique tertiary structure whilst maintaining essential biological functions. Functional classification of IDPs have implicated such proteins as being involved in various physiological processes including transcription and translation regulation, signal transduction and protein modification. Actinidia DRM1 (Ade DORMANCY ASSOCIATED GENE 1), represents a robust dormancy marker whose mRNA transcript expression exhibits a strong inverse correlation with the onset of growth following periods of physiological dormancy. Bioinformatic analyses suggest that DRM1 is plant specific and highly conserved at both the nucleotide and protein levels. It is predicted to be an intrinsically disordered protein with two distinct highly conserved domains. Several Actinidia DRM1 homologues, which align into two distinct Actinidia-specific families, Type I and Type II, have been identified. No candidates for the Arabidopsis DRM1-Homologue (AtDRM2) an additional family member, has been identified in Actinidia.

  3. Dissolution testing of acetylsalicylic acid by a channel flow method-correlation to USP basket and intrinsic dissolution methods.

    PubMed

    Peltonen, Leena; Liljeroth, Peter; Heikkilä, Tiina; Kontturi, Kyösti; Hirvonen, Jouni

    2003-08-01

    A new modification of the channel flow dissolution method is introduced together with the theoretical basis to extract the solubility and mass transfer parameters from the dissolution experiments. Correlation of drug dissolution profiles in the channel flow apparatus was evaluated with respect to USP basket and intrinsic dissolution methods at pH 1.2 or 6.8. Acetylsalicylic acid (ASA) was studied as a pure drug substance and as three simple tablet compositions with microcrystalline cellulose (MCC) and/or lactose as excipients. The channel flow measurements of 100% ASA tablets correlated well with the results of intrinsic dissolution tests. In the channel flow method as well as in the USP basket method the release of ASA was fastest from the tablet compositions containing lactose, while the slowest dissolution rate was observed with the composition containing MCC as the only excipient. As presumed, the dissolution rate of the weak acid was decreased as the pH of the medium was lowered, which was clearly confirmed also by the three dissolution methods. MCC forms matrix tablets and in the USP basket method the dissolution profiles followed square root of time kinetics indicating that diffusion was the rate-controlling step of ASA dissolution. Also the channel flow results indicated that the dissolution of ASA was controlled by mass transfer. The swelling behaviour of the tablets is different in the channel flow method as compared to the basket method: only one tablet surface is exposed to the dissolution medium in the channel flow system. The contact between the tablet surface and the dissolution medium is more similar between the channel flow and intrinsic dissolution methods.

  4. Intrinsic heterogeneity in oscillatory dynamics limits correlation-induced neural synchronization

    PubMed Central

    Burton, Shawn D.; Ermentrout, G. Bard

    2012-01-01

    Synchronous neural oscillations are found throughout the brain and are thought to contribute to neural coding and the propagation of activity. Several proposed mechanisms of synchronization have gained support through combined theoretical and experimental investigation, including mechanisms based on coupling and correlated input. Here, we ask how correlation-induced synchrony is affected by physiological heterogeneity across neurons. To address this question, we examined cell-to-cell differences in phase-response curves (PRCs), which characterize the response of periodically firing neurons to weak perturbations. Using acute slice electrophysiology, we measured PRCs across a single class of principal neurons capable of sensory-evoked oscillations in vivo: the olfactory bulb mitral cells (MCs). Periodically firing MCs displayed a broad range of PRCs, each of which was well fit by a simple three-parameter model. MCs also displayed differences in firing rate-current relationships and in preferred firing rate ranges. Both the observed PRC heterogeneity and moderate firing rate differences (∼10 Hz) separately reduced the maximum correlation-induced synchrony between MCs by up to 25–30%. Simulations further demonstrated that these components of heterogeneity alone were sufficient to account for the difference in synchronization among heterogeneous vs. homogeneous populations in vitro. Within this simulation framework, independent modulation of specific PRC features additionally revealed which aspects of PRC heterogeneity most strongly impact correlation-induced synchronization. Finally, we demonstrated good agreement of novel mathematical theory with our experimental and simulation results, providing a theoretical basis for the influence of heterogeneity on correlation-induced neural synchronization. PMID:22815400

  5. CCD surface photometry of galaxies with dynamical data. II. UBR photometry of 39 elliptical galaxies

    SciTech Connect

    Peletier, R.F.; Davies, R.L.; Davis, L.E.; Illingworth, G.D.; Cawson, M. Harvard-Smithsonian Center for Astrophysics, Cambridge, MA National Optical Astronomical Observatory, Tucson, AZ Lick Observatory, Santa Cruz, CA Steward Observatory, Tucson, AZ Manchester Victoria Univ. )

    1990-10-01

    Intrinsic properties of elliptical galaxies and the mechanisms of their formation and evolution are discussed on the basis of high-precision, multicolor, surface photometry of 39 elliptical galaxies and measurements of rotation curves and velocity dispersion profiles. Using the data collected, a number of correlations between the characteristic parameters of the stellar population of the galaxies have been made to explore their structure and kinematics. The luminosity dependence of color gradients is a good discriminant among various models of galaxy formation. The lowest luminosity galaxies in the sample do not show any color gradients. They have boxy isophotes, and are also rotationally flattened. These properties may be related to the fact that they are companions of larger ellipsoidal systems and it could also provide an important clue to the formation of ellipticals. 78 refs.

  6. Actinidia DRM1 - An Intrinsically Disordered Protein Whose mRNA Expression Is Inversely Correlated with Spring Budbreak in Kiwifruit

    PubMed Central

    Wood, Marion; Rae, Georgina M.; Wu, Rong-Mei; Walton, Eric F.; Xue, Bin; Hellens, Roger P.; Uversky, Vladimir N.

    2013-01-01

    Intrinsically disordered proteins (IDPs) are a relatively recently defined class of proteins which, under native conditions, lack a unique tertiary structure whilst maintaining essential biological functions. Functional classification of IDPs have implicated such proteins as being involved in various physiological processes including transcription and translation regulation, signal transduction and protein modification. Actinidia DRM1 (Ade DORMANCY ASSOCIATED GENE 1), represents a robust dormancy marker whose mRNA transcript expression exhibits a strong inverse correlation with the onset of growth following periods of physiological dormancy. Bioinformatic analyses suggest that DRM1 is plant specific and highly conserved at both the nucleotide and protein levels. It is predicted to be an intrinsically disordered protein with two distinct highly conserved domains. Several Actinidia DRM1 homologues, which align into two distinct Actinidia-specific families, Type I and Type II, have been identified. No candidates for the Arabidopsis DRM1-Homologue (AtDRM2) an additional family member, has been identified in Actinidia. PMID:23516402

  7. "Intrinsic" correlations and their temporal evolutions between winter-time PNA/EPW and winter drought in the west United States.

    PubMed

    Piao, Lin; Fu, Zuntao; Yuan, Naiming

    2016-01-27

    In this study, relations between winter-time Pacific-Northern America pattern (PNA)/East Pacific wave-train (EPW) and winter-time drought in the west United States over the period of 1951-2010 are analyzed. Considering traditional Pearson's Correlation Coefficient can be influenced by non-stationarity and nonlinearity, a recently proposed method, Detrended Partial-Cross-Correlation Analysis (DPCCA) is applied. With DPCCA, we analyzed the "intrinsic" correlations between PNA/EPW and the winter drought with possible effects of ENSO and PDO removed. We found, i) significant negative correlations between PNA/EPW and drought on time scales of 5-6 years after removing the effects of ENSO, ii) and significant negative correlations between PNA/EPW and drought on time scales of 15-25 years after removing the effects of PDO. By further studying the temporal evolutions of the "intrinsic" correlations, we found on time scales of 5-6 years, the "intrinsic" correlations between PNA/EPW and drought can vary severely with time, but for most time, the correlations are negative. While on interdecadal (15-25 years) time scales, after the effects of PDO removed, unlike the relations between PNA and drought, the "intrinsic" correlations between EPW and drought takes nearly homogeneous-sign over the whole period, indicating a better model can be designed by using EPW.

  8. Possible physical explanation of the intrinsic Ep,i-“intensity” correlation commonly used to “standardize” GRBs

    NASA Astrophysics Data System (ADS)

    Frontera, Filippo; Amati, Lorenzo; Farinelli, Ruben; Dichiara, Simone; Guidorzi, Cristiano; Landi, Raffaella; Titarchuk, Lev

    2016-03-01

    It is recognized that very likely the correlation between peak energy Ep and bolometric intensity is intrinsic to GRBs. However, its physical origin is still debated. In this paper, we will discuss a possible interpretation of the correlation in the light of a GRB prompt emission spectral model, GRBCOMP, proposed in [L. Titarchuk, R. Farinelli, F. Frontera and L. Amati, Astrophys. J. 752 (2012) 116]. GRBCOMP is essentially a photospheric model for the prompt emission of GRBs. Its main ingredients are a thermal bath of soft seed photons and a subrelativistically expanding outflow plasma, consequence of the star explosion. The emerging spectrum is the result of two phases: first, up to the photospheric radius, Comptonization of a subrelativistic electron outflow with thermal bath of soft photons, then, convolution of the Comptonized photons in the first phase with a Green function. The result of this convolution is consistent with different physical processes, in particular Inverse Compton. GRBCOMP has been successfully tested using a significant sample of GRB time resolved spectra in the broad energy band from 2keV to 2MeV [F. Frontera, L. Amati, R. Farinelli, S. Dichiara, C. Guidorzi, R. Landi and L. Titarchuk, Astrophys. J. 779 (2013) 175].

  9. Intrinsic galaxy shapes and alignments - II. Modelling the intrinsic alignment contamination of weak lensing surveys

    NASA Astrophysics Data System (ADS)

    Joachimi, B.; Semboloni, E.; Hilbert, S.; Bett, P. E.; Hartlap, J.; Hoekstra, H.; Schneider, P.

    2013-11-01

    Intrinsic galaxy alignments constitute the major astrophysical systematic of forthcoming weak gravitational lensing surveys but also yield unique insights into galaxy formation and evolution. We build analytic models for the distribution of galaxy shapes based on halo properties extracted from the Millennium Simulation, differentiating between early- and late-type galaxies as well as central galaxies and satellites. The resulting ellipticity correlations are investigated for their physical properties and compared to a suite of current observations. The best-faring model is then used to predict the intrinsic alignment contamination of planned weak lensing surveys. We find that late-type galaxy models generally have weak intrinsic ellipticity correlations, marginally increasing towards smaller galaxy separation and higher redshift. The signal for early-type models at fixed halo mass strongly increases by three orders of magnitude over two decades in galaxy separation, and by one order of magnitude from z = 0 to z = 2. The intrinsic alignment strength also depends strongly on halo mass, but not on galaxy luminosity at fixed mass, or galaxy number density in the environment. We identify models that are in good agreement with all observational data, except that all models overpredict alignments of faint early-type galaxies. The best model yields an intrinsic alignment contamination of a Euclid-like survey between 0.5 and 10 per cent at z > 0.6 and on angular scales larger than a few arcminutes. Cutting 20 per cent of red foreground galaxies using observer-frame colours can suppress this contamination by up to a factor of 2.

  10. Intrinsic Noise Level of Noise Cross-Correlation Functions and its Implication to Source Population of Ambient noises

    NASA Astrophysics Data System (ADS)

    Chen, Ying-Nien; Gung, Yuancheng; Chiao, Ling-Yun; Rhie, Junkee

    2017-01-01

    SUMMARYWe present a quantitative procedure to evaluate the <span class="hlt">intrinsic</span> noise level (INL) of the noise cross-<span class="hlt">correlation</span> function (NCF). The method is applied to realistic NCFs derived from the continuous data recorded by the seismic arrays in Taiwan and Korea. The obtained temporal evolution of NCF noise level follows fairly the prediction of the theoretical formulation, confirming the feasibility of the method. We then apply the obtained INL to the assessment of data quality and the source characteristics of ambient noise. We show that the INL-based signal-to-noise ratio provides an exact measure for the true noise level within the NCF and better resolving power for the NCF quality, and such measurement can be implemented to any time windows of the NCFs to evaluate the quality of overtones or coda waves. Moreover, since NCF amplitudes are influenced by both the population and excitation strengths of noises, while INL is primarily sensitive to the overall source population, with information from both measurements, we may better constrain the source characteristics of seismic ambient noises.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://www.osti.gov/scitech/servlets/purl/1226936','SCIGOV-STC'); return false;" href="http://www.osti.gov/scitech/servlets/purl/1226936"><span id="translatedtitle"><span class="hlt">Correlating</span> optical damage threshold with <span class="hlt">intrinsic</span> defect populations in fused silica as a function of heat treatment temperature</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Shen, N.; Matthews, M. J.; Elhadj, S.; Miller, P. E.; Nelson, A. J.; Hamilton, J.</p> <p>2013-04-03</p> <p>Here, chemical vapor deposition (CVD) is used for the production of fused silica optics in high-power laser applications. However, relatively little is known about the ultraviolet laser damage threshold of CVD films and how they relate to <span class="hlt">intrinsic</span> defects produced during deposition. We present here a study relating structural and electronic defects in CVD films to 355 nm pulsed-laser damage threshold as a function of post-deposition annealing temperature (T<sub>HT</sub>). Plasma-enhanced CVD based on SiH<sub>4</sub>/N<sub>2</sub>O under oxygen-rich conditions was used to deposit 1.5, 3.1 and 6.4 µm thick films on etched SiO2 substrates. Rapid annealing was performed using a scanned CO2 laser beam up to T<sub>HT</sub> ~ 2100 K. The films were then characterized using x-ray photoemission spectroscopy, Fourier transform infrared spectroscopy (FTIR) and photoluminescence spectroscopy. A gradual transition in the damage threshold of annealed films was observed for T<sub>HT</sub> values up to 1600 K, <span class="hlt">correlating</span> with a decrease in non-bridging silanol and oxygen deficient centres. An additional sharp transition in damage threshold also occurs at ~1850 K indicating substrate annealing. Based on our results, a mechanism for damage-related defect annealing is proposed, and the potential of using high-T<sub>HT</sub> CVD SiO<sub>2</sub> to mitigate optical damage is also discussed.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=2588346','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=2588346"><span id="translatedtitle">Functional Anthology of <span class="hlt">Intrinsic</span> Disorder. II. Cellular Components, Domains, Technical Terms, Developmental Processes and Coding Sequence Diversities <span class="hlt">Correlated</span> with Long Disordered Regions</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Vucetic, Slobodan; Xie, Hongbo; Iakoucheva, Lilia M.; Oldfield, Christopher J.; Dunker, A. Keith; Obradovic, Zoran; Uversky, Vladimir N.</p> <p>2008-01-01</p> <p>Biologically active proteins without stable ordered structure (i.e., <span class="hlt">intrinsically</span> disordered proteins) are attracting increased attention. Functional repertoires of ordered and disordered proteins are very different, and the ability to differentiate whether a given function is associated with <span class="hlt">intrinsic</span> disorder or with a well-folded protein is crucial for modern protein science. However, there is a large gap between the number of proteins experimentally confirmed to be disordered and their actual number in nature. As a result, studies of functional properties of confirmed disordered proteins, while helpful in revealing the functional diversity of protein disorder, provide only a limited view. To overcome this problem, a bioinformatics approach for comprehensive study of functional roles of protein disorder was proposed in the first paper of this series (Xie H., Vucetic S., Iakoucheva L.M., Oldfield C.J., Dunker A.K., Obradovic Z., Uversky V.N. (2006) Functional anthology of <span class="hlt">intrinsic</span> disorder. I. Biological processes and functions of proteins with long disordered regions. J. Proteome Res.). Applying this novel approach to Swiss-Prot sequences and functional keywords, we found over 238 and 302 keywords to be strongly positively or negatively <span class="hlt">correlated</span>, respectively, with long <span class="hlt">intrinsically</span> disordered regions. This paper describes ~90 Swiss-Prot keywords attributed to the cellular components, domains, technical terms, developmental processes and coding sequence diversities possessing strong positive and negative <span class="hlt">correlation</span> with long disordered regions. PMID:17391015</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4262373','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4262373"><span id="translatedtitle"><span class="hlt">Intrinsic</span> Thermodynamics and Structure <span class="hlt">Correlation</span> of Benzenesulfonamides with a Pyrimidine Moiety Binding to Carbonic Anhydrases I, II, VII, XII, and XIII</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Kišonaitė, Miglė; Zubrienė, Asta; Čapkauskaitė, Edita; Smirnov, Alexey; Smirnovienė, Joana; Kairys, Visvaldas; Michailovienė, Vilma; Manakova, Elena; Gražulis, Saulius; Matulis, Daumantas</p> <p>2014-01-01</p> <p>The early stage of drug discovery is often based on selecting the highest affinity lead compound. To this end the structural and energetic characterization of the binding reaction is important. The binding energetics can be resolved into enthalpic and entropic contributions to the binding Gibbs free energy. Most compound binding reactions are coupled to the absorption or release of protons by the protein or the compound. A distinction between the observed and <span class="hlt">intrinsic</span> parameters of the binding energetics requires the dissection of the protonation/deprotonation processes. Since only the <span class="hlt">intrinsic</span> parameters can be <span class="hlt">correlated</span> with molecular structural perturbations associated with complex formation, it is these parameters that are required for rational drug design. Carbonic anhydrase (CA) isoforms are important therapeutic targets to treat a range of disorders including glaucoma, obesity, epilepsy, and cancer. For effective treatment isoform-specific inhibitors are needed. In this work we investigated the binding and protonation energetics of sixteen [(2-pyrimidinylthio)acetyl]benzenesulfonamide CA inhibitors using isothermal titration calorimetry and fluorescent thermal shift assay. The compounds were built by combining four sulfonamide headgroups with four tailgroups yielding 16 compounds. Their <span class="hlt">intrinsic</span> binding thermodynamics showed the limitations of the functional group energetic additivity approach used in fragment-based drug design, especially at the level of enthalpies and entropies of binding. Combined with high resolution crystal structural data <span class="hlt">correlations</span> were drawn between the chemical functional groups on selected inhibitors and <span class="hlt">intrinsic</span> thermodynamic parameters of CA-inhibitor complex formation. PMID:25493428</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/22102469','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/22102469"><span id="translatedtitle">Age-related changes in dystrophin-glycoprotein complex and in utrophin are not <span class="hlt">correlated</span> with <span class="hlt">intrinsic</span> laryngeal muscles protection in mdx mice.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Ferretti, Renato; Pertille, Adriana; Santo Neto, Humberto; Marques, Maria Julia</p> <p>2011-12-01</p> <p>In this study we investigate whether dystrophic <span class="hlt">intrinsic</span> laryngeal muscles (ILM) from aged mdx mice show alterations in dystrophin-glycoprotein complex (DGC) components.Immunofluorescence and immunoblotting analyses of beta-sarcoglycan, beta-dystroglycan, and utrophin showed that aged ILM had a similar pattern of changes in aged affected muscles (diaphragm and limb), suggesting that aging leads to changes in utrophin and DGC proteins in dystrophic ILM that cannot be <span class="hlt">correlated</span> with their protection from dystrophic change.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/20160011997','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/20160011997"><span id="translatedtitle">Supersonic <span class="hlt">Elliptical</span> Ramp Inlet</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Adamson, Eric E. (Inventor); Fink, Lawrence E. (Inventor); Fugal, Spencer R. (Inventor)</p> <p>2016-01-01</p> <p>A supersonic inlet includes a supersonic section including a cowl which is at least partially <span class="hlt">elliptical</span>, a ramp disposed within the cowl, and a flow inlet disposed between the cowl and the ramp. The ramp may also be at least partially <span class="hlt">elliptical</span>.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://www.osti.gov/scitech/servlets/purl/957799','SCIGOV-STC'); return false;" href="http://www.osti.gov/scitech/servlets/purl/957799"><span id="translatedtitle">Planar <span class="hlt">elliptic</span> growth</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Mineev, Mark</p> <p>2008-01-01</p> <p>The planar <span class="hlt">elliptic</span> extension of the Laplacian growth is, after a proper parametrization, given in a form of a solution to the equation for areapreserving diffeomorphisms. The infinite set of conservation laws associated with such <span class="hlt">elliptic</span> growth is interpreted in terms of potential theory, and the relations between two major forms of the <span class="hlt">elliptic</span> growth are analyzed. The constants of integration for closed form solutions are identified as the singularities of the Schwarz function, which are located both inside and outside the moving contour. Well-posedness of the recovery of the <span class="hlt">elliptic</span> operator governing the process from the continuum of interfaces parametrized by time is addressed and two examples of exact solutions of <span class="hlt">elliptic</span> growth are presented.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/21727754','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/21727754"><span id="translatedtitle"><span class="hlt">Correlation</span> of <span class="hlt">intrinsic</span> in vitro and in vivo clearance for drugs metabolized by hepatic UDP-glucuronosyltransferases in rats.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Nakamori, Fumihiro; Naritomi, Yoichi; Furutani, Masako; Takamura, Fujiko; Miura, Hiroya; Murai, Hidetsugu; Terashita, Shigeyuki; Teramura, Toshio</p> <p>2011-01-01</p> <p>A method for quantitatively predicting the hepatic clearance of drugs by UDP-glucuronosyltransferases (UGTs) from in vitro data has not yet been established. We examined the relationship between in vitro and in vivo <span class="hlt">intrinsic</span> clearance by rat hepatic UGTs using 10 drugs. For these 10 drugs, the in vitro <span class="hlt">intrinsic</span> clearance by UGTs (CL(int, in vitro)) measured using alamethicin-activated rat liver microsomes was in the range 0.10-4500 ml/min/kg. Microsomal binding (f(u, mic)) was determined to be in the range 0.29-0.95 and the unbound <span class="hlt">intrinsic</span> clearance (CL(uint, in vitro)) to be in the range 0.11-9600 ml/min/kg. The contribution of rat hepatic glucuronidation to drug elimination was 12.0%-76.6% and in vivo <span class="hlt">intrinsic</span> clearance by UGTs was 5.7-9000 ml/min/kg. To evaluate the discrepancy between the in vitro and in vivo values, a scaling factor was calculated (CL(int, in vivo)/CL(int, in vitro)); the values were found to be in the range 0.89-110. The average fold error of the scaling factor values incorporating f(u, mic) was closer to unity than that without f(u, mic). The scaling factor values incorporating f(u, mic) were <10 in 8/10 drugs and <2 in 6/10 drugs, indicating a small discrepancy between in vitro and in vivo values. Thus, using alamethicin-activated liver microsomes, incorporating f(u, mic) into CL(int, in vitro), and considering the contribution of glucuronidation may enable us to quantitatively predict in vivo hepatic glucuronidation from in vitro data.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=20170002443&hterms=Evolution&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D30%26Ntt%3DEvolution','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=20170002443&hterms=Evolution&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D30%26Ntt%3DEvolution"><span id="translatedtitle">Evolution of <span class="hlt">Intrinsic</span> Scatter in the SFR-Stellar Mass <span class="hlt">Correlation</span> at 0.5 less than z Less Than 3</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Kurczynski, Peter; Gawiser, Eric; Acquaviva, Viviana; Bell, Eric F.; Dekel, Avishai; De Mello, Duilia F.; Ferguson, Henry C.; Gardner, Jonathan P.; Grogin, Norman A.</p> <p>2016-01-01</p> <p>We present estimates of <span class="hlt">intrinsic</span> scatter in the star formation rate (SFR)--stellar mass (M*) <span class="hlt">correlation</span> in the redshift range 0.5 less than z less than 3.0 and in the mass range 10(exp 7) less than M* less than 10(exp 11) solar mass. We utilize photometry in the Hubble Ultradeep Field (HUDF12) and Ultraviolet Ultra Deep Field (UVUDF) campaigns and CANDELS/GOODS-S and estimate SFR, M* from broadband spectral energy distributions and the best-available redshifts. The maximum depth of the UDF photometry (F160W 29.9 AB, 5 sigma depth) probes the SFR--M* <span class="hlt">correlation</span> down to M* approximately 10(exp 7) solar mass, a factor of 10-100 x lower in M* than previous studies, and comparable to dwarf galaxies in the local universe. We find the slope of the SFR-M* relationship to be near unity at all redshifts and the normalization to decrease with cosmic time. We find a moderate increase in <span class="hlt">intrinsic</span> scatter with cosmic time from 0.2 to 0.4 dex across the epoch of peak cosmic star formation. None of our redshift bins show a statistically significant increase in <span class="hlt">intrinsic</span> scatter approximately 100 Myr. Our results are consistent with a picture of gradual and self-similar assembly of galaxies across more than three orders of magnitude in stellar mass from as low as 10(exp 7) solar mass.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/6062103','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/6062103"><span id="translatedtitle">Disks in <span class="hlt">elliptical</span> galaxies</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Rix, H.; White, S.D.M. )</p> <p>1990-10-01</p> <p>The abundance and strength of disk components in <span class="hlt">elliptical</span> galaxies are investigated by studying the photometric properties of models containing a spheroidal r exp 1/4-law bulge and a weak exponential disk. Pointed isophotes are observed in a substantial fraction of <span class="hlt">elliptical</span> galaxies. If these isophote distortions are interpreted in the framework of the present models, then the statistics of observed samples suggest that almost all radio-weak <span class="hlt">ellipticals</span> could have disks containing roughly 20 percent of the light. It is shown that the E5 galaxy NGC 4660 has the photometric signatures of a disk containing a third of the light. 30 refs.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19800013899','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19800013899"><span id="translatedtitle">The <span class="hlt">elliptic</span> anomaly</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Janin, G.; Bond, V. R.</p> <p>1980-01-01</p> <p>An independent variable different from the time for <span class="hlt">elliptic</span> orbit integration is used. Such a time transformation provides an analytical step-size regulation along the orbit. An intermediate anomaly (an anomaly intermediate between the eccentric and the true anomaly) is suggested for optimum performances. A particular case of an intermediate anomaly (the <span class="hlt">elliptic</span> anomaly) is defined, and its relation with the other anomalies is developed.</p> </li> </ol> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_1");'>1</a></li> <li><a href="#" onclick='return showDiv("page_2");'>2</a></li> <li class="active"><span>3</span></li> <li><a href="#" onclick='return showDiv("page_4");'>4</a></li> <li><a href="#" onclick='return showDiv("page_5");'>5</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div><!-- col-sm-12 --> </div><!-- row --> </div><!-- page_3 --> <div id="page_4" class="hiddenDiv"> <div class="row"> <div class="col-sm-12"> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_2");'>2</a></li> <li><a href="#" onclick='return showDiv("page_3");'>3</a></li> <li class="active"><span>4</span></li> <li><a href="#" onclick='return showDiv("page_5");'>5</a></li> <li><a href="#" onclick='return showDiv("page_6");'>6</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div> </div> <div class="row"> <div class="col-sm-12"> <ol class="result-class" start="61"> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2015AJ....150..162S','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2015AJ....150..162S"><span id="translatedtitle">The Structure of Galaxies. III. Two Structural Families of <span class="hlt">Ellipticals</span></span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Schombert, James M.</p> <p>2015-11-01</p> <p>Using isophotal radius <span class="hlt">correlations</span> for a sample of Two Micron All Sky Survey <span class="hlt">ellipticals</span>, we have constructed a series of template surface brightness profiles to describe the profile shapes of <span class="hlt">ellipticals</span> as a function of luminosity. The templates are a smooth function of luminosity, yet are not adequately matched to any fitting function supporting the view that <span class="hlt">ellipticals</span> are weakly nonhomologous with respect to structure. Through comparison to the templates, it is discovered that <span class="hlt">ellipticals</span> are divided into two families: those well matched to the templates, and a second class of <span class="hlt">ellipticals</span> with distinctly shallower profile slopes. We refer to this second type of <span class="hlt">ellipticals</span> as D class, an old morphological designation acknowledging diffuse appearance on photographic material. D <span class="hlt">ellipticals</span> cover the same range of luminosity, size, and kinematics as normal <span class="hlt">ellipticals</span>, but maintain a signature of recent equal-mass dry mergers. We propose that normal <span class="hlt">ellipticals</span> grow after an initial dissipation formation era by accretion of low-mass companions as outlined in hierarchical formation scenarios, while D <span class="hlt">ellipticals</span> are the result of later equal-mass mergers producing shallow luminosity profiles.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016ApJ...826...45R','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016ApJ...826...45R"><span id="translatedtitle">A <span class="hlt">Correlation</span> between the <span class="hlt">Intrinsic</span> Brightness and Average Decay Rate of Gamma-Ray Burst X-Ray Afterglow Light Curves</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Racusin, J. L.; Oates, S. R.; de Pasquale, M.; Kocevski, D.</p> <p>2016-07-01</p> <p>We present a <span class="hlt">correlation</span> between the average temporal decay ({α }{{X},{avg},\\gt 200{{s}}}) and early-time luminosity ({L}{{X},200{{s}}}) of X-ray afterglows of gamma-ray bursts as observed by the Swift X-ray Telescope. Both quantities are measured relative to a rest-frame time of 200 s after the γ-ray trigger. The luminosity-average decay <span class="hlt">correlation</span> does not depend on specific temporal behavior and contains one scale-independent quantity minimizing the role of selection effects. This is a complementary <span class="hlt">correlation</span> to that discovered by Oates et al. in the optical light curves observed by the Swift Ultraviolet Optical Telescope. The <span class="hlt">correlation</span> indicates that, on average, more luminous X-ray afterglows decay faster than less luminous ones, indicating some relative mechanism for energy dissipation. The X-ray and optical <span class="hlt">correlations</span> are entirely consistent once corrections are applied and contamination is removed. We explore the possible biases introduced by different light-curve morphologies and observational selection effects, and how either geometrical effects or <span class="hlt">intrinsic</span> properties of the central engine and jet could explain the observed <span class="hlt">correlation</span>.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19910023531','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19910023531"><span id="translatedtitle">Multilevel filtering <span class="hlt">elliptic</span> preconditioners</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Kuo, C. C. Jay; Chan, Tony F.; Tong, Charles</p> <p>1989-01-01</p> <p>A class of preconditioners is presented for <span class="hlt">elliptic</span> problems built on ideas borrowed from the digital filtering theory and implemented on a multilevel grid structure. They are designed to be both rapidly convergent and highly parallelizable. The digital filtering viewpoint allows the use of filter design techniques for constructing <span class="hlt">elliptic</span> preconditioners and also provides an alternative framework for understanding several other recently proposed multilevel preconditioners. Numerical results are presented to assess the convergence behavior of the new methods and to compare them with other preconditioners of multilevel type, including the usual multigrid method as preconditioner, the hierarchical basis method and a recent method proposed by Bramble-Pasciak-Xu.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016ApJ...816...11D','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016ApJ...816...11D"><span id="translatedtitle">The <span class="hlt">Ellipticity</span> Distribution of Ambiguously Blended Objects</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Dawson, William A.; Schneider, Michael D.; Tyson, J. Anthony; Jee, M. James</p> <p>2016-01-01</p> <p>Using overlapping fields with space-based Hubble Space Telescope and ground-based Subaru Telescope imaging we identify a population of blended galaxies that are blended to such a large degree that they are detected as single objects in the ground-based monochromatic imaging, which we label “ambiguous blends.” For deep imaging data, such as the depth targeted with the Large Synoptic Survey Telescope (LSST), the ambiguous blend population is both large (∼14%) and has a distribution of <span class="hlt">ellipticities</span> that is different from that of unblended objects in a way that will likely be important for weak lensing measurements. Most notably, for a limiting magnitude of i ∼ 27 we find that ambiguous blending results in a ∼14% increase in shear noise (or an ∼12% decrease in the effective projected number density of lensed galaxies; neff) due to (1) larger <span class="hlt">intrinsic</span> <span class="hlt">ellipticity</span> dispersion, and (2) a scaling with the galaxy number density Ngal that is shallower than 1/&sqrt;{{N}{gal}}. For the LSST Gold Sample (i < 25.3) there is a ∼7% increase in shear noise (or ∼7% decrease in neff). More importantly than these increases in the shear noise, we find that the <span class="hlt">ellipticity</span> distribution of ambiguous blends has an rms that is 13% larger than that of non-blended galaxies. Given the need of future weak lensing surveys to constrain the <span class="hlt">ellipticity</span> distribution of galaxies to better than a percent in order to mitigate cosmic shear multiplicative biases, if it is unaccounted for, the different <span class="hlt">ellipticity</span> distribution of ambiguous blends could be a dominant systematic.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016MNRAS.457.2301S','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016MNRAS.457.2301S"><span id="translatedtitle"><span class="hlt">Intrinsic</span> alignments of BOSS LOWZ galaxies - II. Impact of shape measurement methods</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Singh, Sukhdeep; Mandelbaum, Rachel</p> <p>2016-04-01</p> <p>Measurements of <span class="hlt">intrinsic</span> alignments of galaxy shapes with the large-scale density field, and the inferred <span class="hlt">intrinsic</span> alignments model parameters, are sensitive to the shape measurement methods used. In this paper, we measure the <span class="hlt">intrinsic</span> alignments of the Sloan Digital Sky Survey-III (SDSS-III) Baryon Oscillation Spectroscopic Survey (BOSS) low redshift (LOWZ) galaxies using three different shape measurement methods (re-Gaussianization, isophotal, and de Vaucouleurs), identifying a variation in the inferred <span class="hlt">intrinsic</span> alignments amplitude at the 40 per cent level between these methods, independent of the galaxy luminosity or other properties. We also carry out a suite of systematics tests on the shapes and their two-point <span class="hlt">correlation</span> functions, identifying a pronounced contribution from additive point spread function systematics in the de Vaucouleurs shapes. Since different methods measure galaxy shapes at different effective radii, the trends we identify in the <span class="hlt">intrinsic</span> alignments amplitude are consistent with the interpretation that the outer regions of galaxy shapes are more responsive to tidal fields, resulting in isophote twisting and stronger alignments for isophotal shapes. We observe environment dependence of <span class="hlt">ellipticity</span>, with brightest galaxies in groups being rounder on average compared to satellite and field galaxies. We also study the anisotropy in <span class="hlt">intrinsic</span> alignments measurements introduced by projected shapes, finding effects consistent with predictions of the non-linear alignment model and hydrodynamic simulations. The large variations seen using the different shape measurement methods have important implications for <span class="hlt">intrinsic</span> alignments forecasting and mitigation with future surveys.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017A%26A...597A.122S','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017A%26A...597A.122S"><span id="translatedtitle">Cluster and field <span class="hlt">elliptical</span> galaxies at z 1.3. The marginal role of the environment and the relevance of the galaxy central regions</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Saracco, P.; Gargiulo, A.; Ciocca, F.; Marchesini, D.</p> <p>2017-01-01</p> <p>. Also the Σ1 kpc-mass relation follows two different regimes, above and below the transition mass (Σ1 kpc ∝ Μ*1.07<mt0.64>mt) defining a transition mass density Σ1 kpc ≃ 2-3 × 103M⊙ pc-2. The effective stellar mass density ΣRe does not <span class="hlt">correlate</span> with mass; dense/compact galaxies can be assembled over a wide mass regime, independently of the environment. The central stellar mass density, Σ1 kpc, besides being <span class="hlt">correlated</span> with the mass, is <span class="hlt">correlated</span> to the age of the stellar population: the higher the central stellar mass density, the higher the mass, the older the age of the stellar population. Conclusions: While we found some evidence of environmental effects on the <span class="hlt">elliptical</span> galaxies as a population, we did not find differences between the <span class="hlt">intrinsic</span> properties of cluster and field <span class="hlt">elliptical</span> galaxies at comparable redshift. The structure and the shaping of <span class="hlt">elliptical</span> galaxies at z 1.3 do not depend on the environment. However, a dense environment seems to be more efficient in assembling high-mass large <span class="hlt">ellipticals</span>, much rarer in the field at this redshift. The <span class="hlt">correlation</span> found between the central stellar mass density and the age of the galaxies beside the mass shows the close connection of the central regions to the main phases of mass growth.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19910004829','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19910004829"><span id="translatedtitle">Far-infrared emission from dusty <span class="hlt">ellipticals</span></span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Walsh, Duncan; Knapp, Jill</p> <p>1990-01-01</p> <p>The incidence of dust lanes in <span class="hlt">elliptical</span> galaxies has been estimated at approx. 40 percent by Sadler and Gerhard (1985), although the observed fraction is lower because of inclination effects. A similar percentage of <span class="hlt">ellipticals</span> has been detected by the Infrared Astronomy Satellite (IRAS) at 100 microns (Knapp et al. 1989); these have far-infrared colors expected for emission from cool dust (S sub 60 micron/S sub 100 micron approx. 1/3). For the far-infrared detected galaxies, neither L sub 100 microns/L sub B nor L sub 60 microns/L sub 100 microns are very dependent on dust content, suggesting that the source of the infrared luminosity is the same in both cases; and hence that dust is responsible even when not detected optically. Despite this indication, L sub 100 microns does not prove to be a good indicator of the quantity of cool interstellar matter in <span class="hlt">elliptical</span> galaxies, as measured by the mass of neutral hydrogen. There even exist several examples of <span class="hlt">ellipticals</span> with dust, strong 100 micron flux density and sensitive limits on HI mass (Walsh et al. in preparation). Chief reasons for the lack of <span class="hlt">correlation</span> include the existence of other important sources of far-IR power in <span class="hlt">ellipticals</span>, such as nonthermal continuum emission extending from longer wavelengths in flat spectrum radio sources (Golombek, Miley and Neugebauer 1988); and the fact that far-infrared luminosity per unit dust mass is extremely sensitive to the temperature of the ambient radiation field, which is not accurately known. In addition to having their appearance distorted by dust, several <span class="hlt">ellipticals</span> also show such features as shells, box-shaped isophotes or inner disks. These may be signatures of past mergers, which could also add to the ISM content of the system.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016IAUS..308..437C','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016IAUS..308..437C"><span id="translatedtitle">How the cosmic web induces <span class="hlt">intrinsic</span> alignments of galaxies</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Codis, S.; Dubois, Y.; Pichon, C.; Devriendt, J.; Slyz, A.</p> <p>2016-10-01</p> <p><span class="hlt">Intrinsic</span> alignments are believed to be a major source of systematics for future generation of weak gravitational lensing surveys like Euclid or LSST. Direct measurements of the alignment of the projected light distribution of galaxies in wide field imaging data seem to agree on a contamination at a level of a few per cent of the shear <span class="hlt">correlation</span> functions, although the amplitude of the effect depends on the population of galaxies considered. Given this dependency, it is difficult to use dark matter-only simulations as the sole resource to predict and control <span class="hlt">intrinsic</span> alignments. We report here estimates on the level of <span class="hlt">intrinsic</span> alignment in the cosmological hydrodynamical simulation Horizon-AGN that could be a major source of systematic errors in weak gravitational lensing measurements. In particular, assuming that the spin of galaxies is a good proxy for their <span class="hlt">ellipticity</span>, we show how those spins are spatially <span class="hlt">correlated</span> and how they couple to the tidal field in which they are embedded. We will also present theoretical calculations that illustrate and qualitatively explain the observed signals.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2010JMoSt.974..127Z','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2010JMoSt.974..127Z"><span id="translatedtitle">Evaluation on <span class="hlt">intrinsic</span> quality of licorice influenced by environmental factors by using FTIR combined with 2D-IR <span class="hlt">correlation</span> spectroscopy</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Zhou, Ying-qun; Yu, Hua; Zhang, Yan-ling; Sun, Su-qin; Chen, Shi-lin; Zhao, Run-huai; Zhou, Qun; Noda, Isao</p> <p>2010-06-01</p> <p>To evaluate the <span class="hlt">intrinsic</span> quality of licorice influenced by environmental factors, the spectral comparison of licorice from two typical ecological habitats was conducted by using FTIR and 2D-IR <span class="hlt">correlation</span> spectroscopy. There were differences in the peak intensities of 1155, 1076 and 1048 cm -1 of FTIR profiles. The difference was amplified by the second derivative spectrum for the peak intensities at 1370, 1365 and 1317 cm -1 and the peak shape in 958-920 cm -1 and 1050-988 cm -1. The synchronous 2D-IR spectra within the range of 860-1300 cm -1 were classified into type I and type II and their frequency in the two groups was noticeably different. Although the chemical compounds of licorice samples from two areas were generally similar, the contents of starch, calcium oxalate, and some chemical compounds containing alcohol hydroxyl group were different, indicating the influence of precipitation and temperature. This study demonstrates that the systematical analysis of FTIR, the second derivative spectrum and 2D-IR can effectively determine the differences in licorice samples from different ecological habitats.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://www.dtic.mil/docs/citations/ADA075987','DTIC-ST'); return false;" href="http://www.dtic.mil/docs/citations/ADA075987"><span id="translatedtitle"><span class="hlt">Intrinsic</span> Geodesy</span></a></p> <p><a target="_blank" href="https://publicaccess.dtic.mil/psm/api/service/search/search">DTIC Science & Technology</a></p> <p></p> <p>1952-03-01</p> <p>Variation with the Height of the Principal Radii of Curvature in Somigliana’s Theory"), Bollettino di Geodesia e Scienze Affini, anno VIII, 1950 46...MARUSSI, A., "Principi di Geodesia Intrinseca applicati al campo di Somigliana" ("Principles of <span class="hlt">Intrinsic</span> Geodesy Applied to Somigliana’s Field...34), Bollettino di Geodesia e Scienze Affini, anno VIII, 1950; and also Atti della XLII Riunione _dela Socie&Ljtsjjganaper il Progresso delle Scienze, Roma</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/20100002829','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/20100002829"><span id="translatedtitle">Enhanced <span class="hlt">Elliptic</span> Grid Generation</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Kaul, Upender K.</p> <p>2007-01-01</p> <p>An enhanced method of <span class="hlt">elliptic</span> grid generation has been invented. Whereas prior methods require user input of certain grid parameters, this method provides for these parameters to be determined automatically. "<span class="hlt">Elliptic</span> grid generation" signifies generation of generalized curvilinear coordinate grids through solution of <span class="hlt">elliptic</span> partial differential equations (PDEs). Usually, such grids are fitted to bounding bodies and used in numerical solution of other PDEs like those of fluid flow, heat flow, and electromagnetics. Such a grid is smooth and has continuous first and second derivatives (and possibly also continuous higher-order derivatives), grid lines are appropriately stretched or clustered, and grid lines are orthogonal or nearly so over most of the grid domain. The source terms in the grid-generating PDEs (hereafter called "defining" PDEs) make it possible for the grid to satisfy requirements for clustering and orthogonality properties in the vicinity of specific surfaces in three dimensions or in the vicinity of specific lines in two dimensions. The grid parameters in question are decay parameters that appear in the source terms of the inhomogeneous defining PDEs. The decay parameters are characteristic lengths in exponential- decay factors that express how the influences of the boundaries decrease with distance from the boundaries. These terms govern the rates at which distance between adjacent grid lines change with distance from nearby boundaries. Heretofore, users have arbitrarily specified decay parameters. However, the characteristic lengths are coupled with the strengths of the source terms, such that arbitrary specification could lead to conflicts among parameter values. Moreover, the manual insertion of decay parameters is cumbersome for static grids and infeasible for dynamically changing grids. In the present method, manual insertion and user specification of decay parameters are neither required nor allowed. Instead, the decay parameters are</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/26026609','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/26026609"><span id="translatedtitle">Activation of the Nrf2 response by <span class="hlt">intrinsic</span> hepatotoxic drugs <span class="hlt">correlates</span> with suppression of NF-κB activation and sensitizes toward TNFα-induced cytotoxicity.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Herpers, Bram; Wink, Steven; Fredriksson, Lisa; Di, Zi; Hendriks, Giel; Vrieling, Harry; de Bont, Hans; van de Water, Bob</p> <p>2016-05-01</p> <p>Drug-induced liver injury (DILI) is an important problem both in the clinic and in the development of new safer medicines. Two pivotal adaptation and survival responses to adverse drug reactions are oxidative stress and cytokine signaling based on the activation of the transcription factors Nrf2 and NF-κB, respectively. Here, we systematically investigated Nrf2 and NF-κB signaling upon DILI-related drug exposure. Transcriptomics analyses of 90 DILI compounds in primary human hepatocytes revealed that a strong Nrf2 activation is associated with a suppression of endogenous NF-κB activity. These responses were translated into quantitative high-content live-cell imaging of induction of a selective Nrf2 target, GFP-tagged Srxn1, and the altered nuclear translocation dynamics of a subunit of NF-κB, GFP-tagged p65, upon TNFR signaling induced by TNFα using HepG2 cells. Strong activation of GFP-Srxn1 expression by DILI compounds typically <span class="hlt">correlated</span> with suppression of NF-κB nuclear translocation, yet reversely, activation of NF-κB by TNFα did not affect the Nrf2 response. DILI compounds that provided strong Nrf2 activation, including diclofenac, carbamazepine and ketoconazole, sensitized toward TNFα-mediated cytotoxicity. This was related to an adaptive primary protective response of Nrf2, since loss of Nrf2 enhanced this cytotoxic synergy with TNFα, while KEAP1 downregulation was cytoprotective. These data indicate that both Nrf2 and NF-κB signaling may be pivotal in the regulation of DILI. We propose that the NF-κB-inhibiting effects that coincide with a strong Nrf2 stress response likely sensitize liver cells to pro-apoptotic signaling cascades induced by <span class="hlt">intrinsic</span> cytotoxic pro-inflammatory cytokines.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=424398','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=424398"><span id="translatedtitle"><span class="hlt">Intrinsic</span> bioactivity of thyrotropin in human serum is inversely <span class="hlt">correlated</span> with thyroid hormone concentrations. Application of a new bioassay using the FRTL-5 rat thyroid cell strain.</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Dahlberg, P A; Petrick, P A; Nissim, M; Menezes-Ferreira, M M; Weintraub, B D</p> <p>1987-01-01</p> <p>We have developed a new bioassay for thyrotropin (TSH) in human serum to evaluate bioactivity in normal individuals and patients with different degrees of primary hypothyroidism. Unpurified TSH in serum showed no stimulation of cyclic AMP production in cultured FRTL-5 rat thyroid cells, but after immunopurification showed potent stimulatory activity. Immunoaffinity purification permitted up to 400-fold concentration of serum TSH, allowing bioactivity measurements even in certain normal sera. The limit of detection in the FRTL-5 bioassay was 10 microU of human TSH per 0.5 ml incubate, and half-maximal responses for standard human TSH was 102 +/- 26 (+/- SE) microU/0.5 ml. Immunoaffinity-purified serum TSH varied in bioactivity-to-immunoactivity (B/I) ratios from less than 0.25 to 1.21 among four euthyroid subjects and eight primary hypothyroid patients. An inverse <span class="hlt">correlation</span> was found between B/I ratios of immunopurified basal TSH and the serum-free T4 (r = -0.7237, P less than 0.01), T4 (r = -0.6650, P less than 0.05), and T3 (r = -0.6382, P less than 0.05). B/I ratios of immunopurified TSH from three hypothyroid patients before and after acute stimulation by thyrotropin-releasing hormone showed no significant change, despite major changes in serum TSH. In summary, the present study shows an inverse relationship between the metabolic status of an individual and the <span class="hlt">intrinsic</span> bioactivity of TSH. Images PMID:3571493</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/20110005514','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/20110005514"><span id="translatedtitle">Modulated <span class="hlt">Elliptical</span> Slot</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Abou-Khousa, M. A.</p> <p>2009-01-01</p> <p>A novel modulated slot design has been proposed and tested. The proposed slot is aimed to replace the inefficient small dipoles used in conventional MST-based imaging systems. The developed slot is very attractive as MST array element due to its small size and high efficiency/modulation depth. In fact, the developed slot has been successfully used to implement the first prototype of a microwave camera operating at 24 GHZ. It is also being used in the design of the second generation of the camera. Finally, the designed <span class="hlt">elliptical</span> slot can be used as an electronically controlled waveguide iris for many other purposes (for instance in constructing waveguide reflective phase shifters and multiplexers/switches).</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/22034581','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/22034581"><span id="translatedtitle">THE STELLAR HALOS OF MASSIVE <span class="hlt">ELLIPTICAL</span> GALAXIES</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Greene, Jenny E.; Murphy, Jeremy D.; Comerford, Julia M.; Gebhardt, Karl; Adams, Joshua J.</p> <p>2012-05-01</p> <p>We use the Mitchell Spectrograph (formerly VIRUS-P) on the McDonald Observatory 2.7 m Harlan J. Smith Telescope to search for the chemical signatures of massive <span class="hlt">elliptical</span> galaxy assembly. The Mitchell Spectrograph is an integral-field spectrograph with a uniquely wide field of view (107'' Multiplication-Sign 107''), allowing us to achieve remarkably high signal-to-noise ratios of {approx}20-70 pixel{sup -1} in radial bins of 2-2.5 times the effective radii of the eight galaxies in our sample. Focusing on a sample of massive <span class="hlt">elliptical</span> galaxies with stellar velocity dispersions {sigma}{sub *} > 150 km s{sup -1}, we study the radial dependence in the equivalent widths (EW) of key metal absorption lines. By twice the effective radius, the Mgb EWs have dropped by {approx}50%, and only a weak <span class="hlt">correlation</span> between {sigma}{sub *} and Mgb EW remains. The Mgb EWs at large radii are comparable to those seen in the centers of <span class="hlt">elliptical</span> galaxies that are {approx} an order of magnitude less massive. We find that the well-known metallicity gradients often observed within an effective radius continue smoothly to 2.5 R{sub e} , while the abundance ratio gradients remain flat. Much like the halo of the Milky Way, the stellar halos of our galaxies have low metallicities and high {alpha}-abundance ratios, as expected for very old stars formed in small stellar systems. Our observations support a picture in which the outer parts of massive <span class="hlt">elliptical</span> galaxies are built by the accretion of much smaller systems whose star formation history was truncated at early times.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2012ApJ...750...32G','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2012ApJ...750...32G"><span id="translatedtitle">The Stellar Halos of Massive <span class="hlt">Elliptical</span> Galaxies</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Greene, Jenny E.; Murphy, Jeremy D.; Comerford, Julia M.; Gebhardt, Karl; Adams, Joshua J.</p> <p>2012-05-01</p> <p>We use the Mitchell Spectrograph (formerly VIRUS-P) on the McDonald Observatory 2.7 m Harlan J. Smith Telescope to search for the chemical signatures of massive <span class="hlt">elliptical</span> galaxy assembly. The Mitchell Spectrograph is an integral-field spectrograph with a uniquely wide field of view (107'' × 107''), allowing us to achieve remarkably high signal-to-noise ratios of ~20-70 pixel-1 in radial bins of 2-2.5 times the effective radii of the eight galaxies in our sample. Focusing on a sample of massive <span class="hlt">elliptical</span> galaxies with stellar velocity dispersions σ* > 150 km s-1, we study the radial dependence in the equivalent widths (EW) of key metal absorption lines. By twice the effective radius, the Mgb EWs have dropped by ~50%, and only a weak <span class="hlt">correlation</span> between σ* and Mgb EW remains. The Mgb EWs at large radii are comparable to those seen in the centers of <span class="hlt">elliptical</span> galaxies that are ~ an order of magnitude less massive. We find that the well-known metallicity gradients often observed within an effective radius continue smoothly to 2.5 Re , while the abundance ratio gradients remain flat. Much like the halo of the Milky Way, the stellar halos of our galaxies have low metallicities and high α-abundance ratios, as expected for very old stars formed in small stellar systems. Our observations support a picture in which the outer parts of massive <span class="hlt">elliptical</span> galaxies are built by the accretion of much smaller systems whose star formation history was truncated at early times.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/952928','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/952928"><span id="translatedtitle">Event-by-event <span class="hlt">elliptic</span> flow fluctuations from PHOBOS.</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Alver, B.; Back, B. B.; Baker, M. D.; Ballintijn, M.; Barton, D. S.; Physics; BNL; Inst. of Nuclear Physics; Massachusetts Inst. of Tech.; National Central Univ.; Univ. of Maryland; Univ. of Rochester</p> <p>2009-04-01</p> <p>Recently PHOBOS has focused on the study of fluctuations and <span class="hlt">correlations</span> in particle production in heavy-ion collisions at the highest energies delivered by the Relativistic Heavy Ion Collider (RHIC). In this report, we present results on event-by-event <span class="hlt">elliptic</span> flow fluctuations in Au + Au collisions at {radical}s{sub NN} = 200 GeV. A data-driven method was used to estimate the dominant contribution from non-flow <span class="hlt">correlations</span>. Over the broad range of collision centralities, the observed large <span class="hlt">elliptic</span> flow fluctuations are in agreement with the fluctuations in the initial source eccentricity.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19950043281&hterms=temper&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D30%26Ntt%3Dtemper','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19950043281&hterms=temper&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D30%26Ntt%3Dtemper"><span id="translatedtitle">Dwarf <span class="hlt">elliptical</span> galaxies</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Ferguson, Henry C.; Binggeli, Bruno</p> <p>1994-01-01</p> <p>Dwarf <span class="hlt">elliptical</span> (dE) galaxies, with blue absolute magnitudes typically fainter than M(sub B) = -16, are the most numerous type of galaxy in the nearby universe. Tremendous advances have been made over the past several years in delineating the properties of both Local Group satellite dE's and the large dE populations of nearby clusters. We review some of these advances, with particular attention to how well currently availiable data can constrain (a) models for the formation of dE's, (b) the physical and evolutionary connections between different types of galaxies that overlap in the same portion of the mass-spectrum of galaxies, (c) the contribution of dE's to the galaxy luminosity functions in clusters and the field, (d) the star-forming histories of dE's and their possible contribution to faint galaxy counts, and (e) the clustering properties of dE's. In addressing these issues, we highlight the extent to which selection effects temper these constraints, and outline areas where new data would be particularly valuable.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://www.osti.gov/scitech/servlets/purl/940493','SCIGOV-STC'); return false;" href="http://www.osti.gov/scitech/servlets/purl/940493"><span id="translatedtitle">Image <span class="hlt">Ellipticity</span> from Atmospheric Aberrations</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>de Vries, W H; Olivier, S S; Asztalos, S J; Rosenberg, L J; Baker, K L</p> <p>2007-03-06</p> <p>We investigate the <span class="hlt">ellipticity</span> of the point-spread function (PSF) produced by imaging an unresolved source with a telescope, subject to the effects of atmospheric turbulence. It is important to quantify these effects in order to understand the errors in shape measurements of astronomical objects, such as those used to study weak gravitational lensing of field galaxies. The PSF modeling involves either a Fourier transform of the phase information in the pupil plane or a ray-tracing approach, which has the advantage of requiring fewer computations than the Fourier transform. Using a standard method, involving the Gaussian weighted second moments of intensity, we then calculate the <span class="hlt">ellipticity</span> of the PSF patterns. We find significant <span class="hlt">ellipticity</span> for the instantaneous patterns (up to more than 10%). Longer exposures, which we approximate by combining multiple (N) images from uncorrelated atmospheric realizations, yield progressively lower <span class="hlt">ellipticity</span> (as 1/{radical}N). We also verify that the measured <span class="hlt">ellipticity</span> does not depend on the sampling interval in the pupil plane using the Fourier method. However, we find that the results using the ray-tracing technique do depend on the pupil sampling interval, representing a gradual breakdown of the geometric approximation at high spatial frequencies. Therefore, ray tracing is generally not an accurate method of modeling PSF <span class="hlt">ellipticity</span> induced by atmospheric turbulence unless some additional procedure is implemented to correctly account for the effects of high spatial frequency aberrations. The Fourier method, however, can be used directly to accurately model PSF <span class="hlt">ellipticity</span>, which can give insights into errors in the statistics of field galaxy shapes used in studies of weak gravitational lensing.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/22494865','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/22494865"><span id="translatedtitle">Decoupling antennas in printed technology using <span class="hlt">elliptical</span> metasurface cloaks</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Bernety, Hossein M. E-mail: yakovlev@olemiss.edu; Yakovlev, Alexander B. E-mail: yakovlev@olemiss.edu</p> <p>2016-01-07</p> <p>In this paper, we extend the idea of reducing the electromagnetic interactions between transmitting radiators to the case of widely used planar antennas in printed technology based on the concept of mantle cloaking. Here, we show that how lightweight <span class="hlt">elliptical</span> metasurface cloaks can be engineered to restore the <span class="hlt">intrinsic</span> properties of printed antennas with strip inclusions. In order to present the novel approach, we consider two microstrip-fed monopole antennas resonating at slightly different frequencies cloaked by confocal <span class="hlt">elliptical</span> metasurfaces formed by arrays of sub-wavelength periodic elements, partially embedded in the substrate. The presence of the metasurfaces leads to the drastic suppression of mutual near-field and far-field couplings between the antennas, and thus, their radiation patterns are restored as if they were isolated. Moreover, it is worth noting that this approach is not limited to printed radiators and can be applied to other planar structures as well.</p> </li> </ol> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_2");'>2</a></li> <li><a href="#" onclick='return showDiv("page_3");'>3</a></li> <li class="active"><span>4</span></li> <li><a href="#" onclick='return showDiv("page_5");'>5</a></li> <li><a href="#" onclick='return showDiv("page_6");'>6</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div><!-- col-sm-12 --> </div><!-- row --> </div><!-- page_4 --> <div id="page_5" class="hiddenDiv"> <div class="row"> <div class="col-sm-12"> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_3");'>3</a></li> <li><a href="#" onclick='return showDiv("page_4");'>4</a></li> <li class="active"><span>5</span></li> <li><a href="#" onclick='return showDiv("page_6");'>6</a></li> <li><a href="#" onclick='return showDiv("page_7");'>7</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div> </div> <div class="row"> <div class="col-sm-12"> <ol class="result-class" start="81"> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2009PhTea..47..163N','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2009PhTea..47..163N"><span id="translatedtitle">Energy and the <span class="hlt">Elliptical</span> Orbit</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Nettles, Bill</p> <p>2009-03-01</p> <p>In the January 2007 issue of The Physics Teacher, Prentis, Fulton, Hesse, and Mazzino describe a laboratory exercise in which students use a geometrical analysis inspired by Newton to show that an <span class="hlt">elliptical</span> orbit and an inverse-square law force go hand in hand. The historical, geometrical, and teamwork aspects of the exercise are useful and important. This paper presents an exercise which uses an energy/angular momentum conservation model for <span class="hlt">elliptical</span> orbits. This exercise can be done easily by an individual student and on regular notebook-sized paper.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016AAS...22712105Y','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016AAS...22712105Y"><span id="translatedtitle">The MUSCLES Treasury Survey: <span class="hlt">Intrinsic</span> Lyα Profile Reconstructions and UV, X-ray, and Optical <span class="hlt">Correlations</span> of Low-mass Exoplanet Host Stars</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Youngblood, Allison; France, Kevin; Parke Loyd, R. O.</p> <p>2016-01-01</p> <p>UV stellar radiation can significantly impact planetary atmospheres through heating and photochemistry, even regulating production of potential biomarkers. Cool stars emit the majority of their UV radiation in the form of emission lines, and the incident UV radiation on close-in habitable-zone planets is significant. Lyα (1215.67 Å) dominates the 912 - 3200 Å spectrum of cool stars, but strong absorption from the interstellar medium (ISM) makes direct observations of the <span class="hlt">intrinsic</span> Lyα emission of even nearby stars challenging. The MUSCLES Hubble Space Telescope Treasury Survey (Measurements of the Ultraviolet Spectral Characteristics of Low-mass Exoplanetary Systems) has completed observations of 7 M and 4 K stars hosting exoplanets (d < 22 pc) with simultaneous X-ray and ground-based optical spectroscopy for many of the targets. We have reconstructed the <span class="hlt">intrinsic</span> Lyα profiles using an MCMC technique and used the results to estimate the extreme ultraviolet (100 - 911 Å) spectrum. We also present empirical relations between chromospheric UV and optical lines, e.g., Lyα, Mg II, Ca II H & K, and Hα, for use when direct UV observations of low-mass exoplanet host stars are not possible. The spectra presented here will be made publicly available through MAST to support exoplanet atmosphere modeling.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://eric.ed.gov/?q=fourier&pg=6&id=EJ770453','ERIC'); return false;" href="http://eric.ed.gov/?q=fourier&pg=6&id=EJ770453"><span id="translatedtitle">Fourier Series and <span class="hlt">Elliptic</span> Functions</span></a></p> <p><a target="_blank" href="http://www.eric.ed.gov/ERICWebPortal/search/extended.jsp?_pageLabel=advanced">ERIC Educational Resources Information Center</a></p> <p>Fay, Temple H.</p> <p>2003-01-01</p> <p>Non-linear second-order differential equations whose solutions are the <span class="hlt">elliptic</span> functions "sn"("t, k"), "cn"("t, k") and "dn"("t, k") are investigated. Using "Mathematica", high precision numerical solutions are generated. From these data, Fourier coefficients are determined yielding approximate formulas for these non-elementary functions that are…</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/22263966','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/22263966"><span id="translatedtitle">The ESS <span class="hlt">elliptical</span> cavity cryomodules</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Darve, Christine; Bosland, Pierre; Devanz, Guillaume; Renard, Bertrand; Olivier, Gilles; Thermeau, Jean-Pierre</p> <p>2014-01-29</p> <p>The European Spallation Source (ESS) is a multi-disciplinary research centre under design and construction in Lund, Sweden. This new facility is funded by a collaboration of 17 European countries and is expected to be up to 30 times brighter than today’s leading facilities and neutron sources. The ESS will enable new opportunities for researchers in the fields of life sciences, energy, environmental technology, cultural heritage and fundamental physics. A 5 MW long pulse proton accelerator is used to reach this goal. The pulsed length is 2.86 ms, the repetition frequency is 14 Hz (4 % duty cycle), and the beam current is 62.5 mA. The superconducting section of the Linac accelerates the beam from 80 MeV to 2.0 GeV. It is composed of one string of spoke cavity cryomodule and two strings of <span class="hlt">elliptical</span> cavity cryomodules. These cryomodules contain four <span class="hlt">elliptical</span> Niobium cavities operating at 2 K and at a frequency of 704.42 MHz. This paper introduces the thermo-mechanical design, the prototyping and the expected operation of the ESS <span class="hlt">elliptical</span> cavity cryomodules. An <span class="hlt">Elliptical</span> Cavity Cryomodule Technology Demonstrator (ECCTD) will be built and tested in order to validate the ESS series production.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://eric.ed.gov/?q=Conservation+AND+Laws&pg=5&id=EJ852869','ERIC'); return false;" href="http://eric.ed.gov/?q=Conservation+AND+Laws&pg=5&id=EJ852869"><span id="translatedtitle">Energy and the <span class="hlt">Elliptical</span> Orbit</span></a></p> <p><a target="_blank" href="http://www.eric.ed.gov/ERICWebPortal/search/extended.jsp?_pageLabel=advanced">ERIC Educational Resources Information Center</a></p> <p>Nettles, Bill</p> <p>2009-01-01</p> <p>In the January 2007 issue of "The Physics Teacher," Prentis, Fulton, Hesse, and Mazzino describe a laboratory exercise in which students use a geometrical analysis inspired by Newton to show that an <span class="hlt">elliptical</span> orbit and an inverse-square law force go hand in hand. The historical, geometrical, and teamwork aspects of the exercise are useful and…</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://www.osti.gov/scitech/biblio/7045235','DOE-PATENT-XML'); return false;" href="http://www.osti.gov/scitech/biblio/7045235"><span id="translatedtitle">Wavelength meter having <span class="hlt">elliptical</span> wedge</span></a></p> <p><a target="_blank" href="http://www.osti.gov/doepatents">DOEpatents</a></p> <p>Hackel, R.P.; Feldman, M.</p> <p>1992-12-01</p> <p>A wavelength meter is disclosed which can determine the wavelength of a laser beam from a laser source within an accuracy range of two parts in 10[sup 8]. The wavelength meter has wedge having an <span class="hlt">elliptically</span> shaped face to the optical path of the laser source and includes interferometer plates which form a vacuum housing. 7 figs.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://www.osti.gov/scitech/servlets/purl/868570','DOE-PATENT-XML'); return false;" href="http://www.osti.gov/scitech/servlets/purl/868570"><span id="translatedtitle">Wavelength meter having <span class="hlt">elliptical</span> wedge</span></a></p> <p><a target="_blank" href="http://www.osti.gov/doepatents">DOEpatents</a></p> <p>Hackel, Richard P.; Feldman, Mark</p> <p>1992-01-01</p> <p>A wavelength meter is disclosed which can determine the wavelength of a laser beam from a laser source within an accuracy range of two parts in 10.sup.8. The wavelength meter has wedge having an <span class="hlt">elliptically</span> shaped face to the optical path of the laser source and includes interferometer plates which form a vacuum housing.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/1995A%26A...297L..71W','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/1995A%26A...297L..71W"><span id="translatedtitle">Cold dust in <span class="hlt">elliptical</span> galaxies.</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Wiklind, T.; Henkel, C.</p> <p>1995-05-01</p> <p>We have observed the λ1250 µm flux in 8 <span class="hlt">elliptical</span> galaxies using the MPIfR 7-channel bolometer system attachet to the IRAM 30-m telescope. Five of the galaxies are detected at more than 3σ, two are tentatively detected and for one we obtained an upper limit. For two of the detected galaxies, the CO(2-1) line makes a significant contribution to the measured λ1250 µm flux. A comparison of the λ1250 µm fluxes, corrected for the CO(2-1) line contribution, with IRAS 60 and 100µm data shows that there is a colt dust component (Td~<20K) in two of the <span class="hlt">ellipticals</span>. The other galaxies have λ1250 µm fluxes consistent with a one-temperature component, with Td typically between 20-30K.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/1989PhDT.........8B','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/1989PhDT.........8B"><span id="translatedtitle">Counterrotating cores in <span class="hlt">elliptical</span> galaxies</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Balcella, Marc Comas</p> <p></p> <p>The dynamics of the merger between a high- and a low-<span class="hlt">elliptical</span> galaxy was studied to understand how kinematically peculiar cores in <span class="hlt">elliptical</span> galaxies might form. Numerical simulations of mergers provide rotation curves, surface density profiles, surface density contour plots and velocity maps of the merger remnants, as well as diagnostics on the dynamics such as phase-space diagrams. This type of merger can create counterrotating cores. The core of the smaller galaxy, of higher density, is not disrupted by the primary tidal field and sinks to the center of the primary as an independent dynamical subsystem. Core counterrotation occurs only when the initial merger orbit is retrograde with respect to the pin of the primary. The remnant has higher effective radius and lower mean central surface density than the primary galaxy, but a smaller core radius. The adsorption of orbital energy and angular momentum by the primary particles greatly modifies the kinematic structure of the larger galaxy. Twisted rotation axes and isophote twists appear over the whole body of the remnant. These diagnostics may be used to determine whether observed peculiar cores might have formed via an <span class="hlt">elliptical-elliptical</span> merger. Galaxies with counterrotating cores should show a complex velocity field, isophotal irregularities, and, in general, a slow rotation in the main body of the galaxy. The present experiments are the first galaxy-satellite merger experiments involving an active, rotating secondary. They show that part of the orbital angular momentum is absorbed by the secondary, thus the secondary contributes to its own sinking: the sinking rate depends on the orientation of the secondary spin. Long-slit spectroscopic observations of NGC 3656 are reported.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/8897210','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/8897210"><span id="translatedtitle"><span class="hlt">Elliptic</span> Fourier analysis of mandibular shape.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Ferrario, V F; Sforza, C; Guazzi, M; Serrao, G</p> <p>1996-01-01</p> <p>Craniofacial growth and development involve both size and shape variations. Shape variations can be assessed independently from size using mathematical methods such as the <span class="hlt">elliptic</span> Fourier analysis, which allows a global evaluation of the shape of organs identified by their outlines independently from size, spatial orientation, and relation to reference planes. The mandibular outlines were digitized from the tracings of the Bolton standards (lateral view) from 1 to 18 years of age, and the age differences in shape independently from size were quantified using the <span class="hlt">elliptic</span> Fourier series. A "morphologic distance" MD (i.e., a measurement of differences in shape) between each younger mandible and the oldest one was computed using the relevant Fourier coefficients like the cartesian coordinates in standard metric measurements. MD equals 0 when the profiles are identical. MD (Y) between the Bolton standard at 18 years of age and all the other Bolton tracings were significantly <span class="hlt">correlated</span> (<span class="hlt">correlation</span> coefficient r = 0.987, P < or = 0.001) with age (X) (semi-logarithmic interpolation Y = -3.87.log(e) X + 13.593). Differences between the size-independent shape of the Bolton standard at 18 years and the relevant plot at 1 year were located at the chin, gonion, coronoid process, anterior border of the ramus. Size differences were measured from the areas enclosed by the mandibular outlines. Mandibular area (Y) increased about 2.58 times from 1 to 18 years of age (X) (Y = -0.071.X2 + 4.917.X + 35.904, r = 0.997, P < or = 0.001). The shape effect was largely overwhelmed by the very evident size increments, and it could be measured only using the proper mathematical methods. The method developed could also be applied to the comparison between healthy and diseased individuals.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016ASSL..418...15M','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016ASSL..418...15M"><span id="translatedtitle">The <span class="hlt">Intrinsic</span> Shape of Galaxy Bulges</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Méndez-Abreu, Jairo</p> <p></p> <p>The knowledge of the <span class="hlt">intrinsic</span> three-dimensional (3D) structure of galaxy components provides crucial information about the physical processes driving their formation and evolution. In this paper I discuss the main developments and results in the quest to better understand the 3D shape of galaxy bulges. I start by establishing the basic geometrical description of the problem. Our understanding of the <span class="hlt">intrinsic</span> shape of <span class="hlt">elliptical</span> galaxies and galaxy discs is then presented in a historical context, in order to place the role that the 3D structure of bulges play in the broader picture of galaxy evolution. Our current view on the 3D shape of the Milky Way bulge and future prospects in the field are also depicted.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016JMP....57j3302K','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016JMP....57j3302K"><span id="translatedtitle"><span class="hlt">Elliptic</span> Bessel processes and <span class="hlt">elliptic</span> Dyson models realized as temporally inhomogeneous processes</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Katori, Makoto</p> <p>2016-10-01</p> <p>The Bessel process with parameter D > 1 and the Dyson model of interacting Brownian motions with coupling constant β > 0 are extended to the processes in which the drift term and the interaction terms are given by the logarithmic derivatives of Jacobi's theta functions. They are called the <span class="hlt">elliptic</span> Bessel process, eBES(D), and the <span class="hlt">elliptic</span> Dyson model, eDYS(β), respectively. Both are realized on the circumference of a circle [0, 2πr) with radius r > 0 as temporally inhomogeneous processes defined in a finite time interval [0, t∗), t∗ < ∞. Transformations of them to Schrödinger-type equations with time-dependent potentials lead us to proving that eBES(D) and eDYS(β) can be constructed as the time-dependent Girsanov transformations of Brownian motions. In the special cases where D = 3 and β = 2, observables of the processes are defined and the processes are represented for them using the Brownian paths winding round a circle and pinned at time t∗. We show that eDYS(2) has the determinantal martingale representation for any observable. Then it is proved that eDYS(2) is determinantal for all observables for any finite initial configuration without multiple points. Determinantal processes are stochastic integrable systems in the sense that all spatio-temporal <span class="hlt">correlation</span> functions are given by determinants controlled by a single continuous function called the spatio-temporal <span class="hlt">correlation</span> kernel.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2014SIGMA..10..021S','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2014SIGMA..10..021S"><span id="translatedtitle">Commutative Families of the <span class="hlt">Elliptic</span> Macdonald Operator</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Saito, Yosuke</p> <p>2014-03-01</p> <p>In the paper [J. Math. Phys. 50 (2009), 095215, 42 pages], Feigin, Hashizume, Hoshino, Shiraishi, and Yanagida constructed two families of commuting operators which contain the Macdonald operator (commutative families of the Macdonald operator). They used the Ding-Iohara-Miki algebra and the trigonometric Feigin-Odesskii algebra. In the previous paper [arXiv:1301.4912], the present author constructed the <span class="hlt">elliptic</span> Ding-Iohara-Miki algebra and the free field realization of the <span class="hlt">elliptic</span> Macdonald operator. In this paper, we show that by using the <span class="hlt">elliptic</span> Ding-Iohara-Miki algebra and the <span class="hlt">elliptic</span> Feigin-Odesskii algebra, we can construct commutative families of the <span class="hlt">elliptic</span> Macdonald operator. In Appendix, we will show a relation between the <span class="hlt">elliptic</span> Macdonald operator and its kernel function by the free field realization.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/28360212','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/28360212"><span id="translatedtitle"><span class="hlt">Correlation</span> of (18)F-FDG PET and MR Apparent Diffusion Coefficient (ADC) Histogram Metrics with Survival in Diffuse <span class="hlt">Intrinsic</span> Pontine Glioma: A Report from the Pediatric Brain Tumor Consortium.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Zukotynski, Katherine; Vajapeyam, Sridhar; Fahey, Frederic H; Kocak, Mehmet; Brown, Douglas; Ricci, Kelsey; Onar-Thomas, Arzu; Fouladi, Maryam; Poussaint, Tina Young</p> <p>2017-03-30</p> <p>Rationale: To describe baseline (18)F-labeled 2-fluoro-2-deoxy-D-glucose positron emission tomography (FDG-PET) voxel characteristics in pediatric diffuse <span class="hlt">intrinsic</span> pontine glioma (DIPG) and to <span class="hlt">correlate</span> these metrics with baseline magnetic resonance (MR) apparent diffusion coefficient (ADC) histogram metrics, progression-free survival (PFS) and overall survival (OS). Methods: Baseline brain FDG-PET and MR scans were obtained in 33 children from Pediatric Brain Tumor Consortium (PBTC) clinical DIPG trials. FDG-PET, post-gadolinium (PG) and ADC images were registered to baseline fluid attenuation inversion recovery (FLAIR) images. Three-dimensional regions of interest on FLAIR and PG images and FDG-PET and ADC histograms were generated. Metrics evaluated included peak number, skewness and kurtosis. <span class="hlt">Correlation</span> between PET and ADC histogram metrics was evaluated. PET pixel values within the ROI for each tumor were plotted against ADC values. Association of these imaging markers with survival was described. Results: PET histograms were almost always unimodal (94% vs. 6% bimodal). None of the PET histogram parameters (skewness or kurtosis) had a significant association with PFS, although a higher PET PG skewness tended towards less favorable PFS (Hazard Ratio (95% CI)=3.48 (0.75, 16.28); P = 0.11). There was a significant association of higher ADC PG skewness with shorter PFS (Hazard Ratio (95% CI)=2.56 (1.11, 5.91); P = 0.028) and the suggestion that this also led to shorter OS (Hazard Ratio (95% CI)=2.18 (0.95, 5.04); P = 0.067). Higher ADC PG kurtosis tended towards shorter PFS (Hazard Ratio (95% CI)=1.30 (0.98, 1.74); P = 0.073). In a number of cases, PET and ADC pixel values were negatively <span class="hlt">correlated</span> using the Pearson <span class="hlt">correlation</span> coefficient. Further, the level of PET and ADC <span class="hlt">correlation</span> was significantly positively associated with PFS; tumors with higher values of ADC-PET <span class="hlt">correlation</span> had more favorable PFS (Hazard Ratio (95% CI)=0.17 (0.03, 0.89), P = 0</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/8117727','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/8117727"><span id="translatedtitle">Influence of substrates and MgADP on the time-resolved <span class="hlt">intrinsic</span> fluorescence of phosphofructokinase from Escherichia coli. <span class="hlt">Correlation</span> of tryptophan dynamics to coupling entropy.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Johnson, J L; Reinhart, G D</p> <p>1994-03-08</p> <p>The influence of that MgADP and the substrate ligands MgATP and fructose 6-phosphate (Fru-6-P) have on the structure of E. coli phosphofructokinase (PFK) in the vicinity of the single tryptophan that exists in each subunit has been examined by employing both steady-state and time-resolved measurements of the tryptophan fluorescence. The accessibility of the tryptophan to iodide quenching is over 1 order of magnitude less than experienced by N-acetyltryptophanamide in solution but varies nonetheless with the state of ligation. Most, but not all, of these changes <span class="hlt">correlate</span> with changes in the degree of local motion available to the tryptophan side chain as determined by steady-state and time-resolved polarization measurements. When the data obtained from differential polarization experiments are fit to a model in which the motion of the tryptophan side chain is able to move with high frequency within a cone of limited amplitude as part of an otherwise slowly tumbling spherical protein, it was found that ligands primarily affect the amplitude of the available local motion. By interpreting these effects with reference to the disproportionation equilibria which define the negative coupling free energy between MgADP and Fru-6-P and the positive coupling free energy between MgADP and MgATP, it is apparent that changes in the local motion amplitudes <span class="hlt">correlate</span> with the sign of the component coupling entropy previously determined from van't Hoff analyses (Johnson & Reinhart, 1994).(ABSTRACT TRUNCATED AT 250 WORDS)</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19950047891&hterms=dark+matter&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D30%26Ntt%3Ddark%2Bmatter','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19950047891&hterms=dark+matter&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D30%26Ntt%3Ddark%2Bmatter"><span id="translatedtitle">Dark matter in <span class="hlt">elliptical</span> galaxies</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Carollo, C. M.; Zeeuw, P. T. DE; Marel, R. P. Van Der; Danziger, I. J.; Qian, E. E.</p> <p>1995-01-01</p> <p>We present measurements of the shape of the stellar line-of-sight velocity distribution out to two effective radii along the major axes of the four <span class="hlt">elliptical</span> galaxies NGC 2434, 2663, 3706, and 5018. The velocity dispersion profiles are flat or decline gently with radius. We compare the data to the predictions of f = f(E, L(sub z)) axisymmetric models with and without dark matter. Strong tangential anisotropy is ruled out at large radii. We conclude from our measurements that massive dark halos must be present in three of the four galaxies, while for the fourth galaxy (NGC 2663) the case is inconclusive.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/1989PhDT........65B','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/1989PhDT........65B"><span id="translatedtitle">Counterrotating Cores in <span class="hlt">Elliptical</span> Galaxies.</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Balcells, Marc Comas</p> <p></p> <p>The dynamics of the merger between a high- and a low-luminosity <span class="hlt">elliptical</span> galaxy has been studied to understand how kinematically peculiar cores in <span class="hlt">elliptical</span> galaxies might form. Numerical simulations of mergers provide rotation curves, surface density profiles, surface density contour plots and velocity maps of the merger remnants, as well as diagnostics on the dynamics such as phase-space diagrams. This type of merger can create counterrotating cores. The core of the smaller galaxy, of higher density, is not disrupted by the primary tidal field and sinks to the center of the primary as an independent dynamical subsystem. Core counterrotation occurs only when the initial merger orbit is retrograde with respect to the spin of the primary. The remnant has higher effective radius and lower mean central surface density than the primary galaxy, but a smaller core radius. The adsorption of orbital energy and angular momentum by the primary particles greatly modifies the kinematic structure of the larger galaxy. Twisted rotation axes and isophote twists appear over the whole body of the remnant. These diagnostics may be used to determine whether observed peculiar cores might have formed via an <span class="hlt">elliptical-elliptical</span> merger. Galaxies with counterrotating cores should show a complex velocity field, isophotal irregularities, and, in general, a slow rotation in the main body of the galaxy. The present experiments are the first galaxy-satellite merger experiments involving an active, rotating secondary. They show that part of the orbital angular momentum is absorbed by the secondary, thus the secondary contributes to its own sinking: the sinking rate depends on the orientation of the secondary spin. Long-slit spectroscopic observations of NGC 3656 are reported. Rotation curves indicate that NGC 3656 contains a core spinning in a direction perpendicular to the rotation in the main body of the galaxy. Velocity reversals at intermediate radii are also observed. These features</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017PhRvC..95a4913G','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017PhRvC..95a4913G"><span id="translatedtitle">Skewness of <span class="hlt">elliptic</span> flow fluctuations</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Giacalone, Giuliano; Yan, Li; Noronha-Hostler, Jacquelyn; Ollitrault, Jean-Yves</p> <p>2017-01-01</p> <p>Using event-by-event hydrodynamic calculations, we find that the fluctuations of the <span class="hlt">elliptic</span> flow (v2) in the reaction plane have a negative skew. We compare the skewness of v2 fluctuations to that of initial eccentricity fluctuations. We show that skewness is the main effect lifting the degeneracy between higher-order cumulants, with negative skew corresponding to the hierarchy v2{4 } >v2{6 } observed in Pb+Pb collisions at the CERN Large Hadron Collider. We describe how the skewness can be measured experimentally and show that hydrodynamics naturally reproduces its magnitude and centrality dependence.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/1995RScI...66.1895H','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/1995RScI...66.1895H"><span id="translatedtitle">Advanced Light Source <span class="hlt">elliptical</span> wiggler</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Hoyer, E.; Akre, J.; Humphries, D.; Marks, S.; Minamihara, Y.; Pipersky, P.; Plate, D.; Schlueter, R.</p> <p>1995-02-01</p> <p>A 3.5-m-long <span class="hlt">elliptical</span> wiggler, optimized to produce <span class="hlt">elliptically</span> polarized light in the 50 eV to 10 keV range, is currently under design and construction at the Advanced Light Source at Lawrence Berkeley Laboratory. Calculations of spectral performance show that the flux of circularly polarized photons exceeds 1013 photons/s over the 50 eV to 10 keV operating range for current of 0.4 A and 1.5 GeV electron energy. This device features vertical and horizontal magnetic structures of 14 and 141/2 periods, respectively. The period length is 20.0 cm. The vertical structure is a hybrid permanent magnet design with tapered pole tips that produce a peak field of 2.0 T. The horizontal structure is an iron core electromagnetic design, shifted longitudinally 1/4 period, that is tucked between the upper and lower vertical magnetic structure sections. A maximum peak oscillating field of 0.095 T at a frequency up to 1 Hz will be achieved by excitation of the horizontal poles with a trapezoidal current waveform. The vacuum chamber is an unconventional design that is removable from the magnetic structure, after magnetic measurements, for UHV processing. The chamber is fabricated from non-magnetic stainless steel to minimize the effects of eddy currents. Device design is presented.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2007PhDT........29I','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2007PhDT........29I"><span id="translatedtitle"><span class="hlt">Elliptic</span> constructions of hyperkahler metrics</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Ionas, Radu Aurelian</p> <p></p> <p>In this dissertation we develop a twistor-theoretic method of constructing hyperkahler metrics from holomorphic functions and <span class="hlt">elliptic</span> curves. We obtain, among other things, new results concerning the Atiyah-Hitchin manifold, asymptotically locally Euclidean spaces of type Dn and certain Swann bundles. For example, in the Atiyah-Hitchin case we derive in an explicit holomorphic coordinate basis closed-form formulas for the metric, the holomorphic symplectic form and all three Kahler potentials. The equation describing an asymptotically locally Euclidean space of type Dn is found to admit an algebraic formulation in terms of the group law on a Weierstrass cubic. This curve has the structure of a Cayley cubic for a pencil generated by two transversal plane conics, that is, it takes the form Y2 = det( A+XB ), where A and B are the defining 3 x 3 matrices of the conics. In this light, the equation can be interpreted as the closure condition for an <span class="hlt">elliptic</span> billiard trajectory tangent to the conic B and bouncing into various conics of the pencil determined by the positions of the monopoles.</p> </li> </ol> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_3");'>3</a></li> <li><a href="#" onclick='return showDiv("page_4");'>4</a></li> <li class="active"><span>5</span></li> <li><a href="#" onclick='return showDiv("page_6");'>6</a></li> <li><a href="#" onclick='return showDiv("page_7");'>7</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div><!-- col-sm-12 --> </div><!-- row --> </div><!-- page_5 --> <div id="page_6" class="hiddenDiv"> <div class="row"> <div class="col-sm-12"> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_4");'>4</a></li> <li><a href="#" onclick='return showDiv("page_5");'>5</a></li> <li class="active"><span>6</span></li> <li><a href="#" onclick='return showDiv("page_7");'>7</a></li> <li><a href="#" onclick='return showDiv("page_8");'>8</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div> </div> <div class="row"> <div class="col-sm-12"> <ol class="result-class" start="101"> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016NuPhB.910..431O','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016NuPhB.910..431O"><span id="translatedtitle">Matrix factorizations and <span class="hlt">elliptic</span> fibrations</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Omer, Harun</p> <p>2016-09-01</p> <p>I use matrix factorizations to describe branes at simple singularities of <span class="hlt">elliptic</span> fibrations. Each node of the corresponding Dynkin diagrams of the ADE-type singularities is associated with one indecomposable matrix factorization which can be deformed into one or more factorizations of lower rank. Branes with internal fluxes arise naturally as bound states of the indecomposable factorizations. Describing branes in such a way avoids the need to resolve singularities. This paper looks at gauge group breaking from E8 fibers down to SU (5) fibers due to the relevance of such fibrations for local F-theory GUT models. A purpose of this paper is to understand how the deformations of the singularity are understood in terms of its matrix factorizations. By systematically factorizing the <span class="hlt">elliptic</span> fiber equation, this paper discusses geometries which are relevant for building semi-realistic local models. In the process it becomes evident that breaking patterns which are identical at the level of the Kodaira type of the fibers can be inequivalent at the level of matrix factorizations. Therefore the matrix factorization picture supplements information which the conventional less detailed descriptions lack.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19910011768','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19910011768"><span id="translatedtitle">Pressure algorithm for <span class="hlt">elliptic</span> flow calculations with the PDF method</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Anand, M. S.; Pope, S. B.; Mongia, H. C.</p> <p>1991-01-01</p> <p>An algorithm to determine the mean pressure field for <span class="hlt">elliptic</span> flow calculations with the probability density function (PDF) method is developed and applied. The PDF method is a most promising approach for the computation of turbulent reacting flows. Previous computations of <span class="hlt">elliptic</span> flows with the method were in conjunction with conventional finite volume based calculations that provided the mean pressure field. The algorithm developed and described here permits the mean pressure field to be determined within the PDF calculations. The PDF method incorporating the pressure algorithm is applied to the flow past a backward-facing step. The results are in good agreement with data for the reattachment length, mean velocities, and turbulence quantities including triple <span class="hlt">correlations</span>.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=5059469','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=5059469"><span id="translatedtitle">Thermopile detector of light <span class="hlt">ellipticity</span></span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Lu, Feng; Lee, Jongwon; Jiang, Aiting; Jung, Seungyong; Belkin, Mikhail A.</p> <p>2016-01-01</p> <p>Polarimetric imaging is widely used in applications from material analysis to biomedical diagnostics, vision and astronomy. The degree of circular polarization, or light <span class="hlt">ellipticity</span>, is associated with the S3 Stokes parameter which is defined as the difference in the intensities of the left- and right-circularly polarized components of light. Traditional way of determining this parameter relies on using several external optical elements, such as polarizers and wave plates, along with conventional photodetectors, and performing at least two measurements to distinguish left- and right-circularly polarized light components. Here we theoretically propose and experimentally demonstrate a thermopile photodetector element that provides bipolar voltage output directly proportional to the S3 Stokes parameter of the incident light. PMID:27703152</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19840020446','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19840020446"><span id="translatedtitle"><span class="hlt">Elliptical</span> orbit performance computer program</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Myler, T. R.</p> <p>1981-01-01</p> <p>A FORTRAN coded computer program which generates and plots <span class="hlt">elliptical</span> orbit performance capability of space boosters for presentation purposes is described. Orbital performance capability of space boosters is typically presented as payload weight as a function of perigee and apogee altitudes. The parameters are derived from a parametric computer simulation of the booster flight which yields the payload weight as a function of velocity and altitude at insertion. The process of converting from velocity and altitude to apogee and perigee altitude and plotting the results as a function of payload weight is mechanized with the ELOPE program. The program theory, user instruction, input/output definitions, subroutine descriptions and detailed FORTRAN coding information are included.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016IJBC...2650095K','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016IJBC...2650095K"><span id="translatedtitle"><span class="hlt">Elliptic</span> Functions with Disconnected Julia Sets</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Koss, Lorelei</p> <p>2016-06-01</p> <p>In this paper, we investigate <span class="hlt">elliptic</span> functions of the form fΛ = 1/(1 + (℘Λ)2), where ℘Λ is the Weierstrass <span class="hlt">elliptic</span> function on a real rhombic lattice. We show that a typical function in this family has a superattracting fixed point at the origin and five other equivalence classes of critical points. We investigate conditions on the lattice which guarantee that fΛ has a double toral band, and we show that this family contains the first known examples of <span class="hlt">elliptic</span> functions for which the Julia set is disconnected but not Cantor.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19800019196','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19800019196"><span id="translatedtitle">Stresses and deformations in <span class="hlt">elliptical</span> contacts</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Hamrock, B. J.</p> <p>1980-01-01</p> <p>Topics presented deal with defining conformal and nonconformal surfaces, curvature sum and difference, and surface and subsurface stresses in <span class="hlt">elliptical</span> contacts. Load-deflection relationships for nonconformal contacts are developed. The deformation within the contact is, among other things, a function of the <span class="hlt">ellipticity</span> parameter and <span class="hlt">elliptic</span> integrals of the first and second kinds. Simplified expressions that allow quick calculations of the deformation to be made simply from a knowledge of the applied load, the material properties, and the geometry of the contacting elements are presented.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19930035159&hterms=Aachen&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D60%26Ntt%3DAachen','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19930035159&hterms=Aachen&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D60%26Ntt%3DAachen"><span id="translatedtitle">The noise from supersonic <span class="hlt">elliptic</span> jets</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Morris, Philip J.; Bhat, Thonse R. S.</p> <p>1992-01-01</p> <p>This paper presents calculations of the noise radiated by a supersonic <span class="hlt">elliptic</span> jet. The large scale structures in the jet, that are the predominant source of noise in the downstream direction, are modeled as instability waves. The evolution of the instability waves is determined by a local, linear, inviscid analysis. An expression is derived for the acoustic field outside the jet and the far field directivity associated with each instability wave. Calculations are performed for a Mach 1.5 <span class="hlt">elliptic</span> jet with aspect ratio 2:1 and a Mach 2.0 <span class="hlt">elliptic</span> jet with aspect ratio 2:1 and a Mach 2.0 <span class="hlt">elliptic</span> jet with aspect ratio 3:1. The mean flow development is taken from experimental results. Comparisons are made with far field acoustic measurements.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/9358446','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/9358446"><span id="translatedtitle">Theory of the quadrature <span class="hlt">elliptic</span> birdcage coil.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Leifer, M C</p> <p>1997-11-01</p> <p>This paper presents the theory of the quadrature birdcage coil wound on an <span class="hlt">elliptic</span> cylindrical former. A conformal transformation of the ellipse to a circular geometry is used to derive the optimal sampling of the continuous surface current distribution to produce uniform magnetic fields within an <span class="hlt">elliptic</span> cylinder. The analysis is rigorous for ellipses of any aspect ratio and shows how to produce quadrature operation of the <span class="hlt">elliptic</span> birdcage with a conventional hybrid combiner. Insight gained from the transformation is also used to analyze field homogeneity, find the optimal RF shield shape, and specify component values to produce the correct current distribution in practice. Measurements and images from a 16-leg <span class="hlt">elliptic</span> birdcage coil at both low and high frequencies show good quadrature performance, homogeneity, and sensitivity.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19810004847','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19810004847"><span id="translatedtitle">Elastohydrodynamic lubrication of <span class="hlt">elliptical</span> contacts</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Hamrock, B. J.</p> <p>1981-01-01</p> <p>The determination of the minimum film thickness within contact is considered for both fully flooded and starved conditions. A fully flooded conjunction is one in which the film thickness is not significantly changed when the amount of lubricant is increased. The fully flooded results presented show the influence of contact geometry on minimum film thickness as expressed by the <span class="hlt">ellipticity</span> parameter and the dimensionless speed, load, and materials parameters. These results are applied to materials of high elastic modulus (hard EHL), such as metal, and to materials of low elastic modulus(soft EHL), such as rubber. In addition to the film thickness equations that are developed, contour plots of pressure and film thickness are given which show the essential features of elastohydrodynamically lubricated conjunctions. The crescent shaped region of minimum film thickness, with its side lobes in which the separation between the solids is a minimum, clearly emerges in the numerical solutions. In addition to the 3 presented for the fully flooded results, 15 more cases are used for hard EHL contacts and 18 cases are used for soft EHL contacts in a theoretical study of the influence of lubricant starvation on film thickness and pressure. From the starved results for both hard and soft EHL contacts, a simple and important dimensionless inlet boundary distance is specified. This inlet boundary distance defines whether a fully flooded or a starved condition exists in the contact. Contour plots of pressure and film thickness in and around the contact are shown for conditions.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/1993JMP....34.2257C','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/1993JMP....34.2257C"><span id="translatedtitle"><span class="hlt">Elliptical</span> billiards and hyperelliptic functions</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Crespi, Bruno; Chang, Shau-Jin; Shi, Kang-Jie</p> <p>1993-06-01</p> <p>The geometrical properties of the <span class="hlt">elliptical</span> billiard system are related to Poncelet's theorem. This theorem states that if a polygon is inscribed in a conic and circumscribed about a second conic, every point of the former conic is a vertex of a polygon with the same number of sides and the same perimeter. Chang and Friedberg have extended this theorem to three and higher dimensions. They have shown that the geometrical properties of the hyperelliptic billiard system are related to the algebraic character of a Poincaré map in the phase space. The geometrical and algebraic properties of the system can be understood in terms of the analytical structure of the equations of motion. These equations form a complete system of Abelian integrals. The integrability of the physical system is reflected by the topology of the Riemann surfaces associated to these integrals. The algebraic properties are connected with the existence of addition formulas for hyperelliptic functions. The main purpose of this study is to establish such a connection, and to provide an algebraic proof of Poncelet's theorem in three and higher dimensions.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2010JMP....51c2901F','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2010JMP....51c2901F"><span id="translatedtitle">Pendulum, <span class="hlt">elliptic</span> functions, and relative cohomology classes</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Françoise, J.-P.; Garrido, P. L.; Gallavotti, G.</p> <p>2010-03-01</p> <p>Revisiting canonical integration of the classical pendulum around its unstable equilibrium, normal hyperbolic canonical coordinates are constructed and an identity between <span class="hlt">elliptic</span> functions is found whose proof can be based on symplectic geometry and global relative cohomology. Alternatively it can be reduced to a well known identity between <span class="hlt">elliptic</span> functions. Normal canonical action-angle variables are also constructed around the stable equilibrium and a corresponding identity is exhibited.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://www.dtic.mil/docs/citations/ADA158265','DTIC-ST'); return false;" href="http://www.dtic.mil/docs/citations/ADA158265"><span id="translatedtitle"><span class="hlt">Intrinsic</span> Nilpotent Approximation.</span></a></p> <p><a target="_blank" href="https://publicaccess.dtic.mil/psm/api/service/search/search">DTIC Science & Technology</a></p> <p></p> <p>1985-06-01</p> <p>RD-A1II58 265 <span class="hlt">INTRINSIC</span> NILPOTENT APPROXIMATION(U) MASSACHUSETTS INST 1/2 OF TECH CAMBRIDGE LAB FOR INFORMATION AND, DECISION UMCLRSSI SYSTEMS C...TYPE OF REPORT & PERIOD COVERED <span class="hlt">Intrinsic</span> Nilpotent Approximation Technical Report 6. PERFORMING ORG. REPORT NUMBER LIDS-R-1482 7. AUTHOR(.) S...certain infinite-dimensional filtered Lie algebras L by (finite-dimensional) graded nilpotent Lie algebras or g . where x E M, (x,,Z) E T*M/O. It</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016ArRMA.219..255A','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016ArRMA.219..255A"><span id="translatedtitle">Lipschitz Regularity for <span class="hlt">Elliptic</span> Equations with Random Coefficients</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Armstrong, Scott N.; Mourrat, Jean-Christophe</p> <p>2016-01-01</p> <p>We develop a higher regularity theory for general quasilinear <span class="hlt">elliptic</span> equations and systems in divergence form with random coefficients. The main result is a large-scale L ∞-type estimate for the gradient of a solution. The estimate is proved with optimal stochastic integrability under a one-parameter family of mixing assumptions, allowing for very weak mixing with non-integrable <span class="hlt">correlations</span> to very strong mixing (for example finite range of dependence). We also prove a quenched L 2 estimate for the error in homogenization of Dirichlet problems. The approach is based on subadditive arguments which rely on a variational formulation of general quasilinear divergence-form equations.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2006EAS....20..139M','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2006EAS....20..139M"><span id="translatedtitle">Kinematical and Dynamical Modeling of <span class="hlt">Elliptical</span> Galaxies</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Mamon, G. A.; Łokas, E.; Dekel, A.; Stoehr, F.; Cox, T. J.</p> <p></p> <p>Elements of kinematical and dynamical modeling of <span class="hlt">elliptical</span> galaxies are presented. In projection, NFW models resemble Sérsic models, but with a very narrow range of shapes (m=3±1). The total density profile of <span class="hlt">ellipticals</span> cannot be NFW-like because the predicted local M/L and aperture velocity dispersion within an effective radius (R_e) are much lower than observed. Stars must then dominate <span class="hlt">ellipticals</span> out to a few R_e. Fitting an NFW model to the total density profile of Sérsic+NFW (stars+dark matter [DM]) <span class="hlt">ellipticals</span> results in very high concentration parameters, as found by X-ray observers. Kinematical modeling of <span class="hlt">ellipticals</span> assuming an isotropic NFW DM model underestimates M/L at the virial radius by a factor of 1.6 to 2.4, because dissipationless ΛCDM halos have slightly different density profiles and slightly radial velocity anisotropy. In N-body+gas simulations of <span class="hlt">ellipticals</span> as merger remnants of spirals embedded in DM halos, the slope of the DM density profile is steeper when the initial spiral galaxies are gas-rich. The Hansen & Moore (2006) relation between anisotropy and the slope of the density profile breaks down for gas and DM, but the stars follow an analogous relation with slightly less radial anisotropies for a given density slope. Using kurtosis (h_4) to infer anisotropy in <span class="hlt">ellipticals</span> is dangerous, as h4 is also sensitive to small levels of rotation. The stationary Jeans equation provides accurate masses out to 8 R_e. The discrepancy between the modeling of Romanowsky et al. (2003), indicating a dearth of DM in <span class="hlt">ellipticals</span>, and the simulations analyzed by Dekel et al. (2005), which match the spectroscopic observations of <span class="hlt">ellipticals</span>, is partly due to radial anisotropy and to observing oblate <span class="hlt">ellipticals</span> face-on. However, one of the 15 solutions to the orbit modeling of Romanowsky et al. is found to have an amount and concentration of DM consistent with ΛCDM predictions.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017SuScT..30c3001S','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017SuScT..30c3001S"><span id="translatedtitle">Fabrication of <span class="hlt">elliptical</span> SRF cavities</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Singer, W.</p> <p>2017-03-01</p> <p>The technological and metallurgical requirements of material for high-gradient superconducting cavities are described. High-purity niobium, as the preferred metal for the fabrication of superconducting accelerating cavities, should meet exact specifications. The content of interstitial impurities such as oxygen, nitrogen, and carbon must be below 10 μg g-1. The hydrogen content should be kept below 2 μg g-1 to prevent degradation of the quality factor (Q-value) under certain cool-down conditions. The material should be free of flaws (foreign material inclusions or cracks and laminations) that can initiate a thermal breakdown. Traditional and alternative cavity mechanical fabrication methods are reviewed. Conventionally, niobium cavities are fabricated from sheet niobium by the formation of half-cells by deep drawing, followed by trim machining and electron beam welding. The welding of half-cells is a delicate procedure, requiring intermediate cleaning steps and a careful choice of weld parameters to achieve full penetration of the joints. A challenge for a welded construction is the tight mechanical and electrical tolerances. These can be maintained by a combination of mechanical and radio-frequency measurements on half-cells and by careful tracking of weld shrinkage. The main aspects of quality assurance and quality management are mentioned. The experiences of 800 cavities produced for the European XFEL are presented. Another cavity fabrication approach is slicing discs from the ingot and producing cavities by deep drawing and electron beam welding. Accelerating gradients at the level of 35-45 MV m-1 can be achieved by applying electrochemical polishing treatment. The single-crystal option (grain boundary free) is discussed. It seems that in this case, high performance can be achieved by a simplified treatment procedure. Fabrication of the <span class="hlt">elliptical</span> resonators from a seamless pipe as an alternative is briefly described. This technology has yielded good</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19950056918&hterms=brecht&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3Dbrecht','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19950056918&hterms=brecht&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3Dbrecht"><span id="translatedtitle">Consideration of the Martian magnetotail as evidence for an <span class="hlt">intrinsic</span> magnetic field</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Brecht, Stephen H.</p> <p>1995-01-01</p> <p>It has been suggested by Verigin et al. (1993) that the response of the Martian magnetotail to changes in the solar wind ram pressure indicates the presence of an <span class="hlt">intrinsic</span> dipole magnetic field. 3-D hybrid particle simulations of Mars were performed including the magnetotail regions. The simulations are in agreement with published Phobos 2 data from the 3 <span class="hlt">elliptical</span> orbits and reproduce the magnetopause diameter dependence on the solar wind ram pressure reported by Verigin et al. (1993). However, the simulations were performed with no <span class="hlt">intrinsic</span> field present, indicating that the dependence of the magnetotail width on ram pressure, is not a discriminator for the presence of the <span class="hlt">intrinsic</span> field.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2001ApJ...563..527G','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2001ApJ...563..527G"><span id="translatedtitle">Ultraluminous Infrared Mergers: <span class="hlt">Elliptical</span> Galaxies in Formation?</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Genzel, R.; Tacconi, L. J.; Rigopoulou, D.; Lutz, D.; Tecza, M.</p> <p>2001-12-01</p> <p>We report high-quality near-IR spectroscopy of 12 ultraluminous infrared galaxy mergers (ULIRGs). Our new VLT and Keck data provide ~0.5" resolution, stellar and gas kinematics of these galaxies, most of which are compact systems in the last merger stages. We confirm that ULIRG mergers are ``<span class="hlt">ellipticals</span> in formation.'' Random motions dominate their stellar dynamics, but significant rotation is common. Gasdynamics and stellar dynamics are decoupled in most systems. ULIRGs fall on or near the fundamental plane of hot stellar systems, and especially on its less evolution-sensitive, reff-σ projection. The ULIRG velocity dispersion distribution, their location in the fundamental plane, and their distribution of vrotsini/σ closely resemble those of intermediate-mass (~L*), <span class="hlt">elliptical</span> galaxies with moderate rotation. As a group ULIRGs do not resemble giant <span class="hlt">ellipticals</span> with large cores and little rotation. Our results are in good agreement with other recent studies indicating that disky <span class="hlt">ellipticals</span> with compact cores or cusps can form through dissipative mergers of gas-rich disk galaxies while giant <span class="hlt">ellipticals</span> with large cores have a different formation history. Based on observations at the European Southern Observatory, Chile (ESO 65.N-0266, 65.N-0289), and on observations at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, The University of California, and the National Aeronautics and Space Administration. The Keck Observatory was made possible by the general financial support by the W. M. Keck Foundation.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2003APS..MAR.Z9013H','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2003APS..MAR.Z9013H"><span id="translatedtitle"><span class="hlt">Intrinsic</span> Patterns of Human Activity</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Hu, Kun; Ivanov, Plamen Ch.; Chen, Zhi; Hilton, Michael; Stanley, H. Eugene; Shea, Steven</p> <p>2003-03-01</p> <p>Activity is one of the defining features of life. Control of human activity is complex, being influenced by many factors both extrinsic and <span class="hlt">intrinsic</span> to the body. The most obvious extrinsic factors that affect activity are the daily schedule of planned events, such as work and recreation, as well as reactions to unforeseen or random events. These extrinsic factors may account for the apparently random fluctuations in human motion observed over short time scales. The most obvious <span class="hlt">intrinsic</span> factors are the body clocks including the circadian pacemaker that influences our sleep/wake cycle and ultradian oscillators with shorter time scales [2, 3]. These <span class="hlt">intrinsic</span> rhythms may account for the underlying regularity in average activity level over longer periods of up to 24 h. Here we ask if the known extrinsic and <span class="hlt">intrinsic</span> factors fully account for all complex features observed in recordings of human activity. To this end, we measure activity over two weeks from forearm motion in subjects undergoing their regular daily routine. Utilizing concepts from statistical physics, we demonstrate that during wakefulness human activity possesses previously unrecognized complex dynamic patterns. These patterns of activity are characterized by robust fractal and nonlinear dynamics including a universal probability distribution and long-range power-law <span class="hlt">correlations</span> that are stable over a wide range of time scales (from minutes to hours). Surprisingly, we find that these dynamic patterns are unaffected by changes in the average activity level that occur within individual subjects throughout the day and on different days of the week, and between subjects. Moreover, we find that these patterns persist when the same subjects undergo time-isolation laboratory experiments designed to account for the phase of the circadian pacemaker, and control the known extrinsic factors by restricting behaviors and manipulating scheduled events including the sleep/wake cycle. We attribute these newly</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/pages/biblio/1183854-intrinsic-alignments-galaxies-massiveblack-ii-simulation-analysis-two-point-statistics','SCIGOV-DOEP'); return false;" href="https://www.osti.gov/pages/biblio/1183854-intrinsic-alignments-galaxies-massiveblack-ii-simulation-analysis-two-point-statistics"><span id="translatedtitle"><span class="hlt">Intrinsic</span> alignments of galaxies in the MassiveBlack-II simulation: Analysis of two-point statistics</span></a></p> <p><a target="_blank" href="http://www.osti.gov/pages">DOE PAGES</a></p> <p>Tenneti, Ananth; Singh, Sukhdeep; Mandelbaum, Rachel; ...</p> <p>2015-03-11</p> <p>The <span class="hlt">intrinsic</span> alignment of galaxies with the large-scale density field in an important astrophysical contaminant in upcoming weak lensing surveys. We present detailed measurements of the galaxy <span class="hlt">intrinsic</span> alignments and associated <span class="hlt">ellipticity</span>-direction (ED) and projected shape (wg₊) <span class="hlt">correlation</span> functions for galaxies in the cosmological hydrodynamic MassiveBlack-II (MB-II) simulation. We carefully assess the effects on galaxy shapes, misalignment of the stellar component with the dark matter shape and two-point statistics of iterative weighted (by mass and luminosity) definitions of the (reduced and unreduced) inertia tensor. We find that iterative procedures must be adopted for a reliable measurement of the reduced tensormore » but that luminosity versus mass weighting has only negligible effects. Both ED and wg₊ <span class="hlt">correlations</span> increase in amplitude with subhalo mass (in the range of 10¹⁰ – 6.0 X 10¹⁴h⁻¹ M⊙), with a weak redshift dependence (from z = 1 to z = 0.06) at fixed mass. At z ~ 0.3, we predict a wg₊ that is in reasonable agreement with SDSS LRG measurements and that decreases in amplitude by a factor of ~ 5–18 for galaxies in the LSST survey. We also compared the <span class="hlt">intrinsic</span> alignment of centrals and satellites, with clear detection of satellite radial alignments within the host halos. Finally, we show that wg₊ (using subhalos as tracers of density and wδ (using dark matter density) predictions from the simulations agree with that of non-linear alignment models (NLA) at scales where the 2-halo term dominates in the <span class="hlt">correlations</span> (and tabulate associated NLA fitting parameters). The 1-halo term induces a scale dependent bias at small scales which is not modeled in the NLA model.« less</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://www.osti.gov/scitech/servlets/purl/1183854','SCIGOV-STC'); return false;" href="http://www.osti.gov/scitech/servlets/purl/1183854"><span id="translatedtitle"><span class="hlt">Intrinsic</span> alignments of galaxies in the MassiveBlack-II simulation: Analysis of two-point statistics</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Tenneti, Ananth; Singh, Sukhdeep; Mandelbaum, Rachel; Matteo, Tiziana Di; Feng, Yu; Khandai, Nishikanta</p> <p>2015-03-11</p> <p>The <span class="hlt">intrinsic</span> alignment of galaxies with the large-scale density field in an important astrophysical contaminant in upcoming weak lensing surveys. We present detailed measurements of the galaxy <span class="hlt">intrinsic</span> alignments and associated <span class="hlt">ellipticity</span>-direction (ED) and projected shape (w<sub>g</sub>₊) <span class="hlt">correlation</span> functions for galaxies in the cosmological hydrodynamic MassiveBlack-II (MB-II) simulation. We carefully assess the effects on galaxy shapes, misalignment of the stellar component with the dark matter shape and two-point statistics of iterative weighted (by mass and luminosity) definitions of the (reduced and unreduced) inertia tensor. We find that iterative procedures must be adopted for a reliable measurement of the reduced tensor but that luminosity versus mass weighting has only negligible effects. Both ED and w<sub>g</sub>₊ <span class="hlt">correlations</span> increase in amplitude with subhalo mass (in the range of 10¹⁰ – 6.0 X 10¹⁴h⁻¹ M<sub>⊙</sub>), with a weak redshift dependence (from z = 1 to z = 0.06) at fixed mass. At z ~ 0.3, we predict a w<sub>g</sub>₊ that is in reasonable agreement with SDSS LRG measurements and that decreases in amplitude by a factor of ~ 5–18 for galaxies in the LSST survey. We also compared the <span class="hlt">intrinsic</span> alignment of centrals and satellites, with clear detection of satellite radial alignments within the host halos. Finally, we show that w<sub>g</sub>₊ (using subhalos as tracers of density and w<sub>δ</sub> (using dark matter density) predictions from the simulations agree with that of non-linear alignment models (NLA) at scales where the 2-halo term dominates in the <span class="hlt">correlations</span> (and tabulate associated NLA fitting parameters). The 1-halo term induces a scale dependent bias at small scales which is not modeled in the NLA model.</p> </li> </ol> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_4");'>4</a></li> <li><a href="#" onclick='return showDiv("page_5");'>5</a></li> <li class="active"><span>6</span></li> <li><a href="#" onclick='return showDiv("page_7");'>7</a></li> <li><a href="#" onclick='return showDiv("page_8");'>8</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div><!-- col-sm-12 --> </div><!-- row --> </div><!-- page_6 --> <div id="page_7" class="hiddenDiv"> <div class="row"> <div class="col-sm-12"> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_5");'>5</a></li> <li><a href="#" onclick='return showDiv("page_6");'>6</a></li> <li class="active"><span>7</span></li> <li><a href="#" onclick='return showDiv("page_8");'>8</a></li> <li><a href="#" onclick='return showDiv("page_9");'>9</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div> </div> <div class="row"> <div class="col-sm-12"> <ol class="result-class" start="121"> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19960027467&hterms=role+distribution&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3Drole%2Bdistribution','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19960027467&hterms=role+distribution&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3Drole%2Bdistribution"><span id="translatedtitle">Role of <span class="hlt">intrinsic</span> width in fragment momentum distributions in heavy ion collisions</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Townsend, L. W.; Tripathi, R. K.; Khan, F.</p> <p>1994-01-01</p> <p>It is demonstrated that the <span class="hlt">intrinsic</span> widths incorporating <span class="hlt">correlations</span> in conjunction with dynamical contributions give better agreement with experiments for collisions in the energy range of 200 A MeV to 2.4 GeV than using only <span class="hlt">intrinsic</span> widths without <span class="hlt">correlations</span>. The sensitivity of the <span class="hlt">intrinsic</span> width decreases with increasing projectile mass. A simple recipe for calculating <span class="hlt">intrinsic</span> width <span class="hlt">correlations</span> is presented.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19860004486','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19860004486"><span id="translatedtitle">Multigrid solutions to quasi-<span class="hlt">elliptic</span> schemes</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Brandt, A.; Taasan, S.</p> <p>1985-01-01</p> <p>Quasi-<span class="hlt">elliptic</span> schemes arise from central differencing or finite element discretization of <span class="hlt">elliptic</span> systems with odd order derivatives on non-staggered grids. They are somewhat unstable and less accurate then corresponding staggered-grid schemes. When usual multigrid solvers are applied to them, the asymptotic algebraic convergence is necessarily slow. Nevertheless, it is shown by mode analyses and numerical experiments that the usual FMG algorithm is very efficient in solving quasi-<span class="hlt">elliptic</span> equations to the level of truncation errors. Also, a new type of multigrid algorithm is presented, mode analyzed and tested, for which even the asymptotic algebraic convergence is fast. The essence of that algorithm is applicable to other kinds of problems, including highly indefinite ones.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2014JMOp...61.1069J','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2014JMOp...61.1069J"><span id="translatedtitle">Highly confined photonic nanojet from <span class="hlt">elliptical</span> particles</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Jalali, T.; Erni, D.</p> <p>2014-07-01</p> <p><span class="hlt">Elliptically</span> shaped particles with different size and refractive indices have been studied under plane wave illumination using simulation tools such as 2D-FDTD, 2D-MMP, and 3D-MMP. Owing to careful manipulation, the power distribution in the vicinity of the particles opposite boundary resulted in a tightly focused photonic nanojet. Their waists are significantly smaller than the diffraction limit while propagating over several optical wavelengths without significant divergence. In this paper, we report on the manipulation of the particles <span class="hlt">elliptical</span> shapes and the underlying refractive indices with respect to a maximally confined power distribution in the resulting nanojet which has been parameterized according to both, the beam waist and the beam divergence. The result that <span class="hlt">elliptical</span> particles (i.e. oblate spheroids) turned out to be superior to spherical ones was underpinned within a highly accurate and fast 3D-MMP simulation using ring multipoles.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/1990RScI...61.3738P','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/1990RScI...61.3738P"><span id="translatedtitle">Line focus of an <span class="hlt">elliptic</span> cone for an x-ray crystal spectrograph</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Phillion, D. W.; Hammel, B. A.</p> <p>1990-12-01</p> <p>The crystal in any flat crystal x-ray spectrograph with the film plane at any angle and any position may be bent sagittally into an <span class="hlt">elliptic</span> conical shape such that a perfect line focus is formed on the film plane for a point source at a fixed location. However, for high spectral resolution, only a narrow strip along the cone can be utilized. This strip will be near the plane formed by the axis of the cone and the source point. The <span class="hlt">elliptic</span> cone has mirror symmetry in this plane. The equation of this cone is determined and its properties are discussed. Any conical surface has zero <span class="hlt">intrinsic</span> curvature since one of the two principal radii of curvature is zero, so it is no more difficult to bend a crystal to this shape than to a concave circular cylinder with the same principal radius of curvature.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19860015840','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19860015840"><span id="translatedtitle">Metallicity and the level of the ultraviolet rising branch in <span class="hlt">elliptical</span> galaxies</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Faber, S. M.</p> <p>1986-01-01</p> <p>This final report concerns a project to study the systematics of the ultraviolet flux level in <span class="hlt">elliptical</span> galaxies. Prior to the inception of this work, the systematic behavior of the ultraviolet flux level was basically unknown and ultraviolet fluxes were observed to vary greatly from galaxy to galaxy. There was a suggestion, however, that there might be a dependence of ultraviolet flux on galaxy metallicity, but the <span class="hlt">correlation</span> was based on just six galaxies. IUE spectra of <span class="hlt">elliptical</span> galaxies have been reanalyzed and placed on a consistent, homogenous flux system. The major conclusion is a confirmation of the original hypothesis: galaxies with stronger Mg2 lines show enhanced ultraviolet flux.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://files.eric.ed.gov/fulltext/ED485061.pdf','ERIC'); return false;" href="http://files.eric.ed.gov/fulltext/ED485061.pdf"><span id="translatedtitle">Predicting <span class="hlt">Intrinsic</span> Motivation</span></a></p> <p><a target="_blank" href="http://www.eric.ed.gov/ERICWebPortal/search/extended.jsp?_pageLabel=advanced">ERIC Educational Resources Information Center</a></p> <p>Martens, Rob; Kirschner, Paul A.</p> <p>2004-01-01</p> <p><span class="hlt">Intrinsic</span> motivation can be predicted from participants' perceptions of the social environment and the task environment (Ryan & Deci, 2000)in terms of control, relatedness and competence. To determine the degree of independence of these factors 251 students in higher vocational education (physiotherapy and hotel management) indicated the extent to…</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/19103543','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/19103543"><span id="translatedtitle">[<span class="hlt">Intrinsic</span> cardiac ganglia].</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Birand, Ahmet</p> <p>2008-12-01</p> <p>Heart has been considered as the source and the seat of emotions, passion and love. But from the dawn of XIXth century, scientists have emphasized that the heart, though life depends on its ceaseless activity, is merely a electromechanical pump, pumping oxygenated blood. Nowadays, we all know that heart pumps blood commensurate with the needs of the body and this unending toil, and its regulation depends on the <span class="hlt">intrinsic</span> properties of the myocardium, Frank-Starling Law and neurohumoral contribution. It has been understood, though not clearly enough, that these time-tensions may cause structural or functional cardiac impairments and arrhythmias are related to the autonomic nervous system. Less well known and less taken in account in daily cardiology practice is the fact that heart has an <span class="hlt">intrinsic</span> cardiac nervous system, or "heart brain" consisting of complex ganglia, <span class="hlt">intrinsic</span> cardiac ganglia containing afferent (receiving), local circuit (interneurons) and efferent (transmitting) sympathetic and parasympathetic neurons. This review enlightens structural and functional aspects of <span class="hlt">intrinsic</span> cardiac ganglia as the very first step in the regulation of cardiac function. This issue is important for targets of pharmacological treatment and techniques of cardiac surgery interventions as repair of septal defects, valvular interventions and congenital corrections.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://eric.ed.gov/?q=tripathi&pg=2&id=EJ480276','ERIC'); return false;" href="http://eric.ed.gov/?q=tripathi&pg=2&id=EJ480276"><span id="translatedtitle">Competition and <span class="hlt">Intrinsic</span> Motivation.</span></a></p> <p><a target="_blank" href="http://www.eric.ed.gov/ERICWebPortal/search/extended.jsp?_pageLabel=advanced">ERIC Educational Resources Information Center</a></p> <p>Tripathi, Kailas Nath</p> <p>1992-01-01</p> <p>Reports on a study of competition, motivation, and performance among 60 adolescents in India. Finds that direct competition with another person led to higher levels of immediate performance. Also finds that indirect competition against a pre-set standard resulted in greater <span class="hlt">intrinsic</span> motivation. (CFR)</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://eric.ed.gov/?q=silberman&pg=6&id=EJ302148','ERIC'); return false;" href="http://eric.ed.gov/?q=silberman&pg=6&id=EJ302148"><span id="translatedtitle">Evaluating <span class="hlt">Intrinsic</span> Goals.</span></a></p> <p><a target="_blank" href="http://www.eric.ed.gov/ERICWebPortal/search/extended.jsp?_pageLabel=advanced">ERIC Educational Resources Information Center</a></p> <p>Silberman, Harry F.</p> <p>1984-01-01</p> <p>A social learning model focusing on <span class="hlt">intrinsic</span> outcomes of vocational programs is proposed. It would assess technical skills and knowledge, communication skills and literacy, and personal skills and attitudes. Instruments should be devised to measure characteristics of the learning setting, learner involved activities, and nature of consequences of…</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016JSMTE..08.3106R','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016JSMTE..08.3106R"><span id="translatedtitle"><span class="hlt">Elliptic</span> pfaffians and solvable lattice models</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Rosengren, Hjalmar</p> <p>2016-08-01</p> <p>We introduce and study twelve multivariable theta functions defined by pfaffians with <span class="hlt">elliptic</span> function entries. We show that, when the crossing parameter is a cubic root of unity, the domain wall partition function for the eight-vertex-solid-on-solid model can be written as a sum of two of these pfaffians. As a limit case, we express the domain wall partition function for the three-colour model as a sum of two Hankel determinants. We also show that certain solutions of the TQ-equation for the supersymmetric eight-vertex model can be expressed in terms of <span class="hlt">elliptic</span> pfaffians.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2015APS..DFD.M3004A','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2015APS..DFD.M3004A"><span id="translatedtitle"><span class="hlt">Elliptical</span> Particle Clustering in Cellular Flows</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Atis, Severine; Sapsis, Themistoklis; Peacock, Thomas</p> <p>2015-11-01</p> <p>The transport of finite-sized objects by fluid flows is relevant to a wide variety of phenomena, such as debris transport on the ocean surface or bacteria advection in fluid environment. The shape of the advected objects can strongly alter their coupling with the surrounding flow field, and hence, greatly affecting their dispersion by the flow. We present the results of investigations of the behavior of neutrally buoyant, <span class="hlt">elliptical</span> particles in two-dimensional cellular flows. We find that their trajectories, and overall organization, are markedly different than for spherical particles, with clear clustering for the <span class="hlt">elliptical</span> particles associated with vortices.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19930081267','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19930081267"><span id="translatedtitle">Strength Tests of Thin-walled Duralumin Cylinders of <span class="hlt">Elliptic</span> Section</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Lundquist, Eugene E; Burke, Walter F</p> <p>1935-01-01</p> <p>This report is the fifth of a series presenting the results of strength tests of thin-walled cylinders and truncated cones of circular and <span class="hlt">elliptic</span> section; it includes the results obtained from torsion tests on 30 cylinders, pure bending tests on 30 cylinders, and combined transverse shear and bending tests on 60 cylinders. All the cylinders tested were <span class="hlt">elliptic</span> section with the ends clamped to rigid bulkheads. In the pure bending and combined transverse shear and bending tests the loads were applied in the plane of the major axis. The results of the tests on <span class="hlt">elliptic</span> cylinders are <span class="hlt">correlated</span> with the results of corresponding tests on circular cylinders and are presented in charts suitable for use in design.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19980030781','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19980030781"><span id="translatedtitle">Design of Three-Dimensional Hypersonic Inlets with Rectangular to <span class="hlt">Elliptical</span> Shape Transition</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Smart, M. K.</p> <p>1998-01-01</p> <p>A methodology has been devised for the design of three-dimensional hypersonic inlets which include a rectangular to <span class="hlt">elliptical</span> shape transition. This methodology makes extensive use of inviscid streamtracing techniques to generate a smooth shape transition from a rectangular-like capture to an <span class="hlt">elliptical</span> throat. Highly swept leading edges and a significantly notched cowl enable use of these inlets in fixed geometry configurations. The design procedure includes a three dimensional displacement thickness calculation and uses established <span class="hlt">correlations</span> to check for boundary layer separation due to shock wave interactions. Complete details of the design procedure are presented and the characteristics of a modular inlet with rectangular to <span class="hlt">elliptical</span> shape transition and a design point of Mach 7.1 are examined. Comparison with a classical two-dimensional inlet optimized for maximum total pressure recovery indicates that this three-dimensional inlet demonstrates good performance even well below its design point.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://www.osti.gov/scitech/servlets/purl/10134497','SCIGOV-STC'); return false;" href="http://www.osti.gov/scitech/servlets/purl/10134497"><span id="translatedtitle">Buckling of <span class="hlt">elliptical</span> rings under uniform external pressure</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Tang, Y.</p> <p>1991-04-03</p> <p>A thin, elastic <span class="hlt">elliptical</span> ring is subjected to uniform external pressure. The lowest critical pressure is computed and presented for various ratio of the major axis to the minor axis of the <span class="hlt">elliptical</span> ring. It is found that the critical pressure for an <span class="hlt">elliptical</span> ring is higher than that for the circular ring whose diameter is equal to the major axis of the <span class="hlt">elliptical</span> ring. It can be shown that under the same external pressure, the axial force developed in the <span class="hlt">elliptical</span> ring is less than that developed in the corresponding circular ring. Thus, a higher pressure is required to buckle the <span class="hlt">elliptical</span> rings. Therefore, by changing the shape of the ring from circular to <span class="hlt">elliptical</span>, the capability of the ring to sustain the external pressure can be increased substantially. The results of this study can be useful in the design of <span class="hlt">elliptical</span> reinforcing rings and thin-walled tubes subjected to external pressure.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/22127048','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/22127048"><span id="translatedtitle">DIRECT DETECTIONS OF YOUNG STARS IN NEARBY <span class="hlt">ELLIPTICAL</span> GALAXIES</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Ford, H. Alyson; Bregman, Joel N.</p> <p>2013-06-20</p> <p>Small amounts of star formation in <span class="hlt">elliptical</span> galaxies are suggested by several results: surprisingly young ages from optical line indices, cooling X-ray gas, and mid-infrared dust emission. Such star formation has previously been difficult to directly detect, but using ultraviolet Hubble Space Telescope Wide Field Camera 3 imaging, we have identified individual young stars and star clusters in four nearby <span class="hlt">ellipticals</span>. Ongoing star formation is detected in all galaxies, including three <span class="hlt">ellipticals</span> that have previously exhibited potential signposts of star-forming conditions (NGC 4636, NGC 4697, and NGC 4374), as well as the typical ''red and dead'' NGC 3379. The current star formation in our closest targets, where we are most complete, is between 2.0 and 9.8 Multiplication-Sign 10{sup -5} M{sub Sun} yr{sup -1}. The star formation history was roughly constant from 0.5 to 1.5 Gyr (at (3-5) Multiplication-Sign 10{sup -4} M{sub Sun} yr{sup -1}), but decreased by a factor of several in the past 0.3 Gyr. Most star clusters have a mass between 10{sup 2} and 10{sup 4} M{sub Sun }. The specific star formation rates of {approx}10{sup -16} yr{sup -1} (at the present day) or {approx}10{sup -14} yr{sup -1} (when averaging over the past Gyr) imply that a fraction 10{sup -8} of the stellar mass is younger than 100 Myr and 10{sup -5} is younger than 1 Gyr, quantifying the level of frosting of recent star formation over the otherwise passive stellar population. There is no obvious <span class="hlt">correlation</span> between either the presence or spatial distribution of postulated star formation indicators and the star formation we detect.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://www.osti.gov/scitech/servlets/purl/205931','SCIGOV-STC'); return false;" href="http://www.osti.gov/scitech/servlets/purl/205931"><span id="translatedtitle">Differential spectral synthesis with a library of <span class="hlt">elliptical</span> galaxies</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Gregg, M.</p> <p>1995-12-07</p> <p>Spectrophotometry of <span class="hlt">elliptical</span> galaxies spanning a large rang in luminosity is analyzed for cosmic variations in color and line strength. The results are used to construct a base sequence spectral energy distribution as a function line strength, color, and velocity dispersion, representing old, red, uniform <span class="hlt">elliptical</span> galaxy stellar populations. The sequence can be used as the starting point for investigating and modeling the stellar populations of other systems such as dwarf <span class="hlt">ellipticals</span>, merger remnants, and, eventually, high redshift <span class="hlt">ellipticals</span>.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://www.dtic.mil/docs/citations/ADA625578','DTIC-ST'); return false;" href="http://www.dtic.mil/docs/citations/ADA625578"><span id="translatedtitle">On Fibonacci Numbers Which Are <span class="hlt">Elliptic</span> Carmichael</span></a></p> <p><a target="_blank" href="https://publicaccess.dtic.mil/psm/api/service/search/search">DTIC Science & Technology</a></p> <p></p> <p>2014-12-27</p> <p>On Fibonacci numbers which are <span class="hlt">elliptic</span> Carmichael Florian Luca School of Mathematics University of the Witwatersrand P. O. Box Wits 2050, South...was written during a visit of P. S. to the School of Mathematics of the University of the Witwatersrand in 2014. This author thanks the institution for</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016JHEP...05..076G','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016JHEP...05..076G"><span id="translatedtitle"><span class="hlt">Elliptic</span> genera from multi-centers</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Gaddam, Nava</p> <p>2016-05-01</p> <p>I show how <span class="hlt">elliptic</span> genera for various Calabi-Yau threefolds may be understood from supergravity localization using the quantization of the phase space of certain multi-center configurations. I present a simple procedure that allows for the enumeration of all multi-center configurations contributing to the polar sector of the <span class="hlt">elliptic</span> genera — explicitly verifying this in the cases of the quintic in {P} 4, the sextic in {W}{P} (2,1,1,1,1), the octic in {W}{P} (4,1,1,1,1) and the dectic in {W}{P} (5,2,1,1,1). With an input of the corresponding `single-center' indices (Donaldson-Thomas invariants), the polar terms have been known to determine the <span class="hlt">elliptic</span> genera completely. I argue that this multi-center approach to the low-lying spectrum of the <span class="hlt">elliptic</span> genera is a stepping stone towards an understanding of the exact microscopic states that contribute to supersymmetric single center black hole entropy in {N} = 2 supergravity.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19740036752&hterms=Nomenclature&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D20%26Ntt%3DNomenclature','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19740036752&hterms=Nomenclature&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D20%26Ntt%3DNomenclature"><span id="translatedtitle">Nomenclature of polarized light - <span class="hlt">Elliptical</span> polarization</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Clarke, D.</p> <p>1974-01-01</p> <p>Alternative handedness and sign conventions for relating the orientation of <span class="hlt">elliptical</span> polarization are discussed. The discussion proceeds under two headings: (1) snapshot picture, where the emphasis for the convention is contained in the concept of handedness; and (2) angular momentum consideration, where the emphasis for the convention is strongly associated with mathematical convention and the sign of the fourth Stokes parameter.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/1996SbMat.187.1691S','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/1996SbMat.187.1691S"><span id="translatedtitle">Relative <span class="hlt">elliptic</span> theory and the Sobolev problem</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Sternin, B. Yu; Shatalov, V. E.</p> <p>1996-12-01</p> <p>An operator algebra associated with a smooth embedding i \\colon X\\hookrightarrow M is constructed. For <span class="hlt">elliptic</span> elements of this algebra a finiteness theorem (the Fredholm property) is established, and the index is computed. A connection with Sobolev problems is shown.</p> </li> </ol> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_5");'>5</a></li> <li><a href="#" onclick='return showDiv("page_6");'>6</a></li> <li class="active"><span>7</span></li> <li><a href="#" onclick='return showDiv("page_8");'>8</a></li> <li><a href="#" onclick='return showDiv("page_9");'>9</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div><!-- col-sm-12 --> </div><!-- row --> </div><!-- page_7 --> <div id="page_8" class="hiddenDiv"> <div class="row"> <div class="col-sm-12"> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_6");'>6</a></li> <li><a href="#" onclick='return showDiv("page_7");'>7</a></li> <li class="active"><span>8</span></li> <li><a href="#" onclick='return showDiv("page_9");'>9</a></li> <li><a href="#" onclick='return showDiv("page_10");'>10</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div> </div> <div class="row"> <div class="col-sm-12"> <ol class="result-class" start="141"> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/1999APS..DFD..GC01C','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/1999APS..DFD..GC01C"><span id="translatedtitle">Circular and <span class="hlt">Elliptic</span> Submerged Impinging Water Jets</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Claudey, Eric; Benedicto, Olivier; Ravier, Emmanuel; Gutmark, Ephraim</p> <p>1999-11-01</p> <p>Experiments and CFD have been performed to study circular and <span class="hlt">elliptic</span> jets in a submerged water jet facility. The tests included discharge coefficient measurement to evaluate pressure losses encountered in noncircular nozzles compared to circular ones. Three-dimensional pressure mappings on the impingement surface and PIV measurement of the jet mean and turbulent velocity have been performed at different compound impingement angles relative to the impingement surface and at different stand-off distances. The objective was to investigate the effect of the non-circular geometry on the flow field and on the impact region. The tests were performed in a close loop system in which the water was pumped through the nozzles into a clear Plexiglas tank. The Reynolds numbers were typically in the range of 250000. Discharge coefficients of the <span class="hlt">elliptic</span> nozzle was somewhat lower than that of the circular jet but spreading rate and turbulence level were higher. Pressure mapping showed that the nozzle exit geometry had an effect on the pressure distribution in the impact region and that high-pressure zones were generated at specific impact points. PIV measurements showed that for a same total exit area, the <span class="hlt">elliptic</span> jets affected a surface area that is 8the equivalent circular. The turbulence level in the <span class="hlt">elliptic</span> jet tripled due to the nozzle design. Results of the CFD model were in good agreement with the experimental data.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19920000772&hterms=Mercator+projection&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3DMercator%2Bprojection','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19920000772&hterms=Mercator+projection&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3DMercator%2Bprojection"><span id="translatedtitle">Transverse Mercator Projection Via <span class="hlt">Elliptic</span> Integrals</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Wallis, David E.</p> <p>1992-01-01</p> <p>Improved method of construction of U.S. Army's universal transverse Mercator grid system based on Gauss-Kruger transverse Mercator projection and on use of <span class="hlt">elliptic</span> integrals of second kind. Method can be used to map entire northern or southern hemisphere with respect to single principal meridian.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://www.osti.gov/scitech/servlets/purl/921929','SCIGOV-STC'); return false;" href="http://www.osti.gov/scitech/servlets/purl/921929"><span id="translatedtitle"><span class="hlt">ELLIPTIC</span> FLOW, INITIAL ECCENTRICITY AND <span class="hlt">ELLIPTIC</span> FLOW FLUCTUATIONS IN HEAVY ION COLLISIONS AT RHIC.</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>NOUICER,R.; ALVER, B.; BACK, B.B.; BAKER, M.D.; BALLINTIJN, M.; BARTON, D.S.; ET AL.</p> <p>2007-02-19</p> <p>We present measurements of <span class="hlt">elliptic</span> flow and event-by-event fluctuations established by the PHOBOS experiment. <span class="hlt">Elliptic</span> flow scaled by participant eccentricity is found to be similar for both systems when collisions with the same number of participants or the same particle area density are compared. The agreement of <span class="hlt">elliptic</span> flow between Au+Au and Cu+Cu collisions provides evidence that the matter is created in the initial stage of relativistic heavy ion collisions with transverse granularity similar to that of the participant nucleons. The event-by-event fluctuation results reveal that the initial collision geometry is translated into the final state azimuthal particle distribution, leading to an event-by-event proportionality between the observed <span class="hlt">elliptic</span> flow and initial eccentricity.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2012A%26A...539A..78C','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2012A%26A...539A..78C"><span id="translatedtitle"><span class="hlt">Elliptical</span> instability in terrestrial planets and moons</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Cebron, D.; Le Bars, M.; Moutou, C.; Le Gal, P.</p> <p>2012-03-01</p> <p>Context. The presence of celestial companions means that any planet may be subject to three kinds of harmonic mechanical forcing: tides, precession/nutation, and libration. These forcings can generate flows in internal fluid layers, such as fluid cores and subsurface oceans, whose dynamics then significantly differ from solid body rotation. In particular, tides in non-synchronized bodies and libration in synchronized ones are known to be capable of exciting the so-called <span class="hlt">elliptical</span> instability, i.e. a generic instability corresponding to the destabilization of two-dimensional flows with <span class="hlt">elliptical</span> streamlines, leading to three-dimensional turbulence. Aims: We aim here at confirming the relevance of such an <span class="hlt">elliptical</span> instability in terrestrial bodies by determining its growth rate, as well as its consequences on energy dissipation, on magnetic field induction, and on heat flux fluctuations on planetary scales. Methods: Previous studies and theoretical results for the <span class="hlt">elliptical</span> instability are re-evaluated and extended to cope with an astrophysical context. In particular, generic analytical expressions of the <span class="hlt">elliptical</span> instability growth rate are obtained using a local WKB approach, simultaneously considering for the first time (i) a local temperature gradient due to an imposed temperature contrast across the considered layer or to the presence of a volumic heat source and (ii) an imposed magnetic field along the rotation axis, coming from an external source. Results: The theoretical results are applied to the telluric planets and moons of the solar system as well as to three Super-Earths: 55 CnC e, CoRoT-7b, and GJ 1214b. For the tide-driven <span class="hlt">elliptical</span> instability in non-synchronized bodies, only the early Earth core is shown to be clearly unstable. For the libration-driven <span class="hlt">elliptical</span> instability in synchronized bodies, the core of Io is shown to be stable, contrary to previously thoughts, whereas Europa, 55 CnC e, CoRoT-7b, and GJ 1214b cores can be unstable</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016AIPC.1727b0006D','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016AIPC.1727b0006D"><span id="translatedtitle">Performances study of UWB monopole antennas using half-<span class="hlt">elliptic</span> radiator conformed on <span class="hlt">elliptical</span> surface</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Djidel, S.; Bouamar, M.; Khedrouche, D.</p> <p>2016-04-01</p> <p>This paper presents a performances study of UWB monopole antenna using half-<span class="hlt">elliptic</span> radiator conformed on <span class="hlt">elliptical</span> surface. The proposed antenna, simulated using microwave studio computer CST and High frequency simulator structure HFSS, is designed to operate in frequency interval over 3.1 to 40 GHz. Good return loss and radiation pattern characteristics are obtained in the frequency band of interest. The proposed antenna structure is suitable for ultra-wideband applications, which is, required for many wearable electronics applications.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2012JAMDS...6..484L','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2012JAMDS...6..484L"><span id="translatedtitle">Analysis of the Dynamic Characteristics of <span class="hlt">Elliptical</span> Gears</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Liu, Xing; Nagamura, Kazuteru; Ikejo, Kiyotaka</p> <p></p> <p>To date, <span class="hlt">elliptical</span> gear has been commonly used in automobile, automatic machinery, pumps, flow meters and printing presses for its particular non-uniform rotation. However, the dynamic characteristics of <span class="hlt">elliptical</span> gears have not been clarified yet. In this study, The calculation as well as the experiment of two <span class="hlt">elliptical</span> gears, which are a single <span class="hlt">elliptical</span> gear and a double <span class="hlt">elliptical</span> gear, is carried out to analyze the dynamic characteristics of <span class="hlt">elliptical</span> gears. General factors including the torque, the rotation speed and the tooth root stress of the test gears are investigated. According to the analysis conducted in this study, the dynamic input torque variation of <span class="hlt">elliptical</span> gear becomes larger along with the increase of operating gear rotation speed and the experimental one increases much faster than the calculated one over the Critical Rotation Speed of Tooth Separation (CRSTS) of <span class="hlt">elliptical</span> gear. The experimental input rotation speed varies according to the variation of input torque, leading to the difference between the experimental output rotation speed and the desired one. The calculation results of the CRSTS of <span class="hlt">elliptical</span> gears are almost equal to the experimental ones. The dynamic load variation ratios of <span class="hlt">elliptical</span> gear at different angular position as well as their changing trends with operating gear rotation speed are quite different from each other. And the experimental dynamic load variation ratios of <span class="hlt">elliptical</span> gear show difference from the calculated ones because of tooth separation and tooth impact. The agreement of the calculation and experimental results proves the validity of this study.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2015CeMDA.121...61R','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2015CeMDA.121...61R"><span id="translatedtitle">Frozen-anomaly transformation for the <span class="hlt">elliptic</span> rendezvous problem</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Roa, Javier; Peláez, Jesús</p> <p>2015-01-01</p> <p>A new solution to relative motion on <span class="hlt">elliptical</span> orbits is presented, based on a novel transformation from the reference state vector to the relative state vector. The relative orbit is constructed assuming that the anomaly, and not the time, is the invariant element throughout the transformation. This concept arises naturally from the variational form of anomaly-explicit formulations. In particular, this paper explores the capabilities of a formulation developed by Peláez et al. (Celest Mech Dyn Astron. 97, 131-150, 2007), called Dromo. This formulation exploits the advantages of the ideal reference frames and quaternionic descriptions of the orbital plane. The linear variational form of the equations of motion in Dromo is developed herein, and the resulting transformation matrix is presented. When applied to the reference state vector, this linear transformation provides the relative state vector at any step. The invariance in the anomaly implies a certain time delay in the results. Physical times for leader and follower do not coincide after the transformation. To recover the sense of the solution an additional correction is applied a posteriori to cancel this <span class="hlt">intrinsic</span> time delay. The performance of the new transformation is compared against previous solutions to the problem through a set of numerical examples. Important error reductions in determining the relative orbit are observed in these tests.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2011ApJ...730....9O','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2011ApJ...730....9O"><span id="translatedtitle"><span class="hlt">Elliptically</span> Weighted HOLICs for Weak-lensing Shear Measurement. I. Definitions and Isotropic Point-spread Function Correction</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Okura, Yuki; Futamase, Toshifumi</p> <p>2011-03-01</p> <p>We develop a new method of estimating gravitational shear by adopting an <span class="hlt">elliptical</span> weight function to measure background galaxy images. In doing so, we introduce the new concept of "zero plane," which is an imaginary source plane where shapes of all sources are perfect circles, and regard the <span class="hlt">intrinsic</span> shear as the result of an imaginary lensing distortion. This makes the relation between the observed shear, <span class="hlt">intrinsic</span> shear, and lensing distortion much simpler, and thus higher-order calculations are easier. The <span class="hlt">elliptical</span> weight function allows us to measure the multipole moments of the shapes of background galaxies more precisely by weighting brighter parts of the image highly, and to reduce systematic error due to insufficient expansion of the weight function in the original approach of Kaiser et al. (KSB). Point-spread function (PSF) correction in the <span class="hlt">elliptically</span> weighted higher-order lensing image characteristics (E-HOLICs) method becomes more complicated than in the KSB method. In this paper, we study isotropic PSF correction in detail. By adopting the lensing distortion as the <span class="hlt">ellipticity</span> of the weight function, we are able to show that the shear estimation in the E-HOLICs method reduces to solve a polynomial in the absolute magnitude of the distortion. We compare the systematic errors between our approach and that of KSB using the Shear Testing Programme 2 simulation. It is confirmed that the KSB method overestimates the input shear for images with large <span class="hlt">ellipticities</span>, and E-HOLICs correctly estimates the input shear even for such images. Anisotropic PSF correction and analysis of real data will be presented in a forthcoming paper.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2009ExFl...46..165H','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2009ExFl...46..165H"><span id="translatedtitle">In-cylinder tumble flows and performance of a motorcycle engine with circular and <span class="hlt">elliptic</span> intake ports</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Huang, R. F.; Lin, K. H.; Yeh, C.-N.; Lan, J.</p> <p>2009-01-01</p> <p>The temporal and spatial evolution processes of the flows in the cylinder of a four-valve, four-stroke, single cylinder, reciprocating motorcycle engine installed with the <span class="hlt">elliptic</span> and circular intake ports were experimentally studied by using the particle image velocimetry (PIV). The engine was modified to fit the requirements of PIV measurement. The velocity fields measured by the PIV were analyzed and quantitatively presented as the tumble ratio and turbulence intensity. In the symmetry plane, both the circular and <span class="hlt">elliptic</span> intake ports could initiate a vortex around the central region during the intake stroke. During the compression stroke, the central vortex created in the cylinder of the engine with the circular intake port disappeared, while that in the engine cylinder with the <span class="hlt">elliptic</span> intake port further developed into the tumble motion. In the offset plane, weak vortical structures were initiated by the bluff-body effect of the intake valves during the intake stroke. The vortical structures induced by the <span class="hlt">elliptic</span> intake port were more coherent than those generated by the circular intake port; besides, this feature extends to the compression stroke. The cycle-averaged tumble ratio and the turbulence intensity of the engine with the <span class="hlt">elliptic</span> intake port were dramatically larger than those of the engine with the circular intake port. The measured engine performance was improved a lot by installing the <span class="hlt">elliptic</span> intake port. The <span class="hlt">correlation</span> between the flow features and the enhancement of the engine performance were argued and discussed.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2015NatSR...510386C','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2015NatSR...510386C"><span id="translatedtitle"><span class="hlt">Intrinsically</span> Disordered Energy Landscapes</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Chebaro, Yassmine; Ballard, Andrew J.; Chakraborty, Debayan; Wales, David J.</p> <p>2015-05-01</p> <p>Analysis of an <span class="hlt">intrinsically</span> disordered protein (IDP) reveals an underlying multifunnel structure for the energy landscape. We suggest that such ‘<span class="hlt">intrinsically</span> disordered’ landscapes, with a number of very different competing low-energy structures, are likely to characterise IDPs, and provide a useful way to address their properties. In particular, IDPs are present in many cellular protein interaction networks, and several questions arise regarding how they bind to partners. Are conformations resembling the bound structure selected for binding, or does further folding occur on binding the partner in a induced-fit fashion? We focus on the p53 upregulated modulator of apoptosis (PUMA) protein, which adopts an -helical conformation when bound to its partner, and is involved in the activation of apoptosis. Recent experimental evidence shows that folding is not necessary for binding, and supports an induced-fit mechanism. Using a variety of computational approaches we deduce the molecular mechanism behind the instability of the PUMA peptide as a helix in isolation. We find significant barriers between partially folded states and the helix. Our results show that the favoured conformations are molten-globule like, stabilised by charged and hydrophobic contacts, with structures resembling the bound state relatively unpopulated in equilibrium.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4441119','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4441119"><span id="translatedtitle"><span class="hlt">Intrinsically</span> Disordered Energy Landscapes</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Chebaro, Yassmine; Ballard, Andrew J.; Chakraborty, Debayan; Wales, David J.</p> <p>2015-01-01</p> <p>Analysis of an <span class="hlt">intrinsically</span> disordered protein (IDP) reveals an underlying multifunnel structure for the energy landscape. We suggest that such ‘<span class="hlt">intrinsically</span> disordered’ landscapes, with a number of very different competing low-energy structures, are likely to characterise IDPs, and provide a useful way to address their properties. In particular, IDPs are present in many cellular protein interaction networks, and several questions arise regarding how they bind to partners. Are conformations resembling the bound structure selected for binding, or does further folding occur on binding the partner in a induced-fit fashion? We focus on the p53 upregulated modulator of apoptosis (PUMA) protein, which adopts an -helical conformation when bound to its partner, and is involved in the activation of apoptosis. Recent experimental evidence shows that folding is not necessary for binding, and supports an induced-fit mechanism. Using a variety of computational approaches we deduce the molecular mechanism behind the instability of the PUMA peptide as a helix in isolation. We find significant barriers between partially folded states and the helix. Our results show that the favoured conformations are molten-globule like, stabilised by charged and hydrophobic contacts, with structures resembling the bound state relatively unpopulated in equilibrium. PMID:25999294</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017ZaMP...68...10S','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017ZaMP...68...10S"><span id="translatedtitle">Convergence results for <span class="hlt">elliptic</span> quasivariational inequalities</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Sofonea, Mircea; Benraouda, Ahlem</p> <p>2017-02-01</p> <p>In this paper, we state and prove various convergence results for a general class of <span class="hlt">elliptic</span> quasivariational inequalities with constraints. Thus, we prove the convergence of the solution of a class of penalized problems to the solution of the original inequality, as the penalty parameter converges to zero. We also prove a continuous dependence result of the solution with respect the convex set of constraints. Then, we consider a mathematical model which describes the equilibrium of an elastic rod attached to a nonlinear spring. We derive the variational formulation of the model which is in a form of an <span class="hlt">elliptic</span> quasivariational inequality for the displacement field. We prove the unique weak solvability of the model, and then we state and prove two convergence results and provide their corresponding mechanical interpretation.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=LV-2007-00040&hterms=Dvd&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D80%26Ntt%3DDvd','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=LV-2007-00040&hterms=Dvd&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D80%26Ntt%3DDvd"><span id="translatedtitle">Performance Characteristics of a Preformed <span class="hlt">Elliptical</span> Parachute</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p></p> <p>1963-01-01</p> <p>Performance Characteristics of a Preformed <span class="hlt">Elliptical</span> Parachute at Altitudes between 200,000 and 100,000 Thousand Feet Obtained by In-Flight Photography. The performance characteristics of a pre-formed <span class="hlt">elliptical</span> parachute at altitudes between 200,000 and 100,000 feet were obtained by means of in-flight photography. The tests demonstrate that this type of parachute will open at altitudes of about 200,000 feet if conditions such as twisting of the suspension lines or draping of the suspension lines over the canopy do not occur. Drag-coefficient values between 0.6 and 0.8 were found to be reasonable for this type of parachute system in the altitude range between 200,000 and 100,000 feet. [Entire movie available on DVD from CASI as Doc ID 20070030980. Contact help@sti.nasa.gov</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://www.osti.gov/scitech/servlets/purl/10186744','SCIGOV-STC'); return false;" href="http://www.osti.gov/scitech/servlets/purl/10186744"><span id="translatedtitle">Performance of the ALS <span class="hlt">elliptical</span> wiggler</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Wang, C.X.; Schlueter, R.; Hoyer, E.; Heimann, P.</p> <p>1993-08-01</p> <p>The <span class="hlt">elliptical</span> wiggler is a circularly polarized light source capable of providing very broad spectral coverage and high degree of circular polarization. The main features of an <span class="hlt">elliptical</span> wiggler can be understood through analogy to bending magnet radiation. However, some aspects, such as the end structure`s influence on the degree of circular polarization, require more elaborate methods to characterize. We present an algorithm based on the stationary phase method, which allows calculation of radiation properties from an arbitrary electron trajectory; so a non-sinusoidal magnetic field`s influence on the radiation performance can be taken into account. We show general radiation properties of an ellilptical wiggler and discuss factors affecting radiation performance. Practice issues encountered during the conceptual design of an ellilptical wiggler at the Advanced Light Source are addressed.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2006PhyB..385.1247M','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2006PhyB..385.1247M"><span id="translatedtitle">Performance of an <span class="hlt">elliptically</span> tapered neutron guide</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Mühlbauer, Sebastian; Stadlbauer, Martin; Böni, Peter; Schanzer, Christan; Stahn, Jochen; Filges, Uwe</p> <p>2006-11-01</p> <p>Supermirror coated neutron guides are used at all modern neutron sources for transporting neutrons over large distances. In order to reduce the transmission losses due to multiple internal reflection of neutrons, ballistic neutron guides with linear tapering have been proposed and realized. However, these systems suffer from an inhomogeneous illumination of the sample. Moreover, the flux decreases significantly with increasing distance from the exit of the neutron guide. We propose using <span class="hlt">elliptically</span> tapered guides that provide a more homogeneous phase space at the sample position as well as a focusing at the sample. Moreover, the design of the guide system is simplified because ellipses are simply defined by their long and short axes. In order to prove the concept we have manufactured a doubly focusing guide and investigated its properties with neutrons. The experiments show that the predicted gains using the program package McStas are realized. We discuss several applications of <span class="hlt">elliptic</span> guides in various fields of neutron physics.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://www.osti.gov/scitech/servlets/purl/197802','SCIGOV-STC'); return false;" href="http://www.osti.gov/scitech/servlets/purl/197802"><span id="translatedtitle">An <span class="hlt">elliptical</span> wiggler beamline for the ALS</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Martynov, V.V. |; McKinney, W.R.; Padmore, H.A.</p> <p>1995-10-01</p> <p>A beamline for circularly polarized radiation produced by an <span class="hlt">elliptical</span> wiggler has been designed at the ALS covering the broad energy range from 50 eV to 2000 eV. The rigorous theory of grating diffraction efficiency has been used to maximize transmitted flux. The nature of the <span class="hlt">elliptical</span> wiggler insertion device creates a challenging optical problem due to the large source size in the vertical and horizontal directions. The requirement of high resolving power, combined with the broad tuning range and high heat loads complicate the design. These problems have been solved by using a variable included angle monochromator of the ``constant length`` type with high demagnification onto its entrance slit, and cooled optics.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://www.osti.gov/scitech/servlets/purl/1333527','SCIGOV-STC'); return false;" href="http://www.osti.gov/scitech/servlets/purl/1333527"><span id="translatedtitle"><span class="hlt">Elliptic</span> Genera and 3d Gravity</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Benjamin, Nathan; Cheng, Miranda C. N.; Kachru, Shamit; Moore, Gregory W.; Paquette, Natalie M.</p> <p>2016-03-30</p> <p>We describe general constraints on the <span class="hlt">elliptic</span> genus of a 2d supersymmetric conformal field theory which has a gravity dual with large radius in Planck units. We give examples of theories which do and do not satisfy the bounds we derive, by describing the <span class="hlt">elliptic</span> genera of symmetric product orbifolds of K3, product manifolds, certain simple families of Calabi–Yau hypersurfaces, and symmetric products of the “Monster CFT”. We discuss the distinction between theories with supergravity duals and those whose duals have strings at the scale set by the AdS curvature. Under natural assumptions, we attempt to quantify the fraction of (2,2) supersymmetric conformal theories which admit a weakly curved gravity description, at large central charge.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://www.osti.gov/scitech/servlets/purl/1331206','SCIGOV-STC'); return false;" href="http://www.osti.gov/scitech/servlets/purl/1331206"><span id="translatedtitle"><span class="hlt">Elliptic</span> genera and 3d gravity</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Benjamin, Nathan; Cheng, Miranda C. N.; Kachru, Shamit; Moore, Gregory W.; Paquette, Natalie M.</p> <p>2016-03-30</p> <p>Here, we describe general constraints on the <span class="hlt">elliptic</span> genus of a 2d supersymmetric conformal field theory which has a gravity dual with large radius in Planck units. We give examples of theories which do and do not satisfy the bounds we derive, by describing the <span class="hlt">elliptic</span> genera of symmetric product orbifolds of K<sub>3</sub>, product manifolds, certain simple families of Calabi–Yau hypersurfaces, and symmetric products of the “Monster CFT”. We discuss the distinction between theories with supergravity duals and those whose duals have strings at the scale set by the AdS curvature. Under natural assumptions, we attempt to quantify the fraction of (2,2) supersymmetric conformal theories which admit a weakly curved gravity description, at large central charge.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/pages/biblio/1331206-elliptic-genera-gravity','SCIGOV-DOEP'); return false;" href="https://www.osti.gov/pages/biblio/1331206-elliptic-genera-gravity"><span id="translatedtitle"><span class="hlt">Elliptic</span> genera and 3d gravity</span></a></p> <p><a target="_blank" href="http://www.osti.gov/pages">DOE PAGES</a></p> <p>Benjamin, Nathan; Cheng, Miranda C. N.; Kachru, Shamit; ...</p> <p>2016-03-30</p> <p>Here, we describe general constraints on the <span class="hlt">elliptic</span> genus of a 2d supersymmetric conformal field theory which has a gravity dual with large radius in Planck units. We give examples of theories which do and do not satisfy the bounds we derive, by describing the <span class="hlt">elliptic</span> genera of symmetric product orbifolds of K3, product manifolds, certain simple families of Calabi–Yau hypersurfaces, and symmetric products of the “Monster CFT”. We discuss the distinction between theories with supergravity duals and those whose duals have strings at the scale set by the AdS curvature. Under natural assumptions, we attempt to quantify the fractionmore » of (2,2) supersymmetric conformal theories which admit a weakly curved gravity description, at large central charge.« less</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://www.dtic.mil/docs/citations/ADA241798','DTIC-ST'); return false;" href="http://www.dtic.mil/docs/citations/ADA241798"><span id="translatedtitle">Crack Path Prediction Near an <span class="hlt">Elliptical</span> Inhomogeneity</span></a></p> <p><a target="_blank" href="https://publicaccess.dtic.mil/psm/api/service/search/search">DTIC Science & Technology</a></p> <p></p> <p>1991-09-01</p> <p>Prediction Near an <span class="hlt">Elliptical</span> Inhomogeneity 1L162618AH80 6. AUTHOR(S) Edward M. Patton 7. PERFORMING ORGANIZATION NAME(S) AND ADDRESS(ES) 8 . PERFORMING...oriented crack. Erdogan and Gupta [ 8 ] later solved the problem in which the crack crosses the interface. These solutions are based on the Green’s...the crack propagation direction 8 is greatest. This criterion implies that the stress parallel to that direction would be a minimum, or that the</p> </li> </ol> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_6");'>6</a></li> <li><a href="#" onclick='return showDiv("page_7");'>7</a></li> <li class="active"><span>8</span></li> <li><a href="#" onclick='return showDiv("page_9");'>9</a></li> <li><a href="#" onclick='return showDiv("page_10");'>10</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div><!-- col-sm-12 --> </div><!-- row --> </div><!-- page_8 --> <div id="page_9" class="hiddenDiv"> <div class="row"> <div class="col-sm-12"> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_7");'>7</a></li> <li><a href="#" onclick='return showDiv("page_8");'>8</a></li> <li class="active"><span>9</span></li> <li><a href="#" onclick='return showDiv("page_10");'>10</a></li> <li><a href="#" onclick='return showDiv("page_11");'>11</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div> </div> <div class="row"> <div class="col-sm-12"> <ol class="result-class" start="161"> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19820035254&hterms=photoacoustic&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D10%26Ntt%3Dphotoacoustic','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19820035254&hterms=photoacoustic&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D10%26Ntt%3Dphotoacoustic"><span id="translatedtitle">Photoacoustic cell using <span class="hlt">elliptical</span> acoustic focusing</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Heritier, J.-M.; Fouquet, J. E.; Siegman, A. E.</p> <p>1982-01-01</p> <p>A photoacoustic cell has been developed in the form of an <span class="hlt">elliptical</span> cylinder in which essentially all the acoustic energy generated by a laser beam passing down one axis is focused onto a cylindrical acoustic tranducer located along the other axis. Preliminary measurements on a liquid-filled cell of this design show high sensitivity and a notably clean impulse response. A similar design may be useful for photoacoustic measurements in vapors as well.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19840021491','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19840021491"><span id="translatedtitle">Spectral methods for exterior <span class="hlt">elliptic</span> problems</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Canuto, C.; Hariharan, S. I.; Lustman, L.</p> <p>1984-01-01</p> <p>Spectral approximations for exterior <span class="hlt">elliptic</span> problems in two dimensions are discussed. As in the conventional finite difference or finite element methods, the accuracy of the numerical solutions is limited by the order of the numerical farfield conditions. A spectral boundary treatment is introduced at infinity which is compatible with the infinite order interior spectral scheme. Computational results are presented to demonstrate the spectral accuracy attainable. Although a simple Laplace problem is examined, the analysis covers more complex and general cases.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2004JPhA...37.2721T','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2004JPhA...37.2721T"><span id="translatedtitle">Integrable mappings via rational <span class="hlt">elliptic</span> surfaces</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Tsuda, Teruhisa</p> <p>2004-02-01</p> <p>We present a geometric description of the QRT map (which is an integrable mapping introduced by Quispel, Roberts and Thompson) in terms of the addition formula of a rational <span class="hlt">elliptic</span> surface. By this formulation, we classify all the cases when the QRT map is periodic; and show that its period is 2, 3, 4, 5 or 6. A generalization of the QRT map which acts birationally on a pencil of K3 surfaces, or Calabi-Yau manifolds, is also presented.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://www.dtic.mil/docs/citations/ADA581793','DTIC-ST'); return false;" href="http://www.dtic.mil/docs/citations/ADA581793"><span id="translatedtitle"><span class="hlt">Elliptical</span> Acoustic Particle Motion in Underwater Waveguides</span></a></p> <p><a target="_blank" href="https://publicaccess.dtic.mil/psm/api/service/search/search">DTIC Science & Technology</a></p> <p></p> <p>2013-03-27</p> <p>approximation to the degree of circularity. This approximation, applied to acoustic pressure measurements from two closely spaced hydrophones made in...<span class="hlt">elliptical</span> motion in the vertical plane can be approximated by vertical line array of closely spaced pressure sensors. We demonstrate in this paper how the...an approximate measure of circular- ity. Most importantly, Θ̃ can be formed from two closely spaced (< λ/4) hydrophones, extending this analysis of</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/1990Ap%26SS.168...89G','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/1990Ap%26SS.168...89G"><span id="translatedtitle">Do <span class="hlt">elliptical</span> galaxies suffer from warp?</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Gamaleldin, A. I.</p> <p>1990-06-01</p> <p>Detailed surface isophotometry of NGC 1700 was performed. Luminosity profiles, <span class="hlt">ellipticity</span> curve, reduced luminosity profiles, and the galaxy parameters are illustrated; the study also includes the variation of position angle with the distance from the center of the galaxy. An interesting feature of this object is the twisted shape of the outer isophote which does not appear as an ellipse but as an integral-sign shape, which is attributed to some kind of warp in the galaxy under investigation.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/1992ApJ...396..741L','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/1992ApJ...396..741L"><span id="translatedtitle">Molecular Gas in <span class="hlt">Elliptical</span> Galaxies: Erratum</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Lees, Joanna F.; Knapp, G. R.; Rupen, Michael P.; Phillips, T. G.</p> <p>1992-09-01</p> <p>In the paper "Molecular Gas in <span class="hlt">Elliptical</span> Galaxies" by Joanna F. Lees, G. R. Knapp, Michael P. Rupen, and T. G. Phillips (ApJ, 379,177 [1991]), an error appeared on page 208. Two numbers which were quoted from Young and Knezek (1989) were inadvertently not converted from their CO-H_2_ conversion factor to ours (a difference of 40%). Page 208, column (1), lines 6-7 should read:</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4078883','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4078883"><span id="translatedtitle">MIB Galerkin method for <span class="hlt">elliptic</span> interface problems</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Xia, Kelin; Zhan, Meng; Wei, Guo-Wei</p> <p>2014-01-01</p> <p>Summary Material interfaces are omnipresent in the real-world structures and devices. Mathematical modeling of material interfaces often leads to <span class="hlt">elliptic</span> partial differential equations (PDEs) with discontinuous coefficients and singular sources, which are commonly called <span class="hlt">elliptic</span> interface problems. The development of high-order numerical schemes for <span class="hlt">elliptic</span> interface problems has become a well defined field in applied and computational mathematics and attracted much attention in the past decades. Despite of significant advances, challenges remain in the construction of high-order schemes for nonsmooth interfaces, i.e., interfaces with geometric singularities, such as tips, cusps and sharp edges. The challenge of geometric singularities is amplified when they are associated with low solution regularities, e.g., tip-geometry effects in many fields. The present work introduces a matched interface and boundary (MIB) Galerkin method for solving two-dimensional (2D) <span class="hlt">elliptic</span> PDEs with complex interfaces, geometric singularities and low solution regularities. The Cartesian grid based triangular elements are employed to avoid the time consuming mesh generation procedure. Consequently, the interface cuts through elements. To ensure the continuity of classic basis functions across the interface, two sets of overlapping elements, called MIB elements, are defined near the interface. As a result, differentiation can be computed near the interface as if there is no interface. Interpolation functions are constructed on MIB element spaces to smoothly extend function values across the interface. A set of lowest order interface jump conditions is enforced on the interface, which in turn, determines the interpolation functions. The performance of the proposed MIB Galerkin finite element method is validated by numerical experiments with a wide range of interface geometries, geometric singularities, low regularity solutions and grid resolutions. Extensive numerical studies confirm</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://www.dtic.mil/docs/citations/ADA619858','DTIC-ST'); return false;" href="http://www.dtic.mil/docs/citations/ADA619858"><span id="translatedtitle">Random Matrix Theory and <span class="hlt">Elliptic</span> Curves</span></a></p> <p><a target="_blank" href="https://publicaccess.dtic.mil/psm/api/service/search/search">DTIC Science & Technology</a></p> <p></p> <p>2014-11-24</p> <p>related to the intervals of prime numbers. 15. SUBJECT TERMS EOARD, Random Matrix theory, Riemann Hypothesis, <span class="hlt">Elliptic</span> Curves 16. SECURITY...range of quantities of fundamental importance in number theory. In the cases of the Riemann zeta function and Dirichlet L-functions, this information...investigation using analytic techniques. As an indication of their significance, two of the Clay Millennium Prize Problems, the Riemann Hypothesis and the</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/24999292','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/24999292"><span id="translatedtitle">MIB Galerkin method for <span class="hlt">elliptic</span> interface problems.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Xia, Kelin; Zhan, Meng; Wei, Guo-Wei</p> <p>2014-12-15</p> <p>Material interfaces are omnipresent in the real-world structures and devices. Mathematical modeling of material interfaces often leads to <span class="hlt">elliptic</span> partial differential equations (PDEs) with discontinuous coefficients and singular sources, which are commonly called <span class="hlt">elliptic</span> interface problems. The development of high-order numerical schemes for <span class="hlt">elliptic</span> interface problems has become a well defined field in applied and computational mathematics and attracted much attention in the past decades. Despite of significant advances, challenges remain in the construction of high-order schemes for nonsmooth interfaces, i.e., interfaces with geometric singularities, such as tips, cusps and sharp edges. The challenge of geometric singularities is amplified when they are associated with low solution regularities, e.g., tip-geometry effects in many fields. The present work introduces a matched interface and boundary (MIB) Galerkin method for solving two-dimensional (2D) <span class="hlt">elliptic</span> PDEs with complex interfaces, geometric singularities and low solution regularities. The Cartesian grid based triangular elements are employed to avoid the time consuming mesh generation procedure. Consequently, the interface cuts through elements. To ensure the continuity of classic basis functions across the interface, two sets of overlapping elements, called MIB elements, are defined near the interface. As a result, differentiation can be computed near the interface as if there is no interface. Interpolation functions are constructed on MIB element spaces to smoothly extend function values across the interface. A set of lowest order interface jump conditions is enforced on the interface, which in turn, determines the interpolation functions. The performance of the proposed MIB Galerkin finite element method is validated by numerical experiments with a wide range of interface geometries, geometric singularities, low regularity solutions and grid resolutions. Extensive numerical studies confirm the</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://www.osti.gov/scitech/servlets/purl/763231','SCIGOV-STC'); return false;" href="http://www.osti.gov/scitech/servlets/purl/763231"><span id="translatedtitle"><span class="hlt">Elliptic</span> Solvers for Adaptive Mesh Refinement Grids</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Quinlan, D.J.; Dendy, J.E., Jr.; Shapira, Y.</p> <p>1999-06-03</p> <p>We are developing multigrid methods that will efficiently solve <span class="hlt">elliptic</span> problems with anisotropic and discontinuous coefficients on adaptive grids. The final product will be a library that provides for the simplified solution of such problems. This library will directly benefit the efforts of other Laboratory groups. The focus of this work is research on serial and parallel <span class="hlt">elliptic</span> algorithms and the inclusion of our black-box multigrid techniques into this new setting. The approach applies the Los Alamos object-oriented class libraries that greatly simplify the development of serial and parallel adaptive mesh refinement applications. In the final year of this LDRD, we focused on putting the software together; in particular we completed the final AMR++ library, we wrote tutorials and manuals, and we built example applications. We implemented the Fast Adaptive Composite Grid method as the principal <span class="hlt">elliptic</span> solver. We presented results at the Overset Grid Conference and other more AMR specific conferences. We worked on optimization of serial and parallel performance and published several papers on the details of this work. Performance remains an important issue and is the subject of continuing research work.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/1995PASP..107..502G','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/1995PASP..107..502G"><span id="translatedtitle">Dust and Ionized Gas in <span class="hlt">Elliptical</span> Galaxies</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Goudfrooij, Paul</p> <p>1995-05-01</p> <p>The thesis presents results of a study of the optical and far-infrared properties of dust and ionized gas in a complete, blue magnitude-limited (B_T^0 < 12) sample of 56 luminous <span class="hlt">elliptical</span> (E) galaxies. The main aim is to investigate the origin and fate of this interstellar material and possible implications for scenarios of galaxy formation and evolution. To ensure consistency in the assignment of morphological types, the galaxy sample was drawn exclusively from the Revised Shapley-Ames Catalog of Bright Galaxies. A deep, systematic optical survey has been performed, including CCD imaging through both broad-band filters and narrow-band filters. For each galaxy we have constructed colour index (B-V, B-I) images and images of the H-alpha+ [N II]-emitting gas to derive the distributions of dust features and ionized gas. Long-slit spectra have also been obtained in two resolutions. Low-resolution spectra (covering the whole optical region) are used to study the properties of the underlying stellar populations (e.g., metallicity gradients), and to study the excitation mechanism of the ionized gas. Additional medium-resolution (~2A) spectra in the wavelength region around H-alpha have been obtained for all sample <span class="hlt">elliptical</span> galaxies containing ionized gas to study the kinematics of the gas, and derive pure H-alpha luminosities. In this thesis, analysis of the extensive imaging data and of the medium-resolution spectra is reported. In Chapter 1 we report an early result of our survey: The galaxy IC 1459 is found to exhibit a large (15 Kpc diameter) H-alpha+[N II] emission-line region, showing spiral structure. Patchy dust absorption is also found in the inner part of the emission-line region. This galaxy was already shown to contain a massive stellar core which counter-rotates rapidly with respect to the stellar body of the galaxy. Interestingly, the sense of rotation of the spiral "arms" of the ionized gas distribution is the same as that of the rapidly rotating</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/1231654','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/1231654"><span id="translatedtitle"><span class="hlt">Intrinsic</span> Feature Motion Tracking</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Goddard, Jr., James S.</p> <p>2013-03-19</p> <p>Subject motion during 3D medical scanning can cause blurring and artifacts in the 3D images resulting in either rescans or poor diagnosis. Anesthesia or physical restraints may be used to eliminate motion but are undesirable and can affect results. This software measures the six degree of freedom 3D motion of the subject during the scan under a rigidity assumption using only the <span class="hlt">intrinsic</span> features present on the subject area being monitored. This movement over time can then be used to correct the scan data removing the blur and artifacts. The software acquires images from external cameras or images stored on disk for processing. The images are from two or three calibrated cameras in a stereo arrangement. Algorithms extract and track the features over time and calculate position and orientation changes relative to an initial position. Output is the 3D position and orientation change measured at each image.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016PhRvL.117x0505M','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016PhRvL.117x0505M"><span id="translatedtitle">Gaussian <span class="hlt">Intrinsic</span> Entanglement</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Mišta, Ladislav; Tatham, Richard</p> <p>2016-12-01</p> <p>We introduce a cryptographically motivated quantifier of entanglement in bipartite Gaussian systems called Gaussian <span class="hlt">intrinsic</span> entanglement (GIE). The GIE is defined as the optimized mutual information of a Gaussian distribution of outcomes of measurements on parts of a system, conditioned on the outcomes of a measurement on a purifying subsystem. We show that GIE vanishes only on separable states and exhibits monotonicity under Gaussian local trace-preserving operations and classical communication. In the two-mode case, we compute GIE for all pure states as well as for several important classes of symmetric and asymmetric mixed states. Surprisingly, in all of these cases, GIE is equal to Gaussian Rényi-2 entanglement. As GIE is operationally associated with the secret-key agreement protocol and can be computed for several important classes of states, it offers a compromise between computable and physically meaningful entanglement quantifiers.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19880035410&hterms=Variable+stars&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D30%26Ntt%3DVariable%2Bstars','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19880035410&hterms=Variable+stars&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D30%26Ntt%3DVariable%2Bstars"><span id="translatedtitle"><span class="hlt">Intrinsically</span> variable stars</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Bohm-Vitense, Erika; Querci, Monique</p> <p>1987-01-01</p> <p>The characteristics of <span class="hlt">intrinsically</span> variable stars are examined, reviewing the results of observations obtained with the IUE satellite since its launch in 1978. Selected data on both medium-spectral-class pulsating stars (Delta Cep stars, W Vir stars, and related groups) and late-type variables (M, S, and C giants and supergiants) are presented in spectra, graphs, and tables and described in detail. Topics addressed include the calibration of the the period-luminosity relation, Cepheid distance determination, checking stellar evolution theory by the giant companions of Cepheids, Cepheid masses, the importance of the hydrogen convection zone in Cepheids, temperature and abundance estimates for Population II pulsating stars, mass loss in Population II Cepheids, SWP and LWP images of cold giants and supergiants, temporal variations in the UV lines of cold stars, C-rich cold stars, and cold stars with highly ionized emission lines.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/22167534','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/22167534"><span id="translatedtitle">THE DARK HALO-SPHEROID CONSPIRACY AND THE ORIGIN OF <span class="hlt">ELLIPTICAL</span> GALAXIES</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Remus, Rhea-Silvia; Burkert, Andreas; Dolag, Klaus; Johansson, Peter H.; Naab, Thorsten; Oser, Ludwig; Thomas, Jens</p> <p>2013-04-01</p> <p>Dynamical modeling and strong-lensing data indicate that the total density profiles of early-type galaxies are close to isothermal, i.e., {rho}{sub tot}{proportional_to}r {sup {gamma}} with {gamma} Almost-Equal-To -2. To understand the origin of this universal slope we study a set of simulated spheroids formed in isolated binary mergers as well as the formation within the cosmological framework. The total stellar plus dark matter density profiles can always be described by a power law with an index of {gamma} Almost-Equal-To -2.1 with a tendency toward steeper slopes for more compact, lower-mass <span class="hlt">ellipticals</span>. In the binary mergers the amount of gas involved in the merger determines the precise steepness of the slope. This agrees with results from the cosmological simulations where <span class="hlt">ellipticals</span> with steeper slopes have a higher fraction of stars formed in situ. Each gas-poor merger event evolves the slope toward {gamma} {approx} -2, once this slope is reached further merger events do not change it anymore. All our <span class="hlt">ellipticals</span> have flat <span class="hlt">intrinsic</span> combined stellar and dark matter velocity dispersion profiles. We conclude that flat velocity dispersion profiles and total density distributions with a slope of {gamma} {approx} -2 for the combined system of stars and dark matter act as a natural attractor. The variety of complex formation histories as present in cosmological simulations, including major as well as minor merger events, is essential to generate the full range of observed density slopes seen for present-day <span class="hlt">elliptical</span> galaxies.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/20030065802','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/20030065802"><span id="translatedtitle"><span class="hlt">Elliptic</span> Functions and Integrals with Real Modulus in Fluid Mechanics</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Legendre, Robert</p> <p>1958-01-01</p> <p>Advantage of the <span class="hlt">elliptic</span> functions and of the more general functions of Schwarz for fluid mechanics. Flows outside and inside polygons. Application to the calculation of an elbow diffuser for a wind tunnel. Properties of the <span class="hlt">elliptic</span> integrals of the first kind and of the <span class="hlt">elliptic</span> functions. Properties of the theta functions and decomposition of the <span class="hlt">elliptic</span> functions into products of theta functions. Properties of the zeta functions. Decomposition of the <span class="hlt">elliptic</span> functions into sums of zeta functions and calculations of the <span class="hlt">elliptic</span> integrals. Applications to the calculation of wing profiles, of compressor profiles, and to the study of the vibrations of airplane wings and of compressor vanes. The manuscript of the present paper was checked by Mr. Eichelbrenner who corrected several imperfections and suggested numerous improvements to make reading of the paper easier. However, the limited subject does not permit filling in more than an incomplete knowledge of the properties of analytic functions.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016IJQI...1450028J','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016IJQI...1450028J"><span id="translatedtitle">Qutrit teleportation under <span class="hlt">intrinsic</span> decoherence</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Jafarpour, Mojtaba; Naderi, Negar</p> <p>2016-08-01</p> <p>We study qutrit teleportation and its fidelity in the presence and absence of <span class="hlt">intrinsic</span> decoherence through a qutrit channel. The channel consists of a Heisenberg chain with xyz interaction model and the <span class="hlt">intrinsic</span> decoherence is implemented through the Milburn model. It is shown that while the fidelity diminishes due to <span class="hlt">intrinsic</span> decoherence, it may be enhanced if the channel is initially in an entangled state. It is also observed that, for stronger <span class="hlt">intrinsic</span> decoherence, the initial entanglement of the channel is more effective in enhancing of fidelity.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://www.dtic.mil/docs/citations/ADA619304','DTIC-ST'); return false;" href="http://www.dtic.mil/docs/citations/ADA619304"><span id="translatedtitle"><span class="hlt">Elliptic</span> Length Scales in Laminar, Two-Dimensional Supersonic Flows</span></a></p> <p><a target="_blank" href="https://publicaccess.dtic.mil/psm/api/service/search/search">DTIC Science & Technology</a></p> <p></p> <p>2015-06-01</p> <p>AFRL-RQ-WP-TP-2015-0109 <span class="hlt">ELLIPTIC</span> LENGTH SCALES IN LAMINAR, TWO- DIMENSIONAL SUPERSONIC FLOWS James H. Miller Vehicle Technology Branch...SUBTITLE <span class="hlt">ELLIPTIC</span> LENGTH SCALES IN LAMINAR, TWO-DIMENSIONAL SUPERSONIC FLOWS 5a. CONTRACT NUMBER In-house 5b. GRANT NUMBER 5c. PROGRAM ELEMENT...ANSI Std. Z39-18 1 Approved for public release; distribution unlimited. <span class="hlt">Elliptic</span> Length Scales in Laminar, Two-Dimensional Supersonic Flows</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2015JHEP...07..112B','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2015JHEP...07..112B"><span id="translatedtitle"><span class="hlt">Elliptic</span> multiple zeta values and one-loop superstring amplitudes</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Broedel, Johannes; Mafra, Carlos R.; Matthes, Nils; Schlotterer, Oliver</p> <p>2015-07-01</p> <p>We investigate iterated integrals on an <span class="hlt">elliptic</span> curve, which are a natural genus-one generalization of multiple polylogarithms. These iterated integrals coincide with the multiple <span class="hlt">elliptic</span> polylogarithms introduced by Brown and Levin when constrained to the real line. At unit argument they reduce to an <span class="hlt">elliptic</span> analogue of multiple zeta values, whose network of relations we start to explore. A simple and natural application of this framework are one-loop scattering amplitudes in open superstring theory. In particular, <span class="hlt">elliptic</span> multiple zeta values are a suitable language to express their low energy limit. Similar to the techniques available at tree-level, our formalism allows to completely automatize the calculation.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/20389709','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/20389709"><span id="translatedtitle">Two-dimensional <span class="hlt">elliptical</span> electromagnetic superscatterer and superabsorber.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Zang, Xiaofei; Jiang, Chun</p> <p>2010-03-29</p> <p>Using coordinate transformation stated earlier by Pendry et al. [Science 312, 1780 (2006)], we investigate the two-dimensional <span class="hlt">elliptical</span> electromagnetic superscatterer and superabsorber, based on the concept of complementary media. Such an <span class="hlt">elliptical</span> electromagnetic superscatterer (or superabsorber) is realized by coating an <span class="hlt">elliptical</span> negative refractive material shell. The effectiveness of the <span class="hlt">elliptical</span> electromagnetic superscatterer and superabsorber designs is verified by finite element simulations. The proposed design provides a more practical superscatterer (or superabsorber) geometry when compared to previous designs with axial and radial symmetries. Our results can be extended to an arbitrarily shaped electromagnetic superscatterer and superabsorber.</p> </li> </ol> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_7");'>7</a></li> <li><a href="#" onclick='return showDiv("page_8");'>8</a></li> <li class="active"><span>9</span></li> <li><a href="#" onclick='return showDiv("page_10");'>10</a></li> <li><a href="#" onclick='return showDiv("page_11");'>11</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div><!-- col-sm-12 --> </div><!-- row --> </div><!-- page_9 --> <div id="page_10" class="hiddenDiv"> <div class="row"> <div class="col-sm-12"> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_8");'>8</a></li> <li><a href="#" onclick='return showDiv("page_9");'>9</a></li> <li class="active"><span>10</span></li> <li><a href="#" onclick='return showDiv("page_11");'>11</a></li> <li><a href="#" onclick='return showDiv("page_12");'>12</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div> </div> <div class="row"> <div class="col-sm-12"> <ol class="result-class" start="181"> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/5926364','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/5926364"><span id="translatedtitle">Mixing characteristics of a ducted, <span class="hlt">elliptical</span> jet with dump</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Schadow, K.C.; Wilson, K.J.; Parr, D.M.; Gutmark, E.</p> <p>1986-01-01</p> <p>Mixing between <span class="hlt">elliptical</span> ducted air-jets with dump and nitrogen radially injected through the duct walls was experimentally studied using hot-wire anemometry and gas-sampling techniques. Mixing was considerably increased when the air-jet was issued from <span class="hlt">elliptical</span> relative to circular jet-exit cross-sections. <span class="hlt">Elliptical</span> jets issued from orifices provided better mixing than issued from pipes. Additional mixing enhancement was achieved when the <span class="hlt">elliptical</span> jets were acoustically forced by excited resonant pressure waves of the duct. The mean and turbulence velocity measurements provided insight into the mechanism of the observed mixing enhancement.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016AJ....152..214S','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016AJ....152..214S"><span id="translatedtitle">Colors of <span class="hlt">Ellipticals</span> from GALEX to Spitzer</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Schombert, James M.</p> <p>2016-12-01</p> <p>Multi-color photometry is presented for a large sample of local <span class="hlt">ellipticals</span> selected by morphology and isolation. The sample uses data from the Galaxy Evolution Explorer (GALEX), Sloan Digital Sky Survey (SDSS), Two Micron All-Sky Survey (2MASS), and Spitzer to cover the filters NUV, ugri, JHK and 3.6 μm. Various two-color diagrams, using the half-light aperture defined in the 2MASS J filter, are very coherent from color to color, meaning that galaxies defined to be red in one color are always red in other colors. Comparison to globular cluster colors demonstrates that <span class="hlt">ellipticals</span> are not composed of a single age, single metallicity (e.g., [Fe/H]) stellar population, but require a multi-metallicity model using a chemical enrichment scenario. Such a model is sufficient to explain two-color diagrams and the color-magnitude relations for all colors using only metallicity as a variable on a solely 12 Gyr stellar population with no evidence of stars younger than 10 Gyr. The [Fe/H] values that match galaxy colors range from -0.5 to +0.4, much higher (and older) than population characteristics deduced from Lick/IDS line-strength system studies, indicating an inconsistency between galaxy colors and line indices values for reasons unknown. The NUV colors have unusual behavior, signaling the rise and fall of the UV upturn with <span class="hlt">elliptical</span> luminosity. Models with blue horizontal branch tracks can reproduce this behavior, indicating the UV upturn is strictly a metallicity effect.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2008APS..MAR.C1189K','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2008APS..MAR.C1189K"><span id="translatedtitle"><span class="hlt">Intrinsic</span> Friction Microscopy</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Knorr, Daniel; Overney, Rene</p> <p>2008-03-01</p> <p>A novel scanning probe methodology based on lateral force microscopy is presented wherein kinetic friction measurements, obtained as a function of velocity for various temperatures, are used to deduce apparent Arrhenius-type activation energies for surface and subsurface molecular mobilities. Depending on the coupling strength (cooperativity) between molecular mobilities involved the dissipation energy can carry a significant entropic energy contribution, accounting for the majority of the apparent Arrhenius activation energy. The <span class="hlt">intrinsic</span> friction methodology also provides a means of directly separating enthalpic energy contributions from entropic ones by employing absolute rate theory. As such, the degree of cooperativity in the system is readily apparent. This methodology is illustrated with nanoscale tribological experiments on two systems, (1) monodisperse, atactic polystyrene and (2) self assembling molecular glassy chromophores. In polystyrene, dissipation was found to be a discrete function of loading, where the γ-relaxation (phenyl group rotation) was recovered for ultra low loads and the β-relaxation (local backbone translation) for higher loads in the same temperature range, indicating sensitivity to surface and subsurface mobilities. For self assembling glassy chromophores, the degree of intermolecular cooperativity was deduced using the methodology, resulting in an increased understanding of the interactions between self assembling molecules.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://www.osti.gov/scitech/biblio/5215234','DOE-PATENT-XML'); return false;" href="http://www.osti.gov/scitech/biblio/5215234"><span id="translatedtitle"><span class="hlt">Intrinsically</span> irreversible heat engine</span></a></p> <p><a target="_blank" href="http://www.osti.gov/doepatents">DOEpatents</a></p> <p>Wheatley, J.C.; Swift, G.W.; Migliori, A.</p> <p>1984-01-01</p> <p>A class of heat engines based on an <span class="hlt">intrinsically</span> irreversible heat transfer process is disclosed. In a typical embodiment the engine comprises a compressible fluid that is cyclically compressed and expanded while at the same time being driven in reciprocal motion by a positive displacement drive means. A second thermodynamic medium is maintained in imperfect thermal contact with the fluid and bears a broken thermodynamic symmetry with respect to the fluid. The second thermodynamic medium is a structure adapted to have a low fluid flow impedance with respect to the compressible fluid, and which is further adapted to be in only moderate thermal contact with the fluid. In operation, thermal energy is pumped along the second medium due to a phase lag between the cyclical heating and cooling of the fluid and the resulting heat conduction between the fluid and the medium. In a preferred embodiment the engine comprises an acoustical drive and a housing containing a gas which is driven at a resonant frequency so as to be maintained in a standing wave. Operation of the engine at acoustic frequencies improves the power density and coefficient of performance. The second thermodynamic medium can be coupled to suitable heat exchangers to utilize the engine as a simple refrigeration device having no mechanical moving parts. Alternatively, the engine is reversible in function so as to be utilizable as a prime mover by coupling it to suitable sources and sinks of heat.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://www.osti.gov/scitech/biblio/7255177','DOE-PATENT-XML'); return false;" href="http://www.osti.gov/scitech/biblio/7255177"><span id="translatedtitle"><span class="hlt">Intrinsically</span> irreversible heat engine</span></a></p> <p><a target="_blank" href="http://www.osti.gov/doepatents">DOEpatents</a></p> <p>Wheatley, J.C.; Swift, G.W.; Migliori, A.</p> <p>1984-12-25</p> <p>A class of heat engines based on an <span class="hlt">intrinsically</span> irreversible heat transfer process is disclosed. In a typical embodiment the engine comprises a compressible fluid that is cyclically compressed and expanded while at the same time being driven in reciprocal motion by a positive displacement drive means. A second thermodynamic medium is maintained in imperfect thermal contact with the fluid and bears a broken thermodynamic symmetry with respect to the fluid. The second thermodynamic medium is a structure adapted to have a low fluid flow impedance with respect to the compressible fluid, and which is further adapted to be in only moderate thermal contact with the fluid. In operation, thermal energy is pumped along the second medium due to a phase lag between the cyclical heating and cooling of the fluid and the resulting heat conduction between the fluid and the medium. In a preferred embodiment the engine comprises an acoustical drive and a housing containing a gas which is driven at a resonant frequency so as to be maintained in a standing wave. Operation of the engine at acoustic frequencies improves the power density and coefficient of performance. The second thermodynamic medium can be coupled to suitable heat exchangers to utilize the engine as a simple refrigeration device having no mechanical moving parts. Alternatively, the engine is reversible in function so as to be utilizable as a prime mover by coupling it to suitable sources and sinks of heat. 11 figs.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://www.osti.gov/scitech/servlets/purl/865290','DOE-PATENT-XML'); return false;" href="http://www.osti.gov/scitech/servlets/purl/865290"><span id="translatedtitle"><span class="hlt">Intrinsically</span> irreversible heat engine</span></a></p> <p><a target="_blank" href="http://www.osti.gov/doepatents">DOEpatents</a></p> <p>Wheatley, John C.; Swift, Gregory W.; Migliori, Albert</p> <p>1984-01-01</p> <p>A class of heat engines based on an <span class="hlt">intrinsically</span> irreversible heat transfer process is disclosed. In a typical embodiment the engine comprises a compressible fluid that is cyclically compressed and expanded while at the same time being driven in reciprocal motion by a positive displacement drive means. A second thermodynamic medium is maintained in imperfect thermal contact with the fluid and bears a broken thermodynamic symmetry with respect to the fluid. the second thermodynamic medium is a structure adapted to have a low fluid flow impedance with respect to the compressible fluid, and which is further adapted to be in only moderate thermal contact with the fluid. In operation, thermal energy is pumped along the second medium due to a phase lag between the cyclical heating and cooling of the fluid and the resulting heat conduction between the fluid and the medium. In a preferred embodiment the engine comprises an acoustical drive and a housing containing a gas which is driven at a resonant frequency so as to be maintained in a standing wave. Operation of the engine at acoustic frequencies improves the power density and coefficient of performance. The second thermodynamic medium can be coupled to suitable heat exchangers to utilize the engine as a simple refrigeration device having no mechanical moving parts. Alternatively, the engine is reversible in function so as to be utilizable as a prime mover by coupling it to suitable sources and sinks of heat.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2009Ap%26SS.320...51S','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2009Ap%26SS.320...51S"><span id="translatedtitle">Young circumnuclear disks in <span class="hlt">elliptical</span> galaxies</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Sil'Chenko, Olga K.</p> <p>2009-04-01</p> <p>By means of integral-field spectroscopy with the Multi-Pupil Field/Fiber Spectrograph of the Russian 6-m telescope we have studied the central parts of NGC 759 and NGC 83— regular (non-interacting, without strong nuclear activity) round red luminous ( M B =-20.8--21.6) <span class="hlt">elliptical</span> galaxies which are however known to possess molecular gas. In both galaxies we have found central stellar disks with the extension of 1-2 kpc along the radius which are evidently being formed just now.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/20640295','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/20640295"><span id="translatedtitle"><span class="hlt">Elliptic</span> Rydberg states as direction indicators</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Lindner, Netanel H.; Peres, Asher; Terno, Daniel R.</p> <p>2003-10-01</p> <p>The orientation in space of a Cartesian coordinate system can be indicated by the two vectorial constants of motion of a classical Keplerian orbit: the angular momentum and the Laplace-Runge-Lenz vector. In quantum mechanics, the states of a hydrogen atom that mimic classical <span class="hlt">elliptic</span> orbits are the coherent states of the SO(4) rotation group. It is known how to produce these states experimentally. They have minimal dispersions of the two conserved vectors and can be used as direction indicators. We compare the fidelity of this transmission method with that of the idealized optimal method.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/20050186558','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/20050186558"><span id="translatedtitle">Evolution of Hot Gas in <span class="hlt">Elliptical</span> Galaxies</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Mathews, William G.</p> <p>2004-01-01</p> <p>This theory grant was awarded to study the curious nature, origin and evolution of hot gas in <span class="hlt">elliptical</span> galaxies and their surrounding groups. Understanding the properties of this X-ray emitting gas has profound implications over the broad landscape of modern astrophysics: cosmology, galaxy formation, star formation, cosmic metal enrichment, galactic structure and dynamics, and the physics of hot gases containing dust and magnetic fields. One of our principal specific objectives was to interpret the marvelous new observations from the XMM and Chandru satellite X-ray telescopes.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/21011330','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/21011330"><span id="translatedtitle">Guided modes of <span class="hlt">elliptical</span> metamaterial waveguides</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Halterman, Klaus; Feng, Simin; Overfelt, P. L.</p> <p>2007-07-15</p> <p>The propagation of guided electromagnetic waves in open <span class="hlt">elliptical</span> metamaterial waveguide structures is investigated. The waveguide contains a negative-index media core, where the permittivity {epsilon} and permeability {mu} are negative over a given bandwidth. The allowed mode spectrum for these structures is numerically calculated by solving a dispersion relation that is expressed in terms of Mathieu functions. By probing certain regions of parameter space, we find the possibility exists to have extremely localized waves that transmit along the surface of the waveguide.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2010JPhCS.218a2011M','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2010JPhCS.218a2011M"><span id="translatedtitle"><span class="hlt">Elliptic</span> waveforms for inspiralling compact binaries</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Mikóczi, Balázs</p> <p>2010-03-01</p> <p>The inspiral of supermassive black hole binary systems with high orbital eccentricity are the most promising sources for the gravitational wave observatories. The importance of <span class="hlt">elliptic</span> gravitational waveforms in various physical scenarios has been emphasized by several authors (Wahlquist 1987, Moreno-Garrido, Buitrago and Mediavilla 1994, Martel and Poisson 1999). Taking into account the eccentricity of the orbit in the total waveform improves the parameter estimation for these sources, as it is shown by the construction and analyzation of the Fisher information matrix. In our work we use the Fourier-Bessel analysis of the Kepler motion and the stationary phase approximation of time-depend waveforms.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2012MNRAS.427.3006R','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2012MNRAS.427.3006R"><span id="translatedtitle">The similar stellar populations of quiescent spiral and <span class="hlt">elliptical</span> galaxies</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Robaina, Aday R.; Hoyle, Ben; Gallazzi, Anna; Jiménez, Raul; van der Wel, Arjen; Verde, Licia</p> <p>2012-12-01</p> <p>We compare the stellar population properties in the central regions of visually classified non-star-forming spiral and <span class="hlt">elliptical</span> galaxies from Galaxy Zoo and Sloan Digital Sky Survey (SDSS) Data Release 7. The galaxies lie in the redshift range 0.04 < z < 0.1 and have stellar masses larger than log M* = 10.4. We select only face-on spiral galaxies in order to avoid contamination by light from the disc in the SDSS fibre and enabling the robust visual identification of spiral structure. Overall, we find that galaxies with larger central stellar velocity dispersions, regardless of morphological type, have older ages, higher metallicities and an increased overabundance of α-elements. Age and α-enhancement, at fixed velocity dispersion, do not depend on morphological type. The only parameter that, at a given velocity dispersion, <span class="hlt">correlates</span> with morphological type is metallicity, where the metallicity of the bulges of spiral galaxies is 0.07 dex higher than that of the <span class="hlt">ellipticals</span>. However, for galaxies with a given total stellar mass, this dependence on morphology disappears. Under the assumption that, for our sample, the velocity dispersion traces the mass of the bulge alone, as opposed to the total mass (bulge+disc) of the galaxy, our results imply that the formation epoch of galaxy and the duration of its star-forming period are linked to the mass of the bulge. The extent to which metals are retained within the galaxy, and not removed as a result of outflows, is determined by the total mass of the galaxy.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://eric.ed.gov/?q=electromagnetic+AND+radiation&pg=6&id=EJ203681','ERIC'); return false;" href="http://eric.ed.gov/?q=electromagnetic+AND+radiation&pg=6&id=EJ203681"><span id="translatedtitle"><span class="hlt">Intrinsic</span> Angular Momentum of Light.</span></a></p> <p><a target="_blank" href="http://www.eric.ed.gov/ERICWebPortal/search/extended.jsp?_pageLabel=advanced">ERIC Educational Resources Information Center</a></p> <p>Santarelli, Vincent</p> <p>1979-01-01</p> <p>Derives a familiar torque-angular momentum theorem for the electromagnetic field, and includes the <span class="hlt">intrinsic</span> torques exerted by the fields on the polarized medium. This inclusion leads to the expressions for the <span class="hlt">intrinsic</span> angular momentum carried by the radiation traveling through a charge-free medium. (Author/MA)</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/27806928','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/27806928"><span id="translatedtitle">The <span class="hlt">intrinsic</span> resistance of bacteria.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Gang, Zhang; Jie, Feng</p> <p>2016-10-20</p> <p>Antibiotic resistance is often considered to be a trait acquired by previously susceptible bacteria, on the basis of which can be attributed to the horizontal acquisition of new genes or the occurrence of spontaneous mutation. In addition to acquired resistance, bacteria have a trait of <span class="hlt">intrinsic</span> resistance to different classes of antibiotics. An <span class="hlt">intrinsic</span> resistance gene is involved in <span class="hlt">intrinsic</span> resistance, and its presence in bacterial strains is independent of previous antibiotic exposure and is not caused by horizontal gene transfer. Recently, interest in <span class="hlt">intrinsic</span> resistance genes has increased, because these gene products not only may provide attractive therapeutic targets for development of novel drugs that rejuvenate the activity of existing antibiotics, and but also might predict future emergence of resistant pathogens if they become mobilized. In the present review, we summarize the conventional examples of <span class="hlt">intrinsic</span> resistance, including the impermeability of cellular envelopes, the activity of multidrug efflux pumps or lack of drug targets. We also demonstrate that transferases and enzymes involved in basic bacterial metabolic processes confer <span class="hlt">intrinsic</span> resistance in Escherichia coli, Pseudomonas aeruginosa, and Staphylococcus aureus. We present as well information on the cryptic <span class="hlt">intrinsic</span> resistance genes that do not confer resistance to their native hosts but are capable of conferring resistance when their expression levels are increased and the activation of the cryptic genes. Finally, we discuss that <span class="hlt">intrinsic</span> genes could be the origin of acquired resistance, especially in the genus Acinetobacter.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/21474439','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/21474439"><span id="translatedtitle">THE COOL INTERSTELLAR MEDIUM IN <span class="hlt">ELLIPTICAL</span> GALAXIES. II. GAS CONTENT IN THE VOLUME-LIMITED SAMPLE AND RESULTS FROM THE COMBINED <span class="hlt">ELLIPTICAL</span> AND LENTICULAR SURVEYS</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Welch, Gary A.; Sage, Leslie J.; Young, Lisa M. E-mail: lsage@astro.umd.ed</p> <p>2010-12-10</p> <p>We report new observations of atomic and molecular gas in a volume-limited sample of <span class="hlt">elliptical</span> galaxies. Combining the <span class="hlt">elliptical</span> sample with an earlier and similar lenticular one, we show that cool gas detection rates are very similar among low-luminosity E and S0 galaxies but are much higher among luminous S0s. Using the combined sample we revisit the <span class="hlt">correlation</span> between cool gas mass and blue luminosity which emerged from our lenticular survey, finding strong support for previous claims that the molecular gas in <span class="hlt">ellipticals</span> and lenticulars has different origins. Unexpectedly, however, and contrary to earlier claims, the same is not true for atomic gas. We speculate that both the active galactic nucleus feedback and merger paradigms might offer explanations for differences in detection rates, and might also point toward an understanding of why the two gas phases could follow different evolutionary paths in Es and S0s. Finally, we present a new and puzzling discovery concerning the global mix of atomic and molecular gas in early-type galaxies. Atomic gas comprises a greater fraction of the cool interstellar medium in more gas-rich galaxies, a trend which can be plausibly explained. The puzzle is that galaxies tend to cluster around molecular-to-atomic gas mass ratios near either 0.05 or 0.5.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016NuPhB.907...77K','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016NuPhB.907...77K"><span id="translatedtitle">Thermodynamics of Inozemtsev's <span class="hlt">elliptic</span> spin chain</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Klabbers, Rob</p> <p>2016-06-01</p> <p>We study the thermodynamic behaviour of Inozemtsev's long-range <span class="hlt">elliptic</span> spin chain using the Bethe ansatz equations describing the spectrum of the model in the infinite-length limit. We classify all solutions of these equations in that limit and argue which of these solutions determine the spectrum in the thermodynamic limit. Interestingly, some of the solutions are not selfconjugate, which puts the model in sharp contrast to one of the model's limiting cases, the Heisenberg XXX spin chain. Invoking the string hypothesis we derive the thermodynamic Bethe ansatz equations (TBA-equations) from which we determine the Helmholtz free energy in thermodynamic equilibrium and derive the associated Y-system. We corroborate our results by comparing numerical solutions of the TBA-equations to a direct computation of the free energy for the finite-length hamiltonian. In addition we confirm numerically the interesting conjecture put forward by Finkel and González-López that the original and supersymmetric versions of Inozemtsev's <span class="hlt">elliptic</span> spin chain are equivalent in the thermodynamic limit.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2013PhRvL.110f5008D','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2013PhRvL.110f5008D"><span id="translatedtitle">Kinetic Stress and <span class="hlt">Intrinsic</span> Flow in a Toroidal Plasma</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Ding, W. X.; Lin, L.; Brower, D. L.; Almagri, A. F.; Chapman, B. E.; Fiksel, G.; Den Hartog, D. J.; Sarff, J. S.</p> <p>2013-02-01</p> <p>A new mechanism for <span class="hlt">intrinsic</span> plasma flow has been experimentally identified in a toroidal plasma. For reversed field pinch plasmas with a few percent β (ratio of plasma pressure to magnetic pressure), measurements show that parallel pressure fluctuations <span class="hlt">correlated</span> with magnetic fluctuations create a kinetic stress that can affect momentum balance and the evolution of <span class="hlt">intrinsic</span> plasma flow. This implies kinetic effects are important for flow generation and sustainment.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2009ApJ...693..617H','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2009ApJ...693..617H"><span id="translatedtitle">The <span class="hlt">Ellipticities</span> of Cluster Early-type Galaxies from z ~ 1 to z ~ 0: No Evolution in the Overall Distribution of Bulge-to-Disk Ratios</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Holden, B. P.; Franx, M.; Illingworth, G. D.; Postman, M.; van der Wel, A.; Kelson, D. D.; Blakeslee, J. P.; Ford, H.; Demarco, R.; Mei, S.</p> <p>2009-03-01</p> <p> <span class="hlt">ellipticity</span> at z>0.3, suggesting that rounder S0s are being assigned as <span class="hlt">ellipticals</span>. Taking the <span class="hlt">ellipticity</span> measurements and assuming, as in all previous studies, that the <span class="hlt">intrinsic</span> <span class="hlt">ellipticity</span> distribution of both <span class="hlt">elliptical</span> and S0 galaxies remains constant, then we conclude from the lack of evolution in the observed early-type <span class="hlt">ellipticity</span> distribution that the relative fractions of <span class="hlt">ellipticals</span> and S0s do not evolve from z ~ 1 to z = 0 for a red-sequence selected samples of galaxies in the cores of clusters of galaxies. Based on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract No. NAS5-26555. Some of the data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. This paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2001A%26A...379..767M','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2001A%26A...379..767M"><span id="translatedtitle">Energy, entropy and mass scaling relations for <span class="hlt">elliptical</span> galaxies. Towards a physical understanding of their photometric properties</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Márquez, I.; Lima Neto, G. B.; Capelato, H.; Durret, F.; Lanzoni, B.; Gerbal, D.</p> <p>2001-12-01</p> <p>In the present paper, we show that <span class="hlt">elliptical</span> galaxies (Es) obey a scaling relation between potential energy and mass. Since they are relaxed systems in a post violent-relaxation stage, they are quasi-equilibrium gravitational systems and therefore they also have a quasi-constant specific entropy. Assuming that light traces mass, these two laws imply that in the space defined by the three Sérsic law parameters (intensity Sigma0 , scale a and shape nu ), <span class="hlt">elliptical</span> galaxies are distributed on two intersecting 2-manifolds: the Entropic Surface and the Energy-Mass Surface. Using a sample of 132 galaxies belonging to three nearby clusters, we have verified that <span class="hlt">ellipticals</span> indeed follow these laws. This also implies that they are distributed along the intersection line (the Energy-Entropy line), thus they constitute a one-parameter family. These two physical laws (separately or combined), allow to find the theoretical origin of several observed photometrical relations, such as the <span class="hlt">correlation</span> between absolute magnitude and effective surface brightness, and the fact that <span class="hlt">ellipticals</span> are located on a surface in the [log Reff, -2.5 log Sigma0, log nu ] space. The fact that <span class="hlt">elliptical</span> galaxies are a one-parameter family has important implications for cosmology and galaxy formation and evolution models. Moreover, the Energy-Entropy line could be used as a distance indicator.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2005PMB....50.3197A','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2005PMB....50.3197A"><span id="translatedtitle">An investigation into the vector <span class="hlt">ellipticity</span> of extremely low frequency magnetic fields from appliances in UK homes</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Ainsbury, Elizabeth A.; Conein, Emma; Henshaw, Denis L.</p> <p>2005-07-01</p> <p><span class="hlt">Elliptically</span> polarized magnetic fields induce higher currents in the body compared with their plane polarized counterparts. This investigation examines the degree of vector <span class="hlt">ellipticity</span> of extremely low frequency magnetic fields (ELF-MFs) in the home, with regard to the adverse health effects reportedly associated with ELF-MFs, for instance childhood leukaemia. Tri-axial measurements of the magnitude and phase of the 0-3000 Hz magnetic fields, produced by 226 domestic mains-fed appliances of 32 different types, were carried out in 16 homes in Worcestershire in the summer of 2004. Magnetic field strengths were low, with average (RMS) values of 0.03 ± 0.02 µT across all residences. In contrast, background field <span class="hlt">ellipticities</span> were high, on average 47 ± 11%. Microwave and electric ovens produced the highest <span class="hlt">ellipticities</span>: mean respective values of 21 ± 21% and 21 ± 17% were observed 20 cm away from these appliances. There was a negative <span class="hlt">correlation</span> between field strength and field polarization, which we attribute to the higher relative field contribution close to each individual (single-phase) appliance. The measurements demonstrate that domestic magnetic fields are extremely complex and cannot simply be characterized by traditional measurements such as time-weighted average or peak exposure levels. We conclude that <span class="hlt">ellipticity</span> should become a relevant metric for future epidemiological studies of health and ELF-MF exposure. This work is supported by the charity CHILDREN with LEUKAEMIA, registered charity number 298405.</p> </li> </ol> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_8");'>8</a></li> <li><a href="#" onclick='return showDiv("page_9");'>9</a></li> <li class="active"><span>10</span></li> <li><a href="#" onclick='return showDiv("page_11");'>11</a></li> <li><a href="#" onclick='return showDiv("page_12");'>12</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div><!-- col-sm-12 --> </div><!-- row --> </div><!-- page_10 --> <div id="page_11" class="hiddenDiv"> <div class="row"> <div class="col-sm-12"> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_9");'>9</a></li> <li><a href="#" onclick='return showDiv("page_10");'>10</a></li> <li class="active"><span>11</span></li> <li><a href="#" onclick='return showDiv("page_12");'>12</a></li> <li><a href="#" onclick='return showDiv("page_13");'>13</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div> </div> <div class="row"> <div class="col-sm-12"> <ol class="result-class" start="201"> <li> <p><a target="_blank" onclick="trackOutboundLink('http://eric.ed.gov/?q=orbit&pg=2&id=EJ891960','ERIC'); return false;" href="http://eric.ed.gov/?q=orbit&pg=2&id=EJ891960"><span id="translatedtitle"><span class="hlt">Elliptical</span> Orbit [arrow right] 1/r[superscript 2] Force</span></a></p> <p><a target="_blank" href="http://www.eric.ed.gov/ERICWebPortal/search/extended.jsp?_pageLabel=advanced">ERIC Educational Resources Information Center</a></p> <p>Prentis, Jeffrey; Fulton, Bryan; Hesse, Carol; Mazzino, Laura</p> <p>2007-01-01</p> <p>Newton's proof of the connection between <span class="hlt">elliptical</span> orbits and inverse-square forces ranks among the "top ten" calculations in the history of science. This time-honored calculation is a highlight in an upper-level mechanics course. It would be worthwhile if students in introductory physics could prove the relation "<span class="hlt">elliptical</span> orbit" [arrow right]…</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016JPhCS.668a2103G','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016JPhCS.668a2103G"><span id="translatedtitle">Prospects of <span class="hlt">Elliptic</span> Flow Studies at NICA/MPD</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Geraksiev, Nikolay</p> <p>2016-01-01</p> <p>As a key observable, anisotropic flow presents a unique insight into heavy ion collision physics. The presented poster reveals the prospects of studying <span class="hlt">elliptic</span> flow at the NICA/MPD facility through the UrQMD model. Here, results for the <span class="hlt">elliptic</span> flow of simulated and reconstructed hadrons at the planned NICA energy range are presented.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/21212898','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/21212898"><span id="translatedtitle">Effects of confining walls on heat transfer from a vertical array of isothermal horizontal <span class="hlt">elliptic</span> cylinders</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Yousefi, T.; Paknezhad, M.; Ashjaee, M.; Yazdani, S.</p> <p>2009-09-15</p> <p>Steady state two-dimensional natural convection heat transfer from the vertical array of five horizontal isothermal <span class="hlt">elliptic</span> cylinders with vertical major axis which confined between two adiabatic walls has been studied experimentally. Experiments were carried out using a Mach-Zehnder interferometer. The Rayleigh number based on cylinder major axis was in the range 10{sup 3}{<=}Ra{<=}2.5 x 10{sup 3}, and dimensionless wall spacing 1.5{<=} t/b{<=}9 and infinity. The effect of wall spacing and Rayleigh number on the heat transfer from the individual cylinder and the array were investigated. Experiments are performed for ratio wall spacing to major diameter t/b = 1.5, 2, 2.5, 3, 3.5, 4, 5, 6, 7, 8, 9 and infinity. A <span class="hlt">correlation</span> based on the experimental data for the average Nusselt number of the array as a function of Ra and t/b is presented in the aforementioned ranges. A relation has been derived for optimum wall spacing at which the Nusselt number of the array attains its maximum value. At optimum wall spacing, approximately 10% increase in the heat transfer from the confined array of <span class="hlt">elliptic</span> cylinders has been observed as compared to the unconfined case. Also, a heat transfer <span class="hlt">correlation</span> has been proposed for a single <span class="hlt">elliptic</span> cylinder with vertical major axis and has been compared with earlier works. (author)</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016AIPA....6f5026M','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016AIPA....6f5026M"><span id="translatedtitle">Dynamic susceptibility of onion in ferromagnetic <span class="hlt">elliptical</span> nanoring</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Mu, Congpu; Song, Jiefang; Xu, Jianghong; Wen, Fusheng</p> <p>2016-06-01</p> <p>Micromagnetic simulation was performed to investigate the equilibrium state and dynamic susceptibility spectra of magnetic <span class="hlt">elliptical</span> nanoring. There are two equilibrium states (onion and vortex) obtained in <span class="hlt">elliptical</span> nanoring. The onion state can be used to record information in MRAM. And it is important to investigate the dynamic susceptibility spectra of onion state, which is closely related to writing and reading speed of magnetic memory devices. Those results show that two or three resonance peaks are found under different thickness of <span class="hlt">elliptical</span> nanoring with onion state, respectively. The low resonance frequency of two resonance peaks is increasing with the arm width of the <span class="hlt">elliptical</span> ring, but is decreasing with the thickness. However, the high frequency of two resonance peaks is decreasing with the arm width of the <span class="hlt">elliptical</span> ring.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19950015346','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19950015346"><span id="translatedtitle">Far-infrared mapping of dusty <span class="hlt">elliptical</span> galaxies</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Lees, Joanna F.; Harper, D. A.; Rupen, Michael P.; Knapp, G. R.</p> <p>1994-01-01</p> <p>Preliminary results from a program to map the thermal far-infrared emission from cool dust in <span class="hlt">elliptical</span> galaxies using the Yerkes 60-Channel Camera on the Kuiper Airborne Observatory (KAO) are presented. The 160 micron emission from the <span class="hlt">elliptical</span> NGC 6542 is apparently extended over the optical galaxy whereas the 100 micron emission is unresolved. This implies a dust temperature gradient consistent with that expected for dust with Galactic properties exposed to the general interstellar radiation field of the <span class="hlt">elliptical</span> galaxy. Observations of the <span class="hlt">elliptical</span> NGC 5666 and the NGC 7463/4/5 compact group (consisting of the <span class="hlt">elliptical</span> NGC 7464, the S0 NGC 7465, and the spiral NGC 7463) are also discussed.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2010APS..DFD.GB001G','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2010APS..DFD.GB001G"><span id="translatedtitle">Modeling roughness effects in turbulent boundary layers using <span class="hlt">elliptic</span> relaxation</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>George, Jacob; de Simone, Alejandro; Iaccarino, Gianluca; Jimenez, Javier</p> <p>2010-11-01</p> <p>We present results from the efforts towards modeling roughness in turbulent boundary layers using <span class="hlt">elliptic</span> relaxation. This scheme, included in the v^2-f model and first formulated by Durbin (1993, JFM, vol. 249, p.465) for smooth-walls, uses an <span class="hlt">elliptic</span> partial differential equation to incorporate near-wall turbulence anisotropy and non-local pressure-strain effects. The use of the <span class="hlt">elliptic</span> PDE is extended to model roughness effects in various transitionally-rough and fully-rough boundary layers consisting of a uniform and sparse distribution of cylinders for which experimental data is available. The roughness effects are incorporated through the <span class="hlt">elliptic</span> PDE by including the length and time scales that the roughness imposes upon the flow, which the experiment has shown to be constant within the rough-walls. Further modeling of roughness effects is considered by altering the source terms in the <span class="hlt">elliptic</span> PDE.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/24453871','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/24453871"><span id="translatedtitle">Cotton-type and joint invariants for linear <span class="hlt">elliptic</span> systems.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Aslam, A; Mahomed, F M</p> <p>2013-01-01</p> <p>Cotton-type invariants for a subclass of a system of two linear <span class="hlt">elliptic</span> equations, obtainable from a complex base linear <span class="hlt">elliptic</span> equation, are derived both by spliting of the corresponding complex Cotton invariants of the base complex equation and from the Laplace-type invariants of the system of linear hyperbolic equations equivalent to the system of linear <span class="hlt">elliptic</span> equations via linear complex transformations of the independent variables. It is shown that Cotton-type invariants derived from these two approaches are identical. Furthermore, Cotton-type and joint invariants for a general system of two linear <span class="hlt">elliptic</span> equations are also obtained from the Laplace-type and joint invariants for a system of two linear hyperbolic equations equivalent to the system of linear <span class="hlt">elliptic</span> equations by complex changes of the independent variables. Examples are presented to illustrate the results.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017EPJWC.13708008H','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017EPJWC.13708008H"><span id="translatedtitle">Recent progress on <span class="hlt">intrinsic</span> charm</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Hobbs, T. J.</p> <p>2017-03-01</p> <p>Over the past ˜10 years, the topic of the nucleon's nonperturbative or <span class="hlt">intrinsic</span> charm (IC) content has enjoyed something of a renaissance, largely motivated by theoretical developments involving quark modelers and PDF-fitters. In this talk I will briefly describe the importance of <span class="hlt">intrinsic</span> charm to various issues in high-energy phenomenology, and survey recent progress in constraining its overall normalization and contribution to the momentum sum rule of the nucleon. I end with the conclusion that progress on the side of calculation has now placed the onus on experiment to unambiguously resolve the proton's <span class="hlt">intrinsic</span> charm component.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2000PhFl...12.2345M','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2000PhFl...12.2345M"><span id="translatedtitle">A new form of the <span class="hlt">elliptic</span> relaxation equation to account for wall effects in RANS modeling</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Manceau, Rémi; Hanjalić, Kemal</p> <p>2000-09-01</p> <p>Different methods for improving the behavior in the logarithmic layer of the <span class="hlt">elliptic</span> relaxation equation, which enable the extension of Reynolds stress models or eddy viscosity models down to the wall, are tested in a channel flow at Reτ=590 and compared with direct numerical simulation (DNS) data. First, a priori tests are performed in order to confirm the improvement predicted by the theory, either with the Rotta+IP (isotropization of production) model or the Speziale-Sarkar-Gatski (SSG) model as the source term of the <span class="hlt">elliptic</span> relaxation equation. The best form of the model is then used for full simulations, in Durbin second moment closure or in the frame of the v2¯-f model. It is shown that the results can be significantly improved, in particular by using a formulation based on the refinement of the modeling of the two-point <span class="hlt">correlations</span> involved in the redistribution term.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/22016124','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/22016124"><span id="translatedtitle">TESTING YUKAWA-LIKE POTENTIALS FROM f(R)-GRAVITY IN <span class="hlt">ELLIPTICAL</span> GALAXIES</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Napolitano, N. R.; Capozziello, S.; Capaccioli, M.; Romanowsky, A. J.</p> <p>2012-04-01</p> <p>We present the first analysis of extended stellar kinematics of <span class="hlt">elliptical</span> galaxies where a Yukawa-like correction to the Newtonian gravitational potential derived from f(R)-gravity is considered as an alternative to dark matter. In this framework, we model long-slit data and planetary nebula data out to 7 R{sub eff} of three galaxies with either decreasing or flat dispersion profiles. We use the corrected Newtonian potential in a dispersion-kurtosis Jeans analysis to account for the mass-anisotropy degeneracy. We find that these modified potentials are able to fit nicely all three <span class="hlt">elliptical</span> galaxies and the anisotropy distribution is consistent with that estimated if a dark halo is considered. The parameter which measures the 'strength' of the Yukawa-like correction is, on average, smaller than the one found previously in spiral galaxies and <span class="hlt">correlates</span> both with the scale length of the Yukawa-like term and the orbital anisotropy.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2004PhFl...16..853F','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2004PhFl...16..853F"><span id="translatedtitle">Craik-Criminale solutions and <span class="hlt">elliptic</span> instability in nonlinear-reactive closure models for turbulence</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Fabijonas, Bruce R.; Holm, Darryl D.</p> <p>2004-04-01</p> <p>The Craik-Criminale class of exact solutions is examined for a nonlinear-reactive fluids theory that includes a family of turbulence closure models. These may be formally regarded as either large eddy simulation or Reynolds-averaged Navier-Stokes models of turbulence. All of the turbulence closure models in the class under investigation preserve the existence of <span class="hlt">elliptic</span> instability, although they shift its angle of critical stability as a function of the rotation rate Ω of the coordinate system, the wave number β of the Kelvin wave, and the model parameter α, the turbulence <span class="hlt">correlation</span> length. <span class="hlt">Elliptic</span> instability allows a comparison among the properties of these models. It is emphasized that the physical mechanism for this instability is not wave-wave interaction, but rather wave, mean-flow interaction as governed by the choice of a model's nonlinearity.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016APS..DFDG34009K','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016APS..DFDG34009K"><span id="translatedtitle">Analytical study on the SGS force around an <span class="hlt">elliptic</span> Burgers vortex</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Kobayashi, Hiromichi</p> <p>2016-11-01</p> <p>The subgrid-scale (SGS) force around an <span class="hlt">elliptic</span> Burgers vortex is analytically examined. In turbulence, there are a lot of vortex-tubes whose cross sections are known to be approximated as the ellipse. In this study, the biaxial <span class="hlt">elliptic</span> Burgers vortex is produced by adding the compressive and extensional background straining flow to the conventional Burgers vortex. By using a filtering operation, we revealed that the energy transfer by the Reynolds stress term applying the Bardina model exhibits negative <span class="hlt">correlation</span> to that by the true SGS stress term. However, it has been recently reported that a combination of the Bardina Reynolds term and the eddy viscosity model gives good performance even for the coarse LES of turbulent channel flows. In order to understand that, we discuss some SGS forces: by the true SGS stress tensor, by the eddy viscosity model, by the modified Leonard term and by the Bardina Reynolds term. This work was supported by JSPS KAKENHI Grant Number 26420122.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016MsT..........1U','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016MsT..........1U"><span id="translatedtitle">Investigating the Density of Isolated Field <span class="hlt">Elliptical</span> Galaxies</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Ulgen, E. Kaan</p> <p>2016-02-01</p> <p>In this thesis, 215.590 <span class="hlt">elliptical</span> galaxies with M(r) ≤ -21 in the CFHTLS-W1 field which is covering 72 sq. deg on the sky are examined . Criterion given by Smith et al. (2004) has been used to determine isolated <span class="hlt">elliptical</span> galaxies. 118 isolated <span class="hlt">elliptical</span> galaxies have been determined in total. By using g, r and i photometric bands, the true-colour images of candidates are produced and visually inspected. In order to have a clean list of IfEs some candidates are excluded from the final sample after visual inspection. The final sample consists of 60 IfEs which corresponds to the 0.027 per cent of the whole sample. In other words, IfE density in the W1 is 0.8 IfE / sq.deg. Since the formation of the <span class="hlt">ellipticals</span> in the isolated regions is not known clearly, it is crucial to determine IfEs and compare their photometric and morphological properties to the normal or cluster <span class="hlt">ellipticals</span>. When the (g-i) distributions of three different <span class="hlt">elliptical</span> galaxy class are compared, it is found that they have almost the same colours. When the redshift distributions of the galaxies are considered, it can be seen that IfEs formed later than the cluster and normal <span class="hlt">ellipticals</span>. The average redshift of IfEs is determined as zphot=0.284, while for normal and cluster <span class="hlt">ellipticals</span>, it is, respectively, 0.410 and 0.732. In addition, when the effective radii of the three <span class="hlt">elliptical</span> systems are considered, it is found that the IfEs are bigger than the other two <span class="hlt">elliptical</span> classes.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=20110007181&hterms=halo&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D20%26Ntt%3Dhalo','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=20110007181&hterms=halo&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D20%26Ntt%3Dhalo"><span id="translatedtitle">Subregions of Motion and <span class="hlt">Elliptic</span> Halo Orbits in the <span class="hlt">Elliptic</span> Restricted Three-Body Problem</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Campagnola, Stefano; Lo, Martin; Newton, Paul</p> <p>2008-01-01</p> <p>In this paper we present regions of motion and periodic orbits in the spatial <span class="hlt">elliptic</span> restricted three body problem (ER3BP). Periodic orbits and regions of motion are fundamental keys to understand any dynamical system; for this reason the Hill's surfaces or the families of halo orbits have been extensively studied in the frame of the circular restricted three body problem. It is our opinion that their natural extensions to the ER3BP have not been studied enough. We divide the position space into forbidden subregions, subregions of motion and low-velocity subregions.We use these notions to define necessary condition for a transfer trajectory in the ER3BP. Also we compute branches of <span class="hlt">elliptic</span> halo orbits bifurcating from halo orbits in the circular restricted three body problem. The new periodic orbits have principal periods and stability properties different from those of the originating halo orbit.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19890014548','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19890014548"><span id="translatedtitle">Crack-face displacements for embedded <span class="hlt">elliptic</span> and semi-<span class="hlt">elliptical</span> surface cracks</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Raju, I. S.</p> <p>1989-01-01</p> <p>Analytical expressions for the crack-face displacements of an embedded <span class="hlt">elliptic</span> crack in infinite solid subjected to arbitrary tractions are obtained. The tractions on the crack faces are assumed to be expressed in a polynomial form. These displacements expressions complete the exact solution of Vijayakumar and Atluri, and Nishioki and Atluri. For the special case of an embedded crack in an infinite solid subjected to uniform pressure loading, the present displacements agree with those by Green and Sneddon. The displacement equations derived were used with the finite-element alternating method (FEAM) for the analysis of a semi-<span class="hlt">elliptic</span> surface crack in a finite solid subjected to remote tensile loading. The maximum opening displacements obtained with FEAM are compared to those with the finite-element method with singularity elements. The maximum crack opening displacements by the two methods showed good agreement.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://www.osti.gov/scitech/servlets/purl/1327268','SCIGOV-STC'); return false;" href="http://www.osti.gov/scitech/servlets/purl/1327268"><span id="translatedtitle"><span class="hlt">Elliptical</span> Muon Helical Cooling Channel Coils</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Kahn, S. A.; Flanagan, G.; Lopes, M. L.; Yonehara, K.</p> <p>2013-09-01</p> <p>A helical cooling channel (HCC) consisting of a pressurized gas absorber imbedded in a magnetic channel that provides solenoid, helical dipole and helical quadrupole fields has shown considerable promise in providing six-dimensional phase space reduction for muon beams. The most effective approach to implementing the desired magnetic field is a helical solenoid (HS) channel composed of short solenoid coils arranged in a helical pattern. The HS channel along with an external solenoid allows the B$_z$ and B$_{\\phi}$ components along the reference orbit to be set to any desired values. To set dB$_{\\phi}$/dr to the desired value for optimum focusing requires an additional variable to tune. We shall show that using <span class="hlt">elliptical</span> shaped coils in the HS channel allows the flexibility to achieve the desired dB$_{\\phi}$/dr on the reference orbit without significant change to B$_z$ and B$_{\\phi}$.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19970020569&hterms=loudspeaker&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D20%26Ntt%3Dloudspeaker','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19970020569&hterms=loudspeaker&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D20%26Ntt%3Dloudspeaker"><span id="translatedtitle">Splitting of Forced <span class="hlt">Elliptic</span> Jets and Flames</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Hertzberg, J.; Carlton, J.; Schwieterman, M.; Davis, E.; Bradley, E.; Linne, M.</p> <p>1997-01-01</p> <p>The objective of this work is to understand the fluid dynamics in the interaction of large scale, three-dimensional vortex structures and transitional diffusion flames in a microgravity environment. The vortex structures are used to provide a known perturbation of the type used in passive and active shear layer control techniques. 'Passive techniques' refers to manipulation of the system geometry to influence the three dimensional dynamics of vortex structures, and 'active' refers to any technique which adds energy (acoustic or kinetic) to the flow to influence the shear layer vortex dynamics. In this work the passive forcing is provided by an <span class="hlt">elliptic</span> jet cross-section, and the active forcing is incorporated by perturbing the jet velocity using a loudspeaker in the plenum section.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19870060839&hterms=magnetic+resonance&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D40%26Ntt%3Dmagnetic%2Bresonance','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19870060839&hterms=magnetic+resonance&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D40%26Ntt%3Dmagnetic%2Bresonance"><span id="translatedtitle">Magnetic <span class="hlt">elliptical</span> polarization of Schumann resonances</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Sentman, D. D.</p> <p>1987-01-01</p> <p>Measurements of orthogonal, horizontal components of the magnetic field in the ELF range obtained during September 1985 show that the Schumann resonance eigenfrequencies determined separately for the north-south and east-west magnetic components differ by as much as 0.5 Hz, suggesting that the underlying magnetic signal is not linearly polarized at such times. The high degree of magnetic <span class="hlt">ellipticity</span> found suggests that the side multiplets of the Schumann resonances corresponding to azimuthally inhomogeneous normal modes are strongly excited in the highly asymmetric earth-ionosphere cavity. The dominant sense of polarization over the measurement passband is found to be right-handed during local daylight hours, and to be left-handed during local nighttime hours.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2015PhRvD..91d4016H','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2015PhRvD..91d4016H"><span id="translatedtitle">Horizon complementarity in <span class="hlt">elliptic</span> de Sitter space</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Hackl, Lucas; Neiman, Yasha</p> <p>2015-02-01</p> <p>We study a quantum field in <span class="hlt">elliptic</span> de Sitter space dS4/Z2—the spacetime obtained from identifying antipodal points in dS4. We find that the operator algebra and Hilbert space cannot be defined for the entire space, but only for observable causal patches. This makes the system into an explicit realization of the horizon complementarity principle. In the absence of a global quantum theory, we propose a recipe for translating operators and states between observers. This translation involves information loss, in accordance with the fact that two observers see different patches of the spacetime. As a check, we recover the thermal state at the de Sitter temperature as a state that appears the same to all observers. This thermal state arises from the same functional that, in ordinary dS4, describes the Bunch-Davies vacuum.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19830021439','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19830021439"><span id="translatedtitle">Theoretical results for starved <span class="hlt">elliptical</span> contacts</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Hamrock, B. J.; Dowson, D.</p> <p>1983-01-01</p> <p>Eighteen cases were used in the theoretical study of the influence of lubricant starvation on film thickness and pressure in <span class="hlt">elliptical</span> elastohydrodynamic conjunctions. From the results a simple and important critical dimensionless inlet boundary distance at which lubricant starvation becomes significant was specified. This inlet boundary distance defines whether a fully flooded or a starved condition exists in the contact. Furthermore, it was found that the film thickness for a starved condition is written in dimensionless terms as a function of the inlet distance parameter and the film thickness for a fully flooded condition. Contour plots of pressure and film thickness in and around the contact are shown for fully flooded and starved conditions.</p> </li> </ol> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_9");'>9</a></li> <li><a href="#" onclick='return showDiv("page_10");'>10</a></li> <li class="active"><span>11</span></li> <li><a href="#" onclick='return showDiv("page_12");'>12</a></li> <li><a href="#" onclick='return showDiv("page_13");'>13</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div><!-- col-sm-12 --> </div><!-- row --> </div><!-- page_11 --> <div id="page_12" class="hiddenDiv"> <div class="row"> <div class="col-sm-12"> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_10");'>10</a></li> <li><a href="#" onclick='return showDiv("page_11");'>11</a></li> <li class="active"><span>12</span></li> <li><a href="#" onclick='return showDiv("page_13");'>13</a></li> <li><a href="#" onclick='return showDiv("page_14");'>14</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div> </div> <div class="row"> <div class="col-sm-12"> <ol class="result-class" start="221"> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2006IJTFM.126..937W','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2006IJTFM.126..937W"><span id="translatedtitle">Applications of <span class="hlt">Elliptic</span> Integral and <span class="hlt">Elliptic</span> Function to Electric Power Cable Problems</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Watanabe, Kazuo</p> <p></p> <p>The paper proposes an application of <span class="hlt">elliptic</span> function to a new measuring method of electric resistivity of outer-semiconductive layer of XLPE cable. The new measuring method may substitute the conventional method. The resistivity can be obtained easily by measuring resistance between two electrodes which are attached to a circumferential edge on one side of the outer-semiconductive layer of a cable core sample. The solution process is applicable to heat conduction as well as hydromechanics.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/23482023','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/23482023"><span id="translatedtitle">Quantum-orbit analysis for yield and <span class="hlt">ellipticity</span> of high order harmonic generation with <span class="hlt">elliptically</span> polarized laser field.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Li, Yang; Zhu, Xiaosong; Zhang, Qingbin; Qin, Meiyan; Lu, Peixiang</p> <p>2013-02-25</p> <p>We perform a quantum-orbit analysis for the dependence of high-order-harmonic yield on the driving field <span class="hlt">ellipticity</span> and the polarization properties of the generated high harmonics. The electron trajectories responsible for the emission of particular harmonics are identified. It is found that, in <span class="hlt">elliptically</span> polarized driving field, the electrons have <span class="hlt">ellipticity</span>-dependent initial velocities, which lead to the decrease of the ionization rate. Thus the harmonic yield steeply decreases with laser <span class="hlt">ellipticity</span>. Besides, we show that the polarization properties of the harmonics are related to the complex momenta of the electron. The physical origin of the harmonic <span class="hlt">ellipticity</span> is interpreted as the consequence of quantum-mechanical uncertainty of the electron momentum. Our results are verified with the experimental results as well as the numerical solutions of the time dependent Schrödinger equation from the literature.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/21052536','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/21052536"><span id="translatedtitle"><span class="hlt">Elliptical</span> Undulators HU256 for Synchrotron SOLEIL</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Batrakov, A.; Churkin, I.; Ilyin, I.; Kolokolnikov, Yu.; Rouvinski, E.; Semenov, E.; Steshov, A.; Vobly, P.; Briquez, F.; Chubar, O.; Dael, A.; Marcouile, O.; Marteau, F.; Roux, G.; Valleau, M.</p> <p>2007-01-19</p> <p>Three <span class="hlt">elliptical</span> undulators HU256 of electromagnetic type were produced, tested and magnetically measured by the Budker Institute of Nuclear Physics (Russia) for Synchrotron Soleil (France). The undulators have a new design of a Bx and Bz closed structure for insertion vacuum chamber. In the <span class="hlt">elliptical</span> undulator HU256 with period of the magnetic fields of 256 mm, the vertical magnetic field (Bzmax=0.44 T) formed by 27 Bz laminated dipole magnets is symmetric, and the horizontal magnetic field (Bxmax=0.33 T) formed by 28 Bx laminated dipole magnets is asymmetric. The undulator can work in standard mode as well as in a quasi-periodical mode. The vertical magnetic field may be modulated by switching on the modulation coils placed on the Bz dipoles. Two power supply systems allow us to modulate the horizontal magnetic field, and change the radiation spectrum. The magnetic calculations of the individual dipoles and dipoles in ''undulator'' environment were executed by means of Mermaid 3D Code. The magnetic measurements of the individual dipoles had confirmed the magnetic calculations. On basis of semiempirical dependences from the mechanical characteristics the estimates of the magnetic parameters for all dipoles were calculated. Sorting of dipoles in the undulators have been done, and it has improved the magnetic parameters of the assembled undulators in comparison with the statistical estimations. The magnetic measurements of the undulators HU256 were carried out at Budker INP by Hall probes and at Soleil by Hall probes and Stretched Wire. Now the 1st undulator HU256 is installed at Soleil Storage Ring.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2004AAS...205.9201B','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2004AAS...205.9201B"><span id="translatedtitle"><span class="hlt">Ellipticals</span>: core-Sérsic vs Nuker</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Bartlett, D. F.</p> <p>2004-12-01</p> <p>HST has given the first look at <span class="hlt">elliptical</span> galaxies on scales <1". Lauer et al (1995) used the Wide Field Planetary Camera (WFPC -1) to map the intensity of light I(r) in the inner 10" of 45 type E and S0 galaxies. They discovered that about 40% of the 39 <span class="hlt">ellipticals</span> could not be described by a single power law. These galaxies have a core region where the power law I ∝ r-γ is less steep than the outer region I ∝ r-β . The resulting Nuker law allows for a smooth transition between these regions at a break radius rb. The physical rb varies widely: 30 pc < rb < 1200 pc. Rest et al (2001) used WFPC -2 to confirm the original WFPC -1 results with additional galaxies. Using the full WFPC -2 mosaic, Trujillo, Erwin, Ramos, and Graham (2004) have extended the angular range of Rest et al by a factor between 3 and 8. They find that the extended outer region is incompatible with a Nuker law. Rather the power law for the outer region must be replaced by the Sérsic law, I(r) ∝ e-bn r1/n. They also find that the break radius is generally much reduced. Their published study of 9 core-Sérsic galaxies has 20 pc< rb <150 pc. The new range of rb fits well within 1 wavelength λ of the non-Newtonian sinusoidal gravity. Here the potential of a point mass is GM cos(2 π r/λ )/r and λ =425 pc. (Bartlett 2001, 2004). With this gravity, the potential towards the center of any spherical mass distribution varies as ± sin(2 π r/λ )/r. I identify the + sign with the core-Sérsic galaxies and the - sign with the pure Sérsic galaxies. I will relate Sérsic's n to cosmological time t.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017PhRvC..95c4910A','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017PhRvC..95c4910A"><span id="translatedtitle">Measurement of long-range angular <span class="hlt">correlations</span> and azimuthal anisotropies in high-multiplicity p +Au collisions at √{sNN}=200 GeV</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Aidala, C.; Akiba, Y.; Alfred, M.; Andrieux, V.; Aoki, K.; Apadula, N.; Asano, H.; Ayuso, C.; Azmoun, B.; Babintsev, V.; Bandara, N. S.; Barish, K. N.; Bathe, S.; Bazilevsky, A.; Beaumier, M.; Belmont, R.; Berdnikov, A.; Berdnikov, Y.; Blau, D. S.; Boer, M.; Bok, J. S.; Brooks, M. L.; Bryslawskyj, J.; Bumazhnov, V.; Butler, C.; Campbell, S.; Canoa Roman, V.; Cervantes, R.; Chi, C. Y.; Chiu, M.; Choi, I. J.; Choi, J. B.; Citron, Z.; Connors, M.; Cronin, N.; Csanád, M.; Csörgő, T.; Danley, T. W.; Daugherity, M. S.; David, G.; Deblasio, K.; Dehmelt, K.; Denisov, A.; Deshpande, A.; Desmond, E. J.; Dion, A.; Dixit, D.; Do, J. H.; Drees, A.; Drees, K. A.; Dumancic, M.; Durham, J. M.; Durum, A.; Elder, T.; Enokizono, A.; En'yo, H.; Esumi, S.; Fadem, B.; Fan, W.; Feege, N.; Fields, D. E.; Finger, M.; Finger, M.; Fokin, S. L.; Frantz, J. E.; Franz, A.; Frawley, A. D.; Fukuda, Y.; Gal, C.; Gallus, P.; Garg, P.; Ge, H.; Giordano, F.; Goto, Y.; Grau, N.; Greene, S. V.; Grosse Perdekamp, M.; Gunji, T.; Guragain, H.; Hachiya, T.; Haggerty, J. S.; Hahn, K. I.; Hamagaki, H.; Hamilton, H. F.; Han, S. Y.; Hanks, J.; Hasegawa, S.; Haseler, T. O. S.; He, X.; Hemmick, T. K.; Hill, J. C.; Hill, K.; Hollis, R. S.; Homma, K.; Hong, B.; Hoshino, T.; Hotvedt, N.; Huang, J.; Huang, S.; Imai, K.; Imrek, J.; Inaba, M.; Iordanova, A.; Isenhower, D.; Ito, Y.; Ivanishchev, D.; Jacak, B. V.; Jezghani, M.; Ji, Z.; Jiang, X.; Johnson, B. M.; Jorjadze, V.; Jouan, D.; Jumper, D. S.; Kang, J. H.; Kapukchyan, D.; Karthas, S.; Kawall, D.; Kazantsev, A. V.; Khachatryan, V.; Khanzadeev, A.; Kim, C.; Kim, D. J.; Kim, E.-J.; Kim, M. H.; Kim, M.; Kincses, D.; Kistenev, E.; Klatsky, J.; Kline, P.; Koblesky, T.; Kotov, D.; Kudo, S.; Kurita, K.; Kwon, Y.; Lajoie, J. G.; Lallow, E. O.; Lebedev, A.; Lee, S.; Leitch, M. J.; Leung, Y. H.; Lewis, N. A.; Li, X.; Lim, S. H.; Liu, L. D.; Liu, M. X.; Loggins, V.-R.; Loggins, V.-R.; Lovasz, K.; Lynch, D.; Majoros, T.; Makdisi, Y. I.; Makek, M.; Malaev, M.; Manko, V. I.; Mannel, E.; Masuda, H.; McCumber, M.; McGaughey, P. L.; McGlinchey, D.; McKinney, C.; Mendoza, M.; Mignerey, A. C.; Mihalik, D. E.; Milov, A.; Mishra, D. K.; Mitchell, J. T.; Mitsuka, G.; Miyasaka, S.; Mizuno, S.; Montuenga, P.; Moon, T.; Morrison, D. P.; Morrow, S. I. M.; Murakami, T.; Murata, J.; Nagai, K.; Nagashima, K.; Nagashima, T.; Nagle, J. L.; Nagy, M. I.; Nakagawa, I.; Nakagomi, H.; Nakano, K.; Nattrass, C.; Niida, T.; Nouicer, R.; Novák, T.; Novitzky, N.; Novotny, R.; Nyanin, A. S.; O'Brien, E.; Ogilvie, C. A.; Orjuela Koop, J. D.; Osborn, J. D.; Oskarsson, A.; Ottino, G. J.; Ozawa, K.; Pantuev, V.; Papavassiliou, V.; Park, J. S.; Park, S.; Pate, S. F.; Patel, M.; Peng, W.; Perepelitsa, D. V.; Perera, G. D. N.; Peressounko, D. Yu.; Perezlara, C. E.; Perry, J.; Petti, R.; Phipps, M.; Pinkenburg, C.; Pisani, R. P.; Pun, A.; Purschke, M. L.; Read, K. F.; Reynolds, D.; Riabov, V.; Riabov, Y.; Richford, D.; Rinn, T.; Rolnick, S. D.; Rosati, M.; Rowan, Z.; Runchey, J.; Safonov, A. S.; Sakaguchi, T.; Sako, H.; Samsonov, V.; Sarsour, M.; Sato, K.; Sato, S.; Schaefer, B.; Schmoll, B. K.; Sedgwick, K.; Seidl, R.; Sen, A.; Seto, R.; Sexton, A.; Sharma, D.; Shein, I.; Shibata, T.-A.; Shigaki, K.; Shimomura, M.; Shioya, T.; Shukla, P.; Sickles, A.; Silva, C. L.; Silvermyr, D.; Singh, B. K.; Singh, C. P.; Singh, V.; Slunečka, M.; Smith, K. L.; Snowball, M.; Soltz, R. A.; Sondheim, W. E.; Sorensen, S. P.; Sourikova, I. V.; Stankus, P. W.; Stoll, S. P.; Sugitate, T.; Sukhanov, A.; Sumita, T.; Sun, J.; Syed, S.; Sziklai, J.; Takeda, A.; Tanida, K.; Tannenbaum, M. J.; Tarafdar, S.; Tarnai, G.; Tieulent, R.; Timilsina, A.; Todoroki, T.; Tomášek, M.; Towell, C. L.; Towell, R. S.; Tserruya, I.; Ueda, Y.; Ujvari, B.; van Hecke, H. W.; Vazquez-Carson, S.; Velkovska, J.; Virius, M.; Vrba, V.; Vukman, N.; Wang, X. R.; Wang, Z.; Watanabe, Y.; Watanabe, Y. S.; Wong, C. P.; Woody, C. L.; Xu, C.; Xu, Q.; Xue, L.; Yalcin, S.; Yamaguchi, Y. L.; Yamamoto, H.; Yanovich, A.; Yin, P.; Yoo, J. H.; Yoon, I.; Yu, H.; Yushmanov, I. E.; Zajc, W. A.; Zelenski, A.; Zharko, S.; Zou, L.; Phenix Collaboration</p> <p>2017-03-01</p> <p>We present measurements of long-range angular <span class="hlt">correlations</span> and the transverse momentum dependence of <span class="hlt">elliptic</span> flow v2 in high-multiplicity p +Au collisions at √{s NN}=200 GeV. A comparison of these results to previous measurements in high-multiplicity d +Au and 3He+Au collisions demonstrates a relation between v2 and the initial collision eccentricity ɛ2, suggesting that the observed momentum-space azimuthal anisotropies in these small systems have a collective origin and reflect the initial geometry. Good agreement is observed between the measured v2 and hydrodynamic calculations for all systems, and an argument disfavoring theoretical explanations based on initial momentum-space domain <span class="hlt">correlations</span> is presented. The set of measurements presented here allows us to leverage the distinct <span class="hlt">intrinsic</span> geometry of each of these systems to distinguish between different theoretical descriptions of the long-range <span class="hlt">correlations</span> observed in small collision systems.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016PhRvB..93j4408T','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016PhRvB..93j4408T"><span id="translatedtitle"><span class="hlt">Intrinsic</span> magnetization of antiferromagnetic textures</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Tveten, Erlend G.; Müller, Tristan; Linder, Jacob; Brataas, Arne</p> <p>2016-03-01</p> <p>Antiferromagnets (AFMs) exhibit <span class="hlt">intrinsic</span> magnetization when the order parameter spatially varies. This <span class="hlt">intrinsic</span> spin is present even at equilibrium and can be interpreted as a twisting of the homogeneous AFM into a state with a finite spin. Because magnetic moments couple directly to external magnetic fields, the <span class="hlt">intrinsic</span> magnetization can alter the dynamics of antiferromagnetic textures under such influence. Starting from the discrete Heisenberg model, we derive the continuum limit of the free energy of AFMs in the exchange approximation and explicitly rederive that the spatial variation of the antiferromagnetic order parameter is associated with an <span class="hlt">intrinsic</span> magnetization density. We calculate the magnetization profile of a domain wall and discuss how the <span class="hlt">intrinsic</span> magnetization reacts to external forces. We show conclusively, both analytically and numerically, that a spatially inhomogeneous magnetic field can move and control the position of domain walls in AFMs. By comparing our model to a commonly used alternative parametrization procedure for the continuum fields, we show that the physical interpretations of these fields depend critically on the choice of parametrization procedure for the discrete-to-continuous transition. This can explain why a significant amount of recent studies of the dynamics of AFMs, including effective models that describe the motion of antiferromagnetic domain walls, have neglected the <span class="hlt">intrinsic</span> spin of the textured order parameter.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2014MNRAS.444.3340W','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2014MNRAS.444.3340W"><span id="translatedtitle">The ATLAS 3D project - XXIV. The <span class="hlt">intrinsic</span> shape distribution of early-type galaxies</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Weijmans, Anne-Marie; de Zeeuw, P. T.; Emsellem, Eric; Krajnović, Davor; Lablanche, Pierre-Yves; Alatalo, Katherine; Blitz, Leo; Bois, Maxime; Bournaud, Frédéric; Bureau, Martin; Cappellari, Michele; Crocker, Alison F.; Davies, Roger L.; Davis, Timothy A.; Duc, Pierre-Alain; Khochfar, Sadegh; Kuntschner, Harald; McDermid, Richard M.; Morganti, Raffaella; Naab, Thorsten; Oosterloo, Tom; Sarzi, Marc; Scott, Nicholas; Serra, Paolo; Verdoes Kleijn, Gijs; Young, Lisa M.</p> <p>2014-11-01</p> <p>We use the ATLAS3D sample to perform a study of the <span class="hlt">intrinsic</span> shapes of early-type galaxies, taking advantage of the available combined photometric and kinematic data. Based on our <span class="hlt">ellipticity</span> measurements from the Sloan Digital Sky Survey Data Release 7, and additional imaging from the Isaac Newton Telescope, we first invert the shape distribution of fast and slow rotators under the assumption of axisymmetry. The so-obtained <span class="hlt">intrinsic</span> shape distribution for the fast rotators can be described with a Gaussian with a mean flattening of q = 0.25 and standard deviation σq = 0.14, and an additional tail towards rounder shapes. The slow rotators are much rounder, and are well described with a Gaussian with mean q = 0.63 and σq = 0.09. We then checked that our results were consistent when applying a different and independent method to obtain <span class="hlt">intrinsic</span> shape distributions, by fitting the observed <span class="hlt">ellipticity</span> distributions directly using Gaussian parametrizations for the <span class="hlt">intrinsic</span> axis ratios. Although both fast and slow rotators are identified as early-type galaxies in morphological studies, and in many previous shape studies are therefore grouped together, their shape distributions are significantly different, hinting at different formation scenarios. The <span class="hlt">intrinsic</span> shape distribution of the fast rotators shows similarities with the spiral galaxy population. Including the observed kinematic misalignment in our <span class="hlt">intrinsic</span> shape study shows that the fast rotators are predominantly axisymmetric, with only very little room for triaxiality. For the slow rotators though there are very strong indications that they are (mildly) triaxial.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/20160002237','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/20160002237"><span id="translatedtitle">Dusty Feedback from Massive Black Holes in Two <span class="hlt">Elliptical</span> Galaxies</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Temi, P.; Brighenti, F.; Mathews, W. G.; Amblard, A.; Riguccini, L.</p> <p>2013-01-01</p> <p>Far-infrared dust emission from <span class="hlt">elliptical</span> galaxies informs us about galaxy mergers, feedback energy outbursts from supermassive black holes and the age of galactic stars. We report on the role of AGN feedback observationally by looking for its signatures in <span class="hlt">elliptical</span> galaxies at recent epochs in the nearby universe. We present Herschel observations of two <span class="hlt">elliptical</span> galaxies with strong and spatially extended FIR emission from colder grains 5-10 kpc distant from the galaxy cores. Extended excess cold dust emission is interpreted as evidence of recent feedback-generated AGN energy outbursts in these galaxies, visible only in the FIR, from buoyant gaseous outflows from the galaxy cores.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017ApJ...837L...1M','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017ApJ...837L...1M"><span id="translatedtitle">The Equilibrium Temperature of Planets in <span class="hlt">Elliptical</span> Orbits</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Méndez, Abel; Rivera-Valentín, Edgard G.</p> <p>2017-03-01</p> <p>There exists a positive <span class="hlt">correlation</span> between orbital eccentricity and the average stellar flux that planets receive from their parent star. Often, though, it is assumed that the average equilibrium temperature would correspondingly increase with eccentricity. Here, we test this assumption by calculating and comparing analytic solutions for both the spatial and temporal averages of orbital distance, stellar flux, and equilibrium temperature. Our solutions show that the average equilibrium temperature of a planet, with a constant albedo, slowly decreases with eccentricity until converging to a value 90% that of a circular orbit. This might be the case for many types of planets (e.g., hot Jupiters); however, the actual equilibrium and surface temperature of planets also depend on orbital variations of albedo and greenhouse. Our results also have implications in understanding the climate, habitability, and the occurrence of potential Earth-like planets. For instance, it helps explain why the limits of the habitable zone for planets in highly <span class="hlt">elliptical</span> orbits are wider than expected from the mean flux approximation, as shown by climate models.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/1988PhDT.......218M','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/1988PhDT.......218M"><span id="translatedtitle">Galerkin Methods for Nonlinear <span class="hlt">Elliptic</span> Equations.</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Murdoch, Thomas</p> <p></p> <p>Available from UMI in association with The British Library. Requires signed TDF. This thesis exploits in the nonlinear situation the optimal approximation property of the finite element method for linear, <span class="hlt">elliptic</span> problems. Of particular interest are the steady state semiconductor equations in one and two dimensions. Instead of discretising the differential equations by the finite element method and solving the nonlinear algebraic equations by Newton's method, a Newton linearisation of the continuous problem is preferred and a sequence of linear problems solved until some convergence criterion is achieved. For nonlinear Poisson equations, this approach reduces to solving a sequence of linear, <span class="hlt">elliptic</span>, self -adjoint problems, their approximation by the finite element being optimal in a suitably defined energy norm. Consequently, there is the potential to recover a smoother representation of the underlying solution at each step of the Newton iteration. When this approach is applied to the continuity equations for semiconductor devices, a sequence of linear problems of the form -_{nabla }(anabla u - bu) = f must be solved. The Galerkin method in its crude form does not adequately represent the true solution: however, generalising the framework to permit Petrov-Galerkin approximations remedies the situation. For one dimensional problems, the work of Barrett and Morton allows an optimal test space to be chosen at each step of the Newton iteration so that the resulting approximation is near optimal in a norm closely related to the standard L^2 norm. More detailed information about the underlying solution can then be obtained by recovering a solution of an appropriate form. For two-dimensional problems, since the optimal test functions are difficult to find in practice, an upwinding method due to Heinrich et.al. is used at each step of the Newton iteration. Also, a framework is presented in which various upwind methods may be compared. The thesis also addresses the</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2015PhDT.......187D','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2015PhDT.......187D"><span id="translatedtitle">Tracing the Formation and Evolution of Massive <span class="hlt">Elliptical</span> Galaxies</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Davari, Roozbeh</p> <p></p> <p>Massive galaxies at higher redshift, z > 2, show different characteristics than their local counterparts. They are compact and most likely have a disk. Understanding the evolutionary path of these massive galaxies can give us some clues on how the universe has been behaving in the last 10 billion years. How well can we measure the bulge and disk properties of these systems? We perform two sets of comprehensive simulations in order to systematically quantify the effects of non-homology in structures and the methods employed. For the first set of simulations, by accurately capturing the detailed substructures of nearby <span class="hlt">elliptical</span> galaxies and then rescaling their sizes and signal-to-noise to mimic galaxies at different redshifts, we confirm that the massive quiescent galaxies at z ≈ 2 are significantly more compact <span class="hlt">intrinsically</span> than their local counterparts. Their observed compactness is not a result of missing faint outer light due to systematic errors in modeling. For the second set of simulations, we employ empirical scaling relations to produce realistic-looking two-component local galaxies with a uniform and wide range of bulge-to-total ratios (B/T), and then rescale them to mimic the signal-to-noise ratios and sizes of observed galaxies at z ≈ 2. This provides the first set of simulations for which we can examine the robustness of two-component decomposition of compact disk galaxies at different B/T . We can measure B/T accurately without imposing any constraints on the light profile shape of the bulge, but, due to the small angular sizes of bulges at high redshift, their detailed properties can only be recovered for galaxies with B/T ≥ 0.2. The disk component, by contrast, can be measured with little difficulty. Next, we trace back the evolution of local massive galaxies but performing detailed morphological analysis: namely, single Swrsic fitting and bulge+disk decomposition. CANDELS images and catalogues offer an ideal dataset for this study. We</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://www.osti.gov/scitech/servlets/purl/1035870','SCIGOV-STC'); return false;" href="http://www.osti.gov/scitech/servlets/purl/1035870"><span id="translatedtitle">Physics of <span class="hlt">Intrinsic</span> Rotation in Flux-Driven ITG Turbulence</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Ku, S; Dimond, P H; Dif-Pradalier, G; Kwon, J M; Sarazin, Y; Hahm, T S; Garbet, X; Chang, C S; Latu, G; Yoon, E S; Ghendrih, Ph; Yi, S; Strugarek, A; Solomon, W</p> <p>2012-02-23</p> <p>Global, heat flux-driven ITG gyrokinetic simulations which manifest the formation of macroscopic, mean toroidal flow profiles with peak thermal Mach number 0.05, are reported. Both a particle-in-cell (XGC1p) and a semi-Lagrangian (GYSELA) approach are utilized without a priori assumptions of scale-separation between turbulence and mean fields. Flux-driven ITG simulations with different edge flow boundary conditions show in both approaches the development of net unidirectional <span class="hlt">intrinsic</span> rotation in the co-current direction. <span class="hlt">Intrinsic</span> torque is shown to scale approximately linearly with the inverse scale length of the ion temperature gradient. External momentum input is shown to effectively cancel the <span class="hlt">intrinsic</span> rotation profile, thus confirming the existence of a local residual stress and <span class="hlt">intrinsic</span> torque. Fluctuation intensity, <span class="hlt">intrinsic</span> torque and mean flow are demonstrated to develop inwards from the boundary. The measured <span class="hlt">correlations</span> between residual stress and two fluctuation spectrum symmetry breakers, namely E x B shear and intensity gradient, are similar. Avalanches of (positive) heat flux, which propagate either outwards or inwards, are <span class="hlt">correlated</span> with avalanches of (negative) parallel momentum flux, so that outward transport of heat and inward transport of parallel momentum are <span class="hlt">correlated</span> and mediated by avalanches. The probability distribution functions of the outward heat flux and the inward momentum flux show strong structural similarity</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/24708372','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/24708372"><span id="translatedtitle"><span class="hlt">Intrinsic</span> graph structure estimation using graph Laplacian.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Noda, Atsushi; Hino, Hideitsu; Tatsuno, Masami; Akaho, Shotaro; Murata, Noboru</p> <p>2014-07-01</p> <p>A graph is a mathematical representation of a set of variables where some pairs of the variables are connected by edges. Common examples of graphs are railroads, the Internet, and neural networks. It is both theoretically and practically important to estimate the intensity of direct connections between variables. In this study, a problem of estimating the <span class="hlt">intrinsic</span> graph structure from observed data is considered. The observed data in this study are a matrix with elements representing dependency between nodes in the graph. The dependency represents more than direct connections because it includes influences of various paths. For example, each element of the observed matrix represents a co-occurrence of events at two nodes or a <span class="hlt">correlation</span> of variables corresponding to two nodes. In this setting, spurious <span class="hlt">correlations</span> make the estimation of direct connection difficult. To alleviate this difficulty, a digraph Laplacian is used for characterizing a graph. A generative model of this observed matrix is proposed, and a parameter estimation algorithm for the model is also introduced. The notable advantage of the proposed method is its ability to deal with directed graphs, while conventional graph structure estimation methods such as covariance selections are applicable only to undirected graphs. The algorithm is experimentally shown to be able to identify the <span class="hlt">intrinsic</span> graph structure.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2015EPSC...10..872A','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2015EPSC...10..872A"><span id="translatedtitle"><span class="hlt">Intrinsic</span> structure in Saturn's rings</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Albers, N.</p> <p>2015-10-01</p> <p>Saturn's rings are the most prominent in our Solar system and one example of granular matter in space. Dominated by tides and inelastic collisions the system is highly flattened being almost 300000km wide while only tens of meters thick. Individual particles are composed of primarily water ice and range from microns to few tens of meters in size. Apparent patterns comprise ringlets, gaps, kinematic wakes, propellers, bending waves, and the winding spiral arms of density waves. These large-scale structures are perturbations foremost created by external as well as embedded moons. Observations made by the Cassini spacecraft currently in orbit around Saturn show these structures in unprecedented detail. But high-resolution measurements reveal the presence of small-scale structures throughout the system. These include self-gravity wakes (50-100m), overstable waves (100-300m), subkm structure at the A and B ring edges, "straw" and "ropy" structures (1-3km), and the C ring "ghosts". Most of these had not been anticipated and are found in perturbed regions, driven by resonances with external moons, where the system undergoes periodic phases of compression and relaxation that <span class="hlt">correlate</span> with the presence of structure. High velocity dispersion and the presence of large clumps imply structure formation on time scales as short as one orbit (about 10 hours). The presence of these <span class="hlt">intrinsic</span> structures is seemingly the response to varying local conditions such as internal density, optical depth, underlying particle size distribution, granular temperature, and distance from the central planet. Their abundance provides evidence for an active and dynamic ring system where aggregation and fragmentation are ongoing on orbital timescales. Thus a kinetic description of the rings may be more appropriate than the fluid one. I will present Cassini Ultraviolet Spectrometer (UVIS) High Speed Photometer (HSP) occultations, Voyager 1 and 2 Imaging Science Subsystem (ISS), and high</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/15891978','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/15891978"><span id="translatedtitle">Ulnar <span class="hlt">intrinsic</span> anatomy and dysfunction.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Dell, Paul C; Sforzo, Christopher R</p> <p>2005-01-01</p> <p>Normal hand function is a balance between the extrinsic and <span class="hlt">intrinsic</span> musculature. Although individually the <span class="hlt">intrinsics</span> are small muscles in diameter, collectively they represent a large muscle that contributes approximately 50% of grip strength. Dysfunction of the <span class="hlt">intrinsics</span> consequently leads to impaired grip and pinch strength as well recognized deformities. Low ulnar nerve palsy preserves ulnar innervated extrinsics resulting in sensory loss, digital clawing, thumb deformity, abduction of the small finger, and asynchronous finger motion. High ulnar nerve palsy is characterized by the above plus paralysis of the ulnar profundi and the flexor carpi ulnaris. Understanding the normal anatomy allows the clinician to identify the site of the lesion and plan appropriate surgical intervention. This article revisits the classic work of Richard J. Smith on ulnar nerve palsy with contemporary perspective.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/19836901','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/19836901"><span id="translatedtitle">The relationship between motivational structure, sense of control, <span class="hlt">intrinsic</span> motivation and university students' alcohol consumption.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Shamloo, Zohreh Sepehri; Cox, W Miles</p> <p>2010-02-01</p> <p>The aim of this study was to determine how sense of control and <span class="hlt">intrinsic</span> motivation are related to university students' motivational structure and alcohol consumption. Participants were 94 university students who completed the Personal Concerns Inventory, Shapiro Control Inventory, Helplessness Questionnaire, <span class="hlt">Intrinsic</span>-Extrinsic Aspirations Scale, and Alcohol Use Questionnaire. Results showed that sense of control and <span class="hlt">intrinsic</span> motivation were positively <span class="hlt">correlated</span> with adaptive motivation and negatively <span class="hlt">correlated</span> with alcohol consumption. Mediational analyses indicated that adaptive motivation fully mediated the relationship between sense of control/<span class="hlt">intrinsic</span> motivation and alcohol consumption.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016OptCo.359...31W','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016OptCo.359...31W"><span id="translatedtitle"><span class="hlt">Elliptic</span> Hermite-Gaussian soliton in anisotropic strong nonlocal media</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Wang, Qing; Li, JingZhen</p> <p>2016-01-01</p> <p>The propagation of <span class="hlt">elliptic</span> Hermite-Gaussian (HG) beam in strong nonlocal media with <span class="hlt">elliptic</span> Gaussian-shaped response function was studied by variational approach as well as numerical simulate. The evolution equations of the beam widths in x- and y-directions are obtained and the <span class="hlt">elliptic</span> HG soliton is found. For forming such a soliton, the ratio of the square of the beam width must be proportional to the ratio of the characteristic length of the material, and the initial power should be equal to the two critical powers in x- and y-directions. For the anisotropic nonlinearity of the media, the instability of the high-order <span class="hlt">elliptic</span> HG beam is increase as the increase of the order.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19860026173&hterms=isophotes&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3Disophotes','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19860026173&hterms=isophotes&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3Disophotes"><span id="translatedtitle">Boxy isophotes, discs and dust lanes in <span class="hlt">elliptical</span> galaxies</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Lauer, T. R.</p> <p>1985-01-01</p> <p>CCD images of 42 <span class="hlt">elliptical</span> and S0 galaxies are examined for low-contrast structures or subtle distortions of the isophotes from perfect ellipses. 75 percent of the galaxies have isophotes completely describable as concentric ellipses to within the photometry errors. 'Boxy' isophotes, stellar discs, and dust lanes are detected in the remaining 25 percent of the sample. The boxy <span class="hlt">elliptical</span> galaxies appear dynamically indistinguishable from normal <span class="hlt">ellipticals</span> and are therefore different from boxy bulges, which rotate rapidly. Most of the galaxies with faint discs, however, appear dynamically similar to S0 galaxies. Nearly edge-on dust lanes are found in four galaxies, which suggests that dust lanes may commonly occur in <span class="hlt">elliptical</span> galaxies.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/22418498','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/22418498"><span id="translatedtitle">Rigorous theory on <span class="hlt">elliptical</span> mirror focusing for point scanning microscopy.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Liu, Jian; Tan, Jiubin; Wilson, Tony; Zhong, Cien</p> <p>2012-03-12</p> <p>A rigorous <span class="hlt">elliptical</span> mirror focusing formula based on spherical wave transformation is derived as a kind of imaging technique with high NA for potential applications in molecule imaging, spectroscopy and industrial artifact microscopy. An apodization factor is given and used to compare the energy conversation rules in lens transmission and parabolic and <span class="hlt">elliptical</span> mirror reflections. Simulation results indicate that the axial HFWHM of <span class="hlt">elliptical</span> and parabolic mirrors is about 80% of the corresponding HFWHM of lens in case of NA = 1 and φs = 0, and the side lobe noise is also slightly lower than that of lens, but the transverse HFWHM of mirrors is comparatively wider despite the width of main lobe is still smaller. In comparison with parabolic mirror based system, an <span class="hlt">elliptical</span> mirror based system is potentially promising in aberration control of incident beam when the aperture of mirror is enlarged to adapt a large stage or specimen container at a small beam shading ratio.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://www.osti.gov/scitech/servlets/purl/793986','SCIGOV-STC'); return false;" href="http://www.osti.gov/scitech/servlets/purl/793986"><span id="translatedtitle"><span class="hlt">Elliptic</span> Solvers with Adaptive Mesh Refinement on Complex Geometries</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Phillip, B.</p> <p>2000-07-24</p> <p>Adaptive Mesh Refinement (AMR) is a numerical technique for locally tailoring the resolution computational grids. Multilevel algorithms for solving <span class="hlt">elliptic</span> problems on adaptive grids include the Fast Adaptive Composite grid method (FAC) and its parallel variants (AFAC and AFACx). Theory that confirms the independence of the convergence rates of FAC and AFAC on the number of refinement levels exists under certain <span class="hlt">ellipticity</span> and approximation property conditions. Similar theory needs to be developed for AFACx. The effectiveness of multigrid-based <span class="hlt">elliptic</span> solvers such as FAC, AFAC, and AFACx on adaptively refined overlapping grids is not clearly understood. Finally, a non-trivial eye model problem will be solved by combining the power of using overlapping grids for complex moving geometries, AMR, and multilevel <span class="hlt">elliptic</span> solvers.</p> </li> </ol> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_10");'>10</a></li> <li><a href="#" onclick='return showDiv("page_11");'>11</a></li> <li class="active"><span>12</span></li> <li><a href="#" onclick='return showDiv("page_13");'>13</a></li> <li><a href="#" onclick='return showDiv("page_14");'>14</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div><!-- col-sm-12 --> </div><!-- row --> </div><!-- page_12 --> <div id="page_13" class="hiddenDiv"> <div class="row"> <div class="col-sm-12"> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_11");'>11</a></li> <li><a href="#" onclick='return showDiv("page_12");'>12</a></li> <li class="active"><span>13</span></li> <li><a href="#" onclick='return showDiv("page_14");'>14</a></li> <li><a href="#" onclick='return showDiv("page_15");'>15</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div> </div> <div class="row"> <div class="col-sm-12"> <ol class="result-class" start="241"> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016JDE...260.5043D','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016JDE...260.5043D"><span id="translatedtitle">C1,1 regularity for degenerate <span class="hlt">elliptic</span> obstacle problems</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Daskalopoulos, Panagiota; Feehan, Paul M. N.</p> <p>2016-03-01</p> <p>The Heston stochastic volatility process is a degenerate diffusion process where the degeneracy in the diffusion coefficient is proportional to the square root of the distance to the boundary of the half-plane. The generator of this process with killing, called the <span class="hlt">elliptic</span> Heston operator, is a second-order, degenerate-<span class="hlt">elliptic</span> partial differential operator, where the degeneracy in the operator symbol is proportional to the distance to the boundary of the half-plane. In mathematical finance, solutions to the obstacle problem for the <span class="hlt">elliptic</span> Heston operator correspond to value functions for perpetual American-style options on the underlying asset. With the aid of weighted Sobolev spaces and weighted Hölder spaces, we establish the optimal C 1 , 1 regularity (up to the boundary of the half-plane) for solutions to obstacle problems for the <span class="hlt">elliptic</span> Heston operator when the obstacle functions are sufficiently smooth.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/1999APS..DPP.FP143F','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/1999APS..DPP.FP143F"><span id="translatedtitle">Bifurcations in <span class="hlt">elliptical</span>, asymmetric non-neutral plasmas</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Fajans, Joel; Gilson, Erik</p> <p>1999-11-01</p> <p>When subjected to a stationary, l=2 potential perturbation on the wall, a pure electron plasma will deform into an <span class="hlt">elliptical</span> shape. At first, the plasma's <span class="hlt">ellipticity</span> is proportional to the strength of the potential perturbation. Once the perturbation is increased beyond a critical value, the plasma equilibrium bifurcates into two off-axis states. This bifurcation has been observed experimentally and will be described in this poster. (see http://socrates.berkeley.edu/ fajans/EquilStab/EllipseBifurcation.avi)</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2010Nonli..23.1741L','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2010Nonli..23.1741L"><span id="translatedtitle">A class of variational-hemivariational inequalities of <span class="hlt">elliptic</span> type</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Liu, Zhenhai; Motreanu, Dumitru</p> <p>2010-07-01</p> <p>This paper is devoted to the existence of solutions for variational-hemivariational inequalities of <span class="hlt">elliptic</span> type, with a higher order quasilinear principal part, at resonance as well as at nonresonance. The approach relies on the use of pseudomonotone operators. By means of the notion of Clarke's generalized gradient and the properties of the first eigenfunction of the quasilinear principal part, we also build a Landesman-Lazer theory in the nonsmooth framework of variational-hemivariational inequalities of <span class="hlt">elliptic</span> type.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/1999JMP....40.6339G','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/1999JMP....40.6339G"><span id="translatedtitle">On the explicit solutions of the <span class="hlt">elliptic</span> Calogero system</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Gavrilov, L.; Perelomov, A. M.</p> <p>1999-12-01</p> <p>Let q1,q2,…,qN be the coordinates of N particles on the circle, interacting with the integrable potential ∑j<kN℘(qj-qk), where ℘ is the Weierstrass <span class="hlt">elliptic</span> function. We show that every symmetric <span class="hlt">elliptic</span> function in q1,q2,…,qN is a meromorphic function in time. We give explicit formulas for these functions in terms of genus N-1 theta functions.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2011AIPC.1389..317J','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2011AIPC.1389..317J"><span id="translatedtitle">Remarks of <span class="hlt">Elliptic</span> Curves Derived from Ant Colony Routing</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Jung, Sangsu; Kim, Daeyeoul; Singh, Dhananjay</p> <p>2011-09-01</p> <p>We deal with an ant colony based routing model for wireless multi-hop networks. Our model adopts an <span class="hlt">elliptic</span> curve equation, which is beneficial to design pheromone dynamics for load balancing and packet delivery robustness. Due to the attribute of an <span class="hlt">elliptic</span> curve equation, our model prevents the over-utilization of a specific node, distinctively from conventional ant colony based schemes. Numerical simulations exhibit the characteristics of our model with respect to various parameters.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4948636','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4948636"><span id="translatedtitle">Depth-resolved measurements with <span class="hlt">elliptically</span> polarized reflectance spectroscopy</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Bailey, Maria J.; Sokolov, Konstantin</p> <p>2016-01-01</p> <p>The ability of <span class="hlt">elliptical</span> polarized reflectance spectroscopy (EPRS) to detect spectroscopic alterations in tissue mimicking phantoms and in biological tissue in situ is demonstrated. It is shown that there is a linear relationship between light penetration depth and <span class="hlt">ellipticity</span>. This dependence is used to demonstrate the feasibility of a depth-resolved spectroscopic imaging using EPRS. The advantages and drawbacks of EPRS in evaluation of biological tissue are analyzed and discussed. PMID:27446712</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19880060464&hterms=Monsters&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D30%26Ntt%3DMonsters','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19880060464&hterms=Monsters&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D30%26Ntt%3DMonsters"><span id="translatedtitle">Do massive black holes reside in <span class="hlt">elliptical</span> galaxies?</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Fabian, A. C.; Canizares, C. R.</p> <p>1988-01-01</p> <p>The accretion by a central black hole of the hot interstellar medium in an <span class="hlt">elliptical</span> galaxy is investigated, and the minimum expected luminosity and manner of its emission is estimated. It is not obviously detected at any wavelength. The problem of 'starving the monster', if indeed there is a monster, is raised. The simplest conclusion from the evidence is that most bright <span class="hlt">elliptical</span> galaxies do not contain massive black holes.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://www.osti.gov/scitech/servlets/purl/6431631','SCIGOV-STC'); return false;" href="http://www.osti.gov/scitech/servlets/purl/6431631"><span id="translatedtitle">Beam-beam deflection and signature curves for <span class="hlt">elliptic</span> beams</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Ziemann, V.</p> <p>1990-10-22</p> <p>In this note we will present closed expressions for the beam-beam deflection angle for arbitrary <span class="hlt">elliptic</span> beams including tilt. From these expressions signature curves, i.e., systematic deviations from the round beam deflection curve due to <span class="hlt">ellipticity</span> or tilt are derived. In the course of the presentation we will prove that it is generally impossible to infer individual beam sizes from beam-beam deflection scans. 3 refs., 2 figs.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=2588348','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=2588348"><span id="translatedtitle">Functional Anthology of <span class="hlt">Intrinsic</span> Disorder. III. Ligands, Postranslational Modifications and Diseases Associated with <span class="hlt">Intrinsically</span> Disordered Proteins</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Xie, Hongbo; Vucetic, Slobodan; Iakoucheva, Lilia M.; Oldfield, Christopher J.; Dunker, A. Keith; Obradovic, Zoran; Uversky, Vladimir N.</p> <p>2008-01-01</p> <p>Currently, the understanding of the relationships between function, amino acid sequence and protein structure continues to represent one of the major challenges of the modern protein science. As much as 50% of eukaryotic proteins are likely to contain functionally important long disordered regions. Many proteins are wholly disordered but still possess numerous biologically important functions. However, the number of experimentally confirmed disordered proteins with known biological functions is substantially smaller than their actual number in nature. Therefore, there is a crucial need for novel bioinformatics approaches that allow projection of the current knowledge from a few experimentally verified examples to much larger groups of known and potential proteins. The elaboration of a bioinformatics tool for the analysis of functional diversity of <span class="hlt">intrinsically</span> disordered proteins and application of this data mining tool to >200,000 proteins from Swiss-Prot database, each annotated with at least one of the 875 functional keywords was described in the first paper of this series (Xie H., Vucetic S., Iakoucheva L.M., Oldfield C.J., Dunker A.K., Obradovic Z., Uversky V.N. (2006) Functional anthology of <span class="hlt">intrinsic</span> disorder. I. Biological processes and functions of proteins with long disordered regions. J. Proteome Res.). Using this tool, we have found that out of the 711 Swiss-Prot functional keywords associated with at least 20 proteins, 262 were strongly positively <span class="hlt">correlated</span> with long <span class="hlt">intrinsically</span> disordered regions, and 302 were strongly negatively <span class="hlt">correlated</span>. Illustrative examples of functional disorder or order were found for the vast majority of keywords showing strongest positive or negative <span class="hlt">correlation</span> with <span class="hlt">intrinsic</span> disorder, respectively. Some 80 Swiss-Prot keywords associated with disorder- and order-driven biological processes and protein functions were described in the first paper (Xie H., Vucetic S., Iakoucheva L.M., Oldfield C.J., Dunker A.K., Obradovic</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2013JOpt...15j5709L','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2013JOpt...15j5709L"><span id="translatedtitle">Focusing of an <span class="hlt">elliptical</span> mirror based system with aberrations</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Liu, Jian; Ai, Min; Zhang, He; Wang, Chao; Tan, Jiubin</p> <p>2013-10-01</p> <p>The effect of primary aberrations on the focusing of an <span class="hlt">elliptical</span> mirror based system is studied by using the Debye integral. Specifically, the apodization function for <span class="hlt">elliptical</span> mirror is derived and expressed by the eccentricity of the <span class="hlt">elliptical</span> mirror. For the <span class="hlt">elliptical</span> mirror with low aperture, intensity distributions in the presence of aberrations near focus are presented based on the derived scalar theory, while for the high-aperture condition, vectorial theory is used to describe the electric field in the focal region. In particular, the effect of aberrations is studied under radially polarized illumination. Moreover, tolerance conditions are given based on the knowledge of focusing with aberrations. It is found that the <span class="hlt">elliptical</span> mirror based system shares a similar level of tolerance conditions with that of the single lens, while both of them are more sensitive to the presence of astigmatism than other aberrations. It is believed that the results will theoretically support the application of the high-aperture <span class="hlt">elliptical</span> mirror in scanning microscopy.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://www.osti.gov/scitech/servlets/purl/781479','SCIGOV-STC'); return false;" href="http://www.osti.gov/scitech/servlets/purl/781479"><span id="translatedtitle"><span class="hlt">ELLIPT</span>2D: A Flexible Finite Element Code Written Python</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Pletzer, A.; Mollis, J.C.</p> <p>2001-03-22</p> <p>The use of the Python scripting language for scientific applications and in particular to solve partial differential equations is explored. It is shown that Python's rich data structure and object-oriented features can be exploited to write programs that are not only significantly more concise than their counter parts written in Fortran, C or C++, but are also numerically efficient. To illustrate this, a two-dimensional finite element code (<span class="hlt">ELLIPT</span>2D) has been written. <span class="hlt">ELLIPT</span>2D provides a flexible and easy-to-use framework for solving a large class of second-order <span class="hlt">elliptic</span> problems. The program allows for structured or unstructured meshes. All functions defining the <span class="hlt">elliptic</span> operator are user supplied and so are the boundary conditions, which can be of Dirichlet, Neumann or Robbins type. <span class="hlt">ELLIPT</span>2D makes extensive use of dictionaries (hash tables) as a way to represent sparse matrices.Other key features of the Python language that have been widely used include: operator over loading, error handling, array slicing, and the Tkinter module for building graphical use interfaces. As an example of the utility of <span class="hlt">ELLIPT</span>2D, a nonlinear solution of the Grad-Shafranov equation is computed using a Newton iterative scheme. A second application focuses on a solution of the toroidal Laplace equation coupled to a magnetohydrodynamic stability code, a problem arising in the context of magnetic fusion research.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/21269160','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/21269160"><span id="translatedtitle">STRUCTURE AND FORMATION OF <span class="hlt">ELLIPTICAL</span> AND SPHEROIDAL GALAXIES</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Kormendy, John; Fisher, David B.; Cornell, Mark E.; Bender, Ralf E-mail: dbfisher@astro.as.utexas.edu E-mail: bender@usm.uni-muenchen.de</p> <p>2009-05-15</p> <p>New surface photometry of all known <span class="hlt">elliptical</span> galaxies in the Virgo cluster is combined with published data to derive composite profiles of brightness, <span class="hlt">ellipticity</span>, position angle, isophote shape, and color over large radius ranges. These provide enough leverage to show that Sersic log I {proportional_to} r {sup 1/n} functions fit the brightness profiles I(r) of nearly all <span class="hlt">ellipticals</span> remarkably well over large dynamic ranges. Therefore, we can confidently identify departures from these profiles that are diagnostic of galaxy formation. Two kinds of departures are seen at small radii. All 10 of our <span class="hlt">ellipticals</span> with total absolute magnitudes M{sub VT} {<=} -21.66 have cuspy cores-'missing light'-at small radii. Cores are well known and naturally scoured by binary black holes (BHs) formed in dissipationless ('dry') mergers. All 17 <span class="hlt">ellipticals</span> with -21.54 {<=} M{sub VT} {<=} -15.53 do not have cores. We find a new distinct component in these galaxies: all coreless <span class="hlt">ellipticals</span> in our sample have extra light at the center above the inward extrapolation of the outer Sersic profile. In large <span class="hlt">ellipticals</span>, the excess light is spatially resolved and resembles the central components predicted in numerical simulations of mergers of galaxies that contain gas. In the simulations, the gas dissipates, falls toward the center, undergoes a starburst, and builds a compact stellar component that, as in our observations, is distinct from the Sersic-function main body of the <span class="hlt">elliptical</span>. But <span class="hlt">ellipticals</span> with extra light also contain supermassive BHs. We suggest that the starburst has swamped core scouring by binary BHs. That is, we interpret extra light components as a signature of formation in dissipative ('wet') mergers. Besides extra light, we find three new aspects to the ('E-E') dichotomy into two types of <span class="hlt">elliptical</span> galaxies. Core galaxies are known to be slowly rotating, to have relatively anisotropic velocity distributions, and to have boxy isophotes. We show that they have</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://eric.ed.gov/?q=body+AND+mind&id=EJ1076241','ERIC'); return false;" href="http://eric.ed.gov/?q=body+AND+mind&id=EJ1076241"><span id="translatedtitle"><span class="hlt">Intrinsic</span> Motivation in Physical Education</span></a></p> <p><a target="_blank" href="http://www.eric.ed.gov/ERICWebPortal/search/extended.jsp?_pageLabel=advanced">ERIC Educational Resources Information Center</a></p> <p>Davies, Benjamin; Nambiar, Nathan; Hemphill, Caroline; Devietti, Elizabeth; Massengale, Alexandra; McCredie, Patrick</p> <p>2015-01-01</p> <p>This article describes ways in which educators can use Harter's perceived competence motivation theory, the achievement goal theory, and self-determination theory to develop students' <span class="hlt">intrinsic</span> motivation to maintain physical fitness, as demonstrated by the Sound Body Sound Mind curriculum and proven effective by the 2013 University of…</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://files.eric.ed.gov/fulltext/ED188782.pdf','ERIC'); return false;" href="http://files.eric.ed.gov/fulltext/ED188782.pdf"><span id="translatedtitle">Individual Patterns in <span class="hlt">Intrinsic</span> Motivation.</span></a></p> <p><a target="_blank" href="http://www.eric.ed.gov/ERICWebPortal/search/extended.jsp?_pageLabel=advanced">ERIC Educational Resources Information Center</a></p> <p>Hom, Harry L., Jr.; Maxwell, Frederick R.</p> <p></p> <p>The effects of extrinsic reward on students' <span class="hlt">intrinsic</span> interest was investigated using a single-subject design in a behavior disorders classroom. Baseline measures of the interest level of five children (ages 9-11 years) were collected for academic and non-academic tasks. Assessment was then made of each subject's response hierarchy or level of…</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/20020061791','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/20020061791"><span id="translatedtitle"><span class="hlt">Elliptic</span> Relaxation of a Tensor Representation for the Redistribution Terms in a Reynolds Stress Turbulence Model</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Carlson, J. R.; Gatski, T. B.</p> <p>2002-01-01</p> <p>A formulation to include the effects of wall proximity in a second-moment closure model that utilizes a tensor representation for the redistribution terms in the Reynolds stress equations is presented. The wall-proximity effects are modeled through an <span class="hlt">elliptic</span> relaxation process of the tensor expansion coefficients that properly accounts for both <span class="hlt">correlation</span> length and time scales as the wall is approached. Direct numerical simulation data and Reynolds stress solutions using a full differential approach are compared for the case of fully developed channel flow.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2015OptCo.338..484A','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2015OptCo.338..484A"><span id="translatedtitle">Electron dynamics of molecular double ionization by <span class="hlt">elliptically</span> polarized few-cycle laser pulses</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Ai-Hong, Tong; Guo-Qiang, Feng; Dan, Liu</p> <p>2015-03-01</p> <p>Using the classical ensemble method, we have investigated double ionization (DI) of diatomic molecules driven by <span class="hlt">elliptically</span> polarized few-cycle laser pulses. The results show that DI channel depends strongly on internuclear distances (R), which is dominated by nonsequential double ionization (NSDI) for small and large R, while sequential double ionization (SDI) for mediate R. By tracing NSDI trajectories, we find that NSDI mainly originates from recollision process for small R and collision process for large R. Moreover, the <span class="hlt">correlated</span> momentum distributions along the long axis strongly depend on the carrier-envelope-phase (CEP), and this phase dependence is affected by R.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017GeoJI.tmp...24M','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017GeoJI.tmp...24M"><span id="translatedtitle">Retrieval of Rayleigh Wave <span class="hlt">Ellipticity</span> from Ambient Vibration Recordings</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Maranò, Stefano; Hobiger, Manuel; Fäh, Donat</p> <p>2017-01-01</p> <p>The analysis of ambient vibrations is a useful tool in microzonation and geotechnical investigations. Ambient vibrations are composed to a large part of surface waves, both Love and Rayleigh waves. One reason to analyse surface waves is that they carry information about the subsurface. The dispersion curve of Rayleigh waves and Love waves can be retrieved using array processing techniques. The Rayleigh wave <span class="hlt">ellipticity</span>, including the sense of rotation of the particle motion, can also be retrieved using array techniques. These quantities are used in an inversion procedure aimed at obtaining a structural model of the subsurface. The focus of this work is the retrieval of Rayleigh wave <span class="hlt">ellipticity</span>. We show applications of the (ML) method presented in Maranó et al. (2012) to a number of sites in Switzerland. The sites examined are chosen to reflect a wide range of soil conditions that are of interest in microzonation studies. Using a synthetic wavefield with known structural model, we compare our results with theoretical <span class="hlt">ellipticity</span> curves and we show the accuracy of the considered algorithm. The sense of rotation of the particle motion (prograde vs. retrograde) is also estimated. In addition, we show that by modelling the presence of both Love and Rayleigh waves it is possible to mitigate the disruptive influence of Love waves on the estimation of Rayleigh wave <span class="hlt">ellipticity</span>. Using recordings from several real sites, we show that it is possible to retrieve the <span class="hlt">ellipticity</span> curve over a broad range of frequencies. Fundamental modes and higher modes are retrieved. Singularities of the <span class="hlt">ellipticity</span>, corresponding to a change of the sense of rotation from prograde to retrograde (or vice versa), are detected with great accuracy. Knowledge of Rayleigh wave <span class="hlt">ellipticity</span>, including the sense of rotation, is useful in several ways. The <span class="hlt">ellipticity</span> angle allows us to pinpoint accurately the frequency of singularities (i.e., peaks and zeros of the H/V representation of the</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2015HMT....51..239E','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2015HMT....51..239E"><span id="translatedtitle">Effect of opposed eccentricity on free convective heat transfer through <span class="hlt">elliptical</span> annulus enclosures in blunt and slender orientations</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Eid, E. I.; Abdel-Halim, M.; Easa, A. S.</p> <p>2015-02-01</p> <p>This paper presents an experimental investigation for the effect of opposed lateral and vertical eccentricities on free convective heat transfer through <span class="hlt">elliptical</span> annulus enclosures in blunt and slender orientations. Three test specimens of <span class="hlt">elliptical</span> cylinders having an equal radius ratio and an equal length were prepared. The surface area of the inner cylinder is the same for each specimen as well as the area of the outer cylinder. Different <span class="hlt">elliptical</span> ratios of 0.662, 0.866 and 0.968 were investigated. Experimental tests were done by maintaining constant heat flux on the inner cylinder and the outer one was exposed to approximately constant temperature of the closed laboratory. Both annuals ends of the annular <span class="hlt">elliptical</span> cylinders were closed by cork to form the annular enclosure space. The experimental tests monitored Rayleigh number (1.642 × 103 ≤ Ra* ≤ 3.849 × 106). The effects of both opposed vertical and lateral eccentricities for both blunt and slender orientations were investigated. The experimental results were fitted by <span class="hlt">correlations</span>. Considerable agreement was found in the comparison among the results of present and previous works. Opposed eccentricity enhances free convective heat transfer by about 40 % from concentric. Slender orientation results in more enhancements in free convection than blunt one.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2013NuPhB.871..127B','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2013NuPhB.871..127B"><span id="translatedtitle">An <span class="hlt">elliptic</span> parameterisation of the Zamolodchikov model</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Bazhanov, Vladimir V.; Mangazeev, Vladimir V.; Okada, Yuichiro; Sergeev, Sergey M.</p> <p>2013-06-01</p> <p>The Zamolodchikov model describes an exact relativistic factorized scattering theory of straight strings in (2+1)-dimensional space-time. It also defines an integrable 3D lattice model of statistical mechanics and quantum field theory. The three-string S-matrix satisfies the tetrahedron equation which is a 3D analog of the Yang-Baxter equation. Each S-matrix depends on three dihedral angles formed by three intersecting planes, whereas the tetrahedron equation contains five independent spectral parameters, associated with angles of an Euclidean tetrahedron. The vertex weights are given by rather complicated expressions involving square roots of trigonometric function of the spectral parameters, which is quite unusual from the point of view of 2D solvable lattice models. In this paper we consider a particular four-parameter specialisation of the tetrahedron equation when one of its vertices goes to infinity and the tetrahedron itself degenerates into an infinite prism. We show that in this limit all the vertex weights in the tetrahedron equation can be represented as meromorphic functions on an <span class="hlt">elliptic</span> curve. Moreover we show that a special reduction of the tetrahedron equation in this case leads precisely to an example of the tetrahedral Zamolodchikov algebra, previously constructed by Korepanov. This algebra plays important role for a "layered" construction of the Shastry's R-matrix and the 2D S-matrix appearing in the problem of the ADS/CFT correspondence for N=4 SUSY Yang-Mills theory in four dimensions. Possible applications of our results in this field are briefly discussed.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/24589355','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/24589355"><span id="translatedtitle">New force field on modeling <span class="hlt">intrinsically</span> disordered proteins.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Wang, Wei; Ye, Wei; Jiang, Cheng; Luo, Ray; Chen, Hai-Feng</p> <p>2014-09-01</p> <p><span class="hlt">Intrinsically</span> disordered proteins or <span class="hlt">intrinsically</span> disordered protein regions comprise a large portion of eukaryotic proteomes (between 35% and 51%). These <span class="hlt">intrinsically</span> disordered proteins were found to link with cancer and various other diseases. However, widely used additive force field parameter sets are insufficient in quantifying the structural properties of <span class="hlt">intrinsically</span> disordered proteins. Therefore, we explored to a systematic correction of a base additive force field parameter set (chosen as Amber ff99SBildn) to correct the biases that was first demonstrated in simulations with the base parameter set. Specifically, the φ/ψ distributions of disorder-promoting residues were systematically corrected with the CMAP method. Our simulations show that the CMAP corrected Amber parameter set, termed ff99IDPs, improves the φ/ψ distributions of the disorder-promoting residues with respect to the benchmark data of <span class="hlt">intrinsically</span> disordered protein structures, with root mean-squared percentage deviation less than 0.15% between the simulation and the benchmark. Our further validation shows that the chemical shifts from the ff99IDPs simulations are in quantitative agreement with those from reported NMR measurements for two tested IDPs, MeV NTAIL , and p53. The predicted residue dipolar couplings also show high <span class="hlt">correlation</span> with experimental data. Interestingly, our simulations show that ff99IDPs can still be used to model the ordered state when the <span class="hlt">intrinsically</span> disordered proteins are in complex, in contrast to ff99SBildn that can be applied well only to the ordered complex structures. These findings confirm that the newly proposed Amber ff99IDPs parameter set provides a reasonable tool in further studies of <span class="hlt">intrinsically</span> disordered protein structures. In addition, our study also shows the importance of considering <span class="hlt">intrinsically</span> disordered protein structures in general-purposed force field developments for both additive and non-additive models.</p> </li> </ol> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_11");'>11</a></li> <li><a href="#" onclick='return showDiv("page_12");'>12</a></li> <li class="active"><span>13</span></li> <li><a href="#" onclick='return showDiv("page_14");'>14</a></li> <li><a href="#" onclick='return showDiv("page_15");'>15</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div><!-- col-sm-12 --> </div><!-- row --> </div><!-- page_13 --> <div id="page_14" class="hiddenDiv"> <div class="row"> <div class="col-sm-12"> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_12");'>12</a></li> <li><a href="#" onclick='return showDiv("page_13");'>13</a></li> <li class="active"><span>14</span></li> <li><a href="#" onclick='return showDiv("page_15");'>15</a></li> <li><a href="#" onclick='return showDiv("page_16");'>16</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div> </div> <div class="row"> <div class="col-sm-12"> <ol class="result-class" start="261"> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=393832','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=393832"><span id="translatedtitle"><span class="hlt">Intrinsic</span> randomness and <span class="hlt">intrinsic</span> irreversibility in classical dynamical systems</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Courbage, M.; Prigogine, I.</p> <p>1983-01-01</p> <p>We continue our previous work on dynamic “<span class="hlt">intrinsically</span> random” systems for which we can derive dissipative Markov processes through a one-to-one change of representation. For these systems, the unitary group of evolution can be transformed in this way into two distinct Markov processes leading to equilibrium for either t→ + ∞ or t→ - ∞. To lift the degeneracy, we first formulate the second principle as a selection rule that is meaningful in <span class="hlt">intrinsically</span> random systems. For these systems, this excludes a set of unrealizable states. As a result of this exclusion, permitted initial conditions correspond to a set of states that is not invariant through velocity inversion. In this way, the time-reversal symmetry of dynamics is broken and these systems acquire a new feature we may call “<span class="hlt">intrinsic</span> irreversibility.” The set of admitted initial conditions can be characterized by an entropy displaying the amount of information necessary for their preparation. The initial conditions selected by the second law correspond to a finite amount of information, while the initial conditions that are rejected correspond to an infinite amount of information and are therefore “impossible.” We believe that our formulation permits a microscopic formulation of the second law of thermodynamics for well-defined classes of dynamical systems. PMID:16578774</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016JSV...380....1K','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016JSV...380....1K"><span id="translatedtitle">Jacobi <span class="hlt">elliptic</span> functions: A review of nonlinear oscillatory application problems</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Kovacic, Ivana; Cveticanin, Livija; Zukovic, Miodrag; Rakaric, Zvonko</p> <p>2016-10-01</p> <p>This review paper is concerned with the applications of Jacobi <span class="hlt">elliptic</span> functions to nonlinear oscillators whose restoring force has a monomial or binomial form that involves cubic and/or quadratic nonlinearity. First, geometric interpretations of three basic Jacobi <span class="hlt">elliptic</span> functions are given and their characteristics are discussed. It is shown then how their different forms can be utilized to express exact solutions for the response of certain free conservative oscillators. These forms are subsequently used as a starting point for a presentation of different quantitative techniques for obtaining an approximate response for free perturbed nonlinear oscillators. An illustrative example is provided. Further, two types of externally forced nonlinear oscillators are reviewed: (i) those that are excited by <span class="hlt">elliptic</span>-type excitations with different exact and approximate solutions; (ii) those that are damped and excited by harmonic excitations, but their approximate response is expressed in terms of Jacobi <span class="hlt">elliptic</span> functions. Characteristics of the steady-state response are discussed and certain qualitative differences with respect to the classical Duffing oscillator excited harmonically are pointed out. Parametric oscillations of the oscillators excited by an <span class="hlt">elliptic</span>-type forcing are considered as well, and the differences with respect to the stability chart of the classical Mathieu equation are emphasized. The adjustment of the Melnikov method to derive the general condition for the onset of homoclinic bifurcations in a system parametrically excited by an <span class="hlt">elliptic</span>-type forcing is provided and compared with those corresponding to harmonic excitations. Advantages and disadvantages of the use of Jacobi <span class="hlt">elliptic</span> functions in nonlinear oscillatory application problems are discussed and some suggestions for future work are given.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016Ap%26SS.361..303H','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016Ap%26SS.361..303H"><span id="translatedtitle">Quasar redshifts: the <span class="hlt">intrinsic</span> component</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Hansen, Peter M.</p> <p>2016-09-01</p> <p>The large observed redshift of quasars has suggested large cosmological distances and a corresponding enormous energy output to explain the brightness or luminosity as seen at earth. Alternative or complementary sources of redshift have not been identified by the astronomical community. This study examines one possible source of additional redshift: an <span class="hlt">intrinsic</span> component based on the plasma characteristics of high temperature and high electron density which are believed to be present.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=5362738','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=5362738"><span id="translatedtitle">Sessile Nanodroplets on <span class="hlt">Elliptical</span> Patches of Enhanced Lyophilicity</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p></p> <p>2017-01-01</p> <p>We theoretically investigate the shape of a nanodroplet on a lyophilic <span class="hlt">elliptical</span> patch in lyophobic surroundings on a flat substrate. To compute the droplet equilibrium shape, we minimize its interfacial free energy using both Surface Evolver and Monte Carlo calculations, finding good agreement between the two methods. We observe different droplet shapes, which are controlled by the droplet volume and the aspect ratio of the ellipse. In particular, we study the behavior of the nanodroplet contact angle along the three-phase contact line, explaining the different droplet shapes. Although the nanodroplet contact angle is constant and fixed by Young’s law inside and outside the <span class="hlt">elliptical</span> patch, its value varies along the rim of the <span class="hlt">elliptical</span> patch. We find that because of the pinning of the nanodroplet contact line at the rim of the <span class="hlt">elliptical</span> patch, which has a nonconstant curvature, there is a regime of aspect ratios of the <span class="hlt">elliptical</span> patch in which the nanodroplet starts expanding to the lyophobic part of the substrate, although there is still a finite area of the lyophilic patch free to be wetted. PMID:28248114</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19930092359','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19930092359"><span id="translatedtitle"><span class="hlt">Elliptic</span> Cones Alone and with Wings at Supersonic Speed</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Jorgensen, Leland H</p> <p>1958-01-01</p> <p>To help fill the gap in the knowledge of aerodynamics of shapes intermediate between bodies of revolution and flat triangular wings, force and moment characteristics for <span class="hlt">elliptic</span> cones have been experimentally determined for Mach numbers of 1.97 and 2.94. <span class="hlt">Elliptic</span> cones having cross-sectional axis ratios from 1 through 6 and with lengths and base areas equal to circular cones of fineness ratios 3.67 and 5 have been studied for angles of bank of 0 degree and 90 degrees. <span class="hlt">Elliptic</span> and circular cones in combination with triangular wings of aspect ratios 1 and 1.5 also have been considered. The angle-of-attack range was from 0 degree to about 16 degrees, and the Reynolds number was 8 x 10(6), based on model length. In addition to the forces and moments at angle of attack, pressure distributions for <span class="hlt">elliptic</span> cones at zero angle of attack have been determined. The results of this investigation indicate that there are distinct aerodynamic advantages to the use of <span class="hlt">elliptic</span> cones.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2004cosp...35.4682U','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2004cosp...35.4682U"><span id="translatedtitle">Observations On The Stability Of <span class="hlt">Elliptical</span> Liquid Bridges</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Uguz, A.</p> <p></p> <p>A liquid bridge is a region of liquid suspended between two solids. These bridges occur within natural and technological contexts. For long enough cylinders in zero gravity, the bridge collapses at what is known as the Plateau limit, i.e. the bridge becomes unstable when its length exceeds its circumference. This limit is reached when there is a balance between the stabilization effect of longitudinal curvature and the destabilization effect caused by transverse curvature. In this presentation, the effect of distortion of the circular end plates to the nearby <span class="hlt">elliptical</span> ones is studied. The circular disks can be distorted to an ellipse by many ways: usually by either keeping the area of the circle constant, or by keeping the perimeter constant, which determines the shape of the <span class="hlt">elliptical</span> liquid bridge. Our aim is to find out the critical length of a static <span class="hlt">elliptical</span> liquid bridge where the bridge collapses and compare it with the critical length of a cylindrical bridge by requiring that the volume of the <span class="hlt">elliptical</span> bridge suspended between the plates 'L' apart be equal to the volume of the nearby right circular. An analytical expression is given that will let us conclude that an <span class="hlt">elliptical</span> liquid bridge is more stable than a circular one. In addition different results will be obtained for different operating conditions and these will be discussed.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2011PhDT.......233G','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2011PhDT.......233G"><span id="translatedtitle"><span class="hlt">Elliptic</span> Boundary Value Problems On Non-Smooth Domains</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Geng, Jun</p> <p>2011-07-01</p> <p>In this dissertation we study the Lp Neumann boundary problem for Laplace's equation in convex domains and the W1,p estimates for the second order <span class="hlt">elliptic</span> equations with Neumann boundary data in Lipschitz domains. We also study the uniform W1, p estimates for homogenization of <span class="hlt">elliptic</span> systems. In the case of convex domains we are able to show that the Lp Neumann problem for Laplace's equation is uniquely solvable for 1 < p < infinity. In the case of second order <span class="hlt">elliptic</span> equations in Lipschitz domains, for any fixed p > 2, we prove that a weak reverse Holder inequality implies the W1, p estimates for solutions with Neumann boundary conditions. As a result, we are able to show that if the coefficient matrix for <span class="hlt">elliptic</span> equation is symmetric and in VMO( Rn ), the W1,p estimates hold for 32 -- epsilon < p < 3 + epsilon if n ≥ 3, and for 43 -- epsilon < p < 4 + epsilon if n = 2. Finally, we show that the uniform W 1,p estimates for homogenization of <span class="hlt">elliptic</span> systems hold when | 1p -- 1/2| < 12n + delta. KEYWORDS: Lipschitz domains; convex domains; Neumann problem; Dirichlet problem; Homogenization problem</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/27936491','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/27936491"><span id="translatedtitle"><span class="hlt">Intrinsic</span> α helix propensities compact hydrodynamic radii in <span class="hlt">intrinsically</span> disordered proteins.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>English, Lance R; Tilton, Erin C; Ricard, Benjamin J; Whitten, Steven T</p> <p>2017-02-01</p> <p>Proteins that lack tertiary stability under normal conditions, known as <span class="hlt">intrinsically</span> disordered, exhibit a wide range of biological activities. Molecular descriptions for the biology of <span class="hlt">intrinsically</span> disordered proteins (IDPs) consequently rely on disordered structural models, which in turn require experiments that assess the origins to structural features observed. For example, while hydrodynamic size is mostly insensitive to sequence composition in chemically denatured proteins, IDPs show strong sequence-specific effects in the hydrodynamic radius (Rh ) when measured under normal conditions. To investigate sequence-modulation of IDP Rh , disordered ensembles generated by a hard sphere collision model modified with a structure-based parameterization of the solution energetics were used to parse the contributions of net charge, main chain dihedral angle bias, and excluded volume on hydrodynamic size. Ensembles for polypeptides 10-35 residues in length were then used to establish power-law scaling relationships for comparison to experimental Rh from 26 IDPs. Results showed the expected outcomes of increased hydrodynamic size from increases in excluded volume and net charge, and compaction from chain-solvent interactions. Chain bias representing <span class="hlt">intrinsic</span> preferences for α helix and polyproline II (PPII ), however, modulated Rh with intricate dependence on the simulated propensities. PPII propensities at levels expected in IDPs <span class="hlt">correlated</span> with heightened Rh sensitivity to even weak α helix propensities, indicating bias for common (φ, ψ) are important determinants of hydrodynamic size. Moreover, data show that IDP Rh can be predicted from sequence with good accuracy from a small set of physicochemical properties, namely <span class="hlt">intrinsic</span> conformational propensities and net charge. Proteins 2017; 85:296-311. © 2016 Wiley Periodicals, Inc.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19930067320&hterms=phenomenon+child&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D20%26Ntt%3Dphenomenon%2Bchild','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19930067320&hterms=phenomenon+child&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D20%26Ntt%3Dphenomenon%2Bchild"><span id="translatedtitle">Precession and circularization of <span class="hlt">elliptical</span> space-tether motion</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Chapel, Jim D.; Grosserode, Patrick</p> <p>1993-01-01</p> <p>In this paper, we present a simplified analytic model for predicting motion of long space tethers. The perturbation model developed here addresses skip rope motion, where each end of the tether is held in place and the middle of the tether swings with a motion similar to that of a child's skip rope. If the motion of the tether midpoint is <span class="hlt">elliptical</span> rather than circular, precession of the ellipse complicates the procedures required to damp this motion. The simplified analytic model developed in this paper parametrically predicts the precession of <span class="hlt">elliptical</span> skip rope motion. Furthermore, the model shows that <span class="hlt">elliptic</span> skip rope motion will circularize when damping is present in the longitudinal direction. Compared with high-fidelity simulation results, this simplified model provides excellent predictions of these phenomena.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/20953283','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/20953283"><span id="translatedtitle">System Size, Energy, Pseudorapidity, and Centrality Dependence of <span class="hlt">Elliptic</span> Flow</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Alver, B.; Ballintijn, M.; Busza, W.; Decowski, M. P.; Gulbrandsen, K.; Henderson, C.; Kane, J. L.; Kulinich, P.; Li, W.; Loizides, C.; Reed, C.; Roland, C.; Roland, G.; Stephans, G. S. F.; Vale, C.; Nieuwenhuizen, G. J. van; Vaurynovich, S. S.; Verdier, R.; Veres, G. I.; Wenger, E.</p> <p>2007-06-15</p> <p>This Letter presents measurements of the <span class="hlt">elliptic</span> flow of charged particles as a function of pseudorapidity and centrality from Cu-Cu collisions at 62.4 and 200 GeV using the PHOBOS detector at the Relativistic Heavy Ion Collider. The <span class="hlt">elliptic</span> flow in Cu-Cu collisions is found to be significant even for the most central events. For comparison with the Au-Au results, it is found that the detailed way in which the collision geometry (eccentricity) is estimated is of critical importance when scaling out system-size effects. A new form of eccentricity, called the participant eccentricity, is introduced which yields a scaled <span class="hlt">elliptic</span> flow in the Cu-Cu system that has the same relative magnitude and qualitative features as that in the Au-Au system.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19880040839&hterms=Radius&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D10%26Ntt%3DA.%2BRadius','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19880040839&hterms=Radius&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D10%26Ntt%3DA.%2BRadius"><span id="translatedtitle">Mass distributions in <span class="hlt">elliptical</span> galaxies at large radii</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Sarazin, Craig L.</p> <p>1987-01-01</p> <p>Recently, X-ray observations have shown that <span class="hlt">elliptical</span> galaxies generally contain large quantities of hot gas. Central dominant cluster <span class="hlt">ellipticals</span> have even more gas, which they have accreted from the surrounding clusters. The mass distributions in these galaxies can be derived from the condition of hydrostatic equilibrium. M87, the best studied central dominant galaxy, has a massive, dark halo with a total mass of about 4 x 10 to the 12th solar masses within a radius of 300 kpc. The total mass-to-light ratio within this radius is at least 150 solar mass/solar luminosity. The X-ray observations of normal <span class="hlt">ellipticals</span> also strongly suggest that they have heavy halos, although the distribution of the mass is much less certain than in M87.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/23410439','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/23410439"><span id="translatedtitle">Evolution of a barotropic shear layer into <span class="hlt">elliptical</span> vortices.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Guha, Anirban; Rahmani, Mona; Lawrence, Gregory A</p> <p>2013-01-01</p> <p>When a barotropic shear layer becomes unstable, it produces the well-known Kelvin-Helmholtz instability (KHI). The nonlinear manifestation of the KHI is usually in the form of spiral billows. However, a piecewise linear shear layer produces a different type of KHI characterized by <span class="hlt">elliptical</span> vortices of constant vorticity connected via thin braids. Using direct numerical simulation and contour dynamics, we show that the interaction between two counterpropagating vorticity waves is solely responsible for this KHI formation. We investigate the oscillation of the vorticity wave amplitude, the rotation and nutation of the <span class="hlt">elliptical</span> vortex, and straining of the braids. Our analysis also provides a possible explanation for the formation and evolution of <span class="hlt">elliptical</span> vortices appearing in geophysical and astrophysical flows, e.g., meddies, stratospheric polar vortices, Jovian vortices, Neptune's Great Dark Spot, and coherent vortices in the wind belts of Uranus.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19820041687&hterms=industrial+Revolution&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D30%26Ntt%3Dindustrial%2BRevolution','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19820041687&hterms=industrial+Revolution&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D30%26Ntt%3Dindustrial%2BRevolution"><span id="translatedtitle">Ball bearing lubrication: The elastohydrodynamics of <span class="hlt">elliptical</span> contacts</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Hamrock, B. J.; Dowson, D.</p> <p>1981-01-01</p> <p>The history of ball bearings is examined, taking into account rollers and the wheel in the early civilizations, the development of early forms of rolling-element bearings in the classical civilizations, the Middle Ages, the Industrial Revolution, the emergence of the precision ball bearing, scientific studies of contact mechanics and rolling friction, and the past fifty years. An introduction to ball bearings is presented, and aspects of ball bearing mechanics are explored. Basic characteristics of lubrication are considered along with lubrication equations, the lubrication of rigid ellipsoidal solids, and elastohydrodynamic lubrication theory. Attention is given to the theoretical results for fully flooded <span class="hlt">elliptical</span> hydrodynamic contacts, the theoretical results for starved <span class="hlt">elliptical</span> contacts, experimental investigations, the elastohydrodynamics of <span class="hlt">elliptical</span> contacts for materials of low elastic modulus, the film thickness for different regimes of fluid-film lubrication, and applications.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19960049876&hterms=boerstoel&qs=N%3D0%26Ntk%3DAuthor-Name%26Ntx%3Dmode%2Bmatchall%26Ntt%3Dboerstoel','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19960049876&hterms=boerstoel&qs=N%3D0%26Ntk%3DAuthor-Name%26Ntx%3Dmode%2Bmatchall%26Ntt%3Dboerstoel"><span id="translatedtitle"><span class="hlt">Elliptic</span> surface grid generation on minimal and parametrized surfaces</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Spekreijse, S. P.; Nijhuis, G. H.; Boerstoel, J. W.</p> <p>1995-01-01</p> <p>An <span class="hlt">elliptic</span> grid generation method, which generates boundary conforming grids in a two dimensional physical space, is presented. The method is based on the composition of an algebraic and <span class="hlt">elliptic</span> transformation. The composite mapping obeys the Poisson grid generation system with control functions specified by the algebraic transformation. It is shown that the grid generation on a minimal surface in a three dimensional space is equivalent to the grid generation in a two dimensional domain in physical space. A second <span class="hlt">elliptic</span> grid generation method, which generates boundary conforming grids on smooth surfaces, is presented. Concerning surface modeling, it is shown that bicubic Hermit interpolation is an excellent method to generate a smooth surface crossing a discrete set of control points.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19920011130','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19920011130"><span id="translatedtitle"><span class="hlt">Elliptic</span> jets, part 2. Dynamics of coherent structures: Pairing</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Husain, Hyder S.; Hussain, Fazle</p> <p>1992-01-01</p> <p>The dynamics of the jet column mode of vortex pairing in the near field of an <span class="hlt">elliptic</span> jet was investigated. Hot-wire measurements and flow visualization were used to examine the details of the pairing mechanism of nonplanar vortical <span class="hlt">elliptic</span> structures and its effect on such turbulence measures as coherent velocities, incoherent turbulence intensities, incoherent and coherent Reynolds, stresses, turbulence production, and mass entrainment. It was found that pairing of <span class="hlt">elliptic</span> vortices in the jet column does not occur uniformly around the entire perimeter, unlike in a circular jet. Merger occurs only in the initial major-axis plane. In the initial minor-axis plane, the trailing vortex rushes through the leading vortex without pairing and then breaks down violently, producing considerably greater entrainment and mixing than in circular or plane jets.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016PhyD..315....1F','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016PhyD..315....1F"><span id="translatedtitle">Polar rotation angle identifies <span class="hlt">elliptic</span> islands in unsteady dynamical systems</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Farazmand, Mohammad; Haller, George</p> <p>2016-02-01</p> <p>We propose rotation inferred from the polar decomposition of the flow gradient as a diagnostic for <span class="hlt">elliptic</span> (or vortex-type) invariant regions in non-autonomous dynamical systems. We consider here two- and three-dimensional systems, in which polar rotation can be characterized by a single angle. For this polar rotation angle (PRA), we derive explicit formulas using the singular values and vectors of the flow gradient. We find that closed level sets of the PRA reveal <span class="hlt">elliptic</span> islands in great detail, and singular level sets of the PRA uncover centers of such islands. Both features turn out to be objective (frame-invariant) for two-dimensional systems. We illustrate the diagnostic power of PRA for <span class="hlt">elliptic</span> structures on several examples.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2011OptCo.284..282W','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2011OptCo.284..282W"><span id="translatedtitle">Nonclassical properties of odd and even <span class="hlt">elliptical</span> states</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Wang, Yueyuan; Liao, Qinghong; Liu, Zhengjun; Wang, Jicheng; Liu, Shutian</p> <p>2011-01-01</p> <p>As a generalization of the optical circular states, <span class="hlt">elliptical</span> states which are quantum superposition of coherent states on an ellipse in the α plane are constructed. The statistical properties of the states are investigated by using sub-Poissonian photon statistics, quadrature squeezing, Wigner function and phase distribution. It is shown that the <span class="hlt">elliptical</span> states exhibit stronger quadrature squeezing. The interference fringes between the coherent states form the <span class="hlt">elliptic</span> annuli of Fock states in the Wigner function picture. The phase distribution is no longer uniform as the circular states. An experimental scheme is proposed for generating equidistant coherent-state superpositions on an ellipse for the motion of the center of mass of a trapped ion.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/27627309','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/27627309"><span id="translatedtitle">Dynamical properties of the soft-wall <span class="hlt">elliptical</span> billiard.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Kroetz, Tiago; Oliveira, Hércules A; Portela, Jefferson S E; Viana, Ricardo L</p> <p>2016-08-01</p> <p>Physical systems such as optical traps and microwave cavities are realistically modeled by billiards with soft walls. In order to investigate the influence of the wall softness on the billiard dynamics, we study numerically a smooth two-dimensional potential well that has the <span class="hlt">elliptical</span> (hard-wall) billiard as a limiting case. Considering two parameters, the eccentricity of the <span class="hlt">elliptical</span> equipotential curves and the wall hardness, which defines the steepness of the well, we show that (1) whereas the hard-wall limit is integrable and thus completely regular, the soft wall <span class="hlt">elliptical</span> billiard exhibits chaos, (2) the chaotic fraction of the phase space depends nonmonotonically on the hardness of the wall, and (3) the effect of the hardness on the dynamics depends strongly on the eccentricity of the billiard. We further show that the limaçon billiard can exhibit enhanced chaos induced by wall softness, which suggests that our findings generalize to quasi-integrable systems.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016CeMDA.125..383X','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016CeMDA.125..383X"><span id="translatedtitle">Cluster flight control for fractionated spacecraft on an <span class="hlt">elliptic</span> orbit</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Xu, Ming; Liang, Yuying; Tan, Tian; Wei, Lixin</p> <p>2016-08-01</p> <p>This paper deals with the stabilization of cluster flight on an <span class="hlt">elliptic</span> reference orbit by the Hamiltonian structure-preserving control using the relative position measurement only. The linearized Melton's relative equation is utilized to derive the controller and then the full nonlinear relative dynamics are employed to numerically evaluate the controller's performance. In this paper, the hyperbolic and <span class="hlt">elliptic</span> eigenvalues and their manifolds are treated without distinction notations. This new treatment not only contributes to solving the difficulty in feedback of the unfixed-dimensional manifolds, but also allows more opportunities to set the controlled frequencies of foundational motions or to optimize control gains. Any initial condition can be stabilized on a Kolmogorov-Arnold-Moser torus near a controlled <span class="hlt">elliptic</span> equilibrium. The motions are stabilized around the natural relative trajectories rather than track a reference relative configuration. In addition, the bounded quasi-periodic trajectories generated by the controller have advantages in rapid reconfiguration and unpredictable evolution.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/22158244','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/22158244"><span id="translatedtitle">Two ten-billion-solar-mass black holes at the centres of giant <span class="hlt">elliptical</span> galaxies.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>McConnell, Nicholas J; Ma, Chung-Pei; Gebhardt, Karl; Wright, Shelley A; Murphy, Jeremy D; Lauer, Tod R; Graham, James R; Richstone, Douglas O</p> <p>2011-12-08</p> <p>Observational work conducted over the past few decades indicates that all massive galaxies have supermassive black holes at their centres. Although the luminosities and brightness fluctuations of quasars in the early Universe suggest that some were powered by black holes with masses greater than 10 billion solar masses, the remnants of these objects have not been found in the nearby Universe. The giant <span class="hlt">elliptical</span> galaxy Messier 87 hosts the hitherto most massive known black hole, which has a mass of 6.3 billion solar masses. Here we report that NGC 3842, the brightest galaxy in a cluster at a distance from Earth of 98 megaparsecs, has a central black hole with a mass of 9.7 billion solar masses, and that a black hole of comparable or greater mass is present in NGC 4889, the brightest galaxy in the Coma cluster (at a distance of 103 megaparsecs). These two black holes are significantly more massive than predicted by linearly extrapolating the widely used <span class="hlt">correlations</span> between black-hole mass and the stellar velocity dispersion or bulge luminosity of the host galaxy. Although these <span class="hlt">correlations</span> remain useful for predicting black-hole masses in less massive <span class="hlt">elliptical</span> galaxies, our measurements suggest that different evolutionary processes influence the growth of the largest galaxies and their black holes.</p> </li> </ol> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_12");'>12</a></li> <li><a href="#" onclick='return showDiv("page_13");'>13</a></li> <li class="active"><span>14</span></li> <li><a href="#" onclick='return showDiv("page_15");'>15</a></li> <li><a href="#" onclick='return showDiv("page_16");'>16</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div><!-- col-sm-12 --> </div><!-- row --> </div><!-- page_14 --> <div id="page_15" class="hiddenDiv"> <div class="row"> <div class="col-sm-12"> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_13");'>13</a></li> <li><a href="#" onclick='return showDiv("page_14");'>14</a></li> <li class="active"><span>15</span></li> <li><a href="#" onclick='return showDiv("page_16");'>16</a></li> <li><a href="#" onclick='return showDiv("page_17");'>17</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div> </div> <div class="row"> <div class="col-sm-12"> <ol class="result-class" start="281"> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017AAS...22911405A','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017AAS...22911405A"><span id="translatedtitle">Measuring the extent of x-ray emitting hot gas haloes around <span class="hlt">elliptical</span> galaxies</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Alpaslan, Mehmet; Marcum, Pamela M.</p> <p>2017-01-01</p> <p>The hot, x-ray emitting gas halos around galaxies can serve as tracers of previous merger history, and provide insight into the formation processes of <span class="hlt">elliptical</span> galaxies. In order to better understand the relationship between a galaxy's local environment and its x-ray emitting hot gas corona, we examine the x-ray emission from 117 early type galaxies selected from SDSS DR12 that have been observed with Chandra's ACIS detector. We have developed a new methodology for determining the effective and Petrosian radii of the x-ray emission from the hot coronae of these galaxies, and with it find a positive <span class="hlt">correlation</span> between fifth nearest neighbour density and corona size. Notably, we do not see a corresponding <span class="hlt">correlation</span> between size and other galaxy properties such as mass, r-band Petrosian radius, and metallicity. These results suggest that the physical processes that drive the extension of the hot gas halo do not significantly influence the stellar content of the <span class="hlt">elliptical</span> galaxy.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2006GApFD.100..299L','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2006GApFD.100..299L"><span id="translatedtitle">Magnetic field induced by <span class="hlt">elliptical</span> instability in a rotating spheroid</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Lacaze, L.; Herreman, W.; Le Bars, M.; Le Dizès, S.; Le Gal, P.</p> <p>2006-10-01</p> <p>The tidal or the <span class="hlt">elliptical</span> instability of the rotating fluid flows is generated by the resonant interaction of the inertial waves. In a slightly <span class="hlt">elliptically</span> deformed rotating sphere, the most unstable linear mode is called the spin-over mode, and is a solid body rotation versus an axis aligned with the maximum strain direction. In the non-viscous case, this instability corresponds to the median moment of the inertial instability of the solid rotating bodies. This analogy is furthermore illustrated by an <span class="hlt">elliptical</span> top experiment, which shows the expected inviscid heteroclinic behaviour. In geophysics, the <span class="hlt">elliptical</span> instability may appear in the molten liquid cores of the rotating planets, which are slightly deformed by the tidal gravitational effects of the close bodies. It may then participate in the general outer core dynamics and possibly the geodynamo process. In this context, Kerswell and Malkus (Kerswell, R.R. and Malkus, W.V.R., Tidal instability as the source for Io's magnetic signature. Geophys. Res. Lett., 1998, 25, 603 606) showed that the puzzling magnetic field of the Jovian satellite Io may indeed be induced by the <span class="hlt">elliptically</span> unstable motions of its liquid core that deflect the Jupiter's magnetic field. Our magnetohydrodynamics (MHD) experiment is a toy-experiment of this geophysical situation and demonstrates for the first time the possibility of an induction of a magnetic field by the flow motions due to the <span class="hlt">elliptical</span> instability. A full analytical calculation of the magnetic dipole induced by the spin-over is presented. Finally, exponential growths of this induced magnetic field in a slightly deformed rotating sphere filled with galinstan liquid metal are measured for different rotating rates. Their growth rates compare well with the theoretical predictions in the limit of a vanishing Lorentz force.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2011MNRAS.410..280J','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2011MNRAS.410..280J"><span id="translatedtitle">The colour-magnitude relation of <span class="hlt">elliptical</span> and lenticular galaxies in the ESO Distant Cluster Survey</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Jaffé, Yara L.; Aragón-Salamanca, Alfonso; De Lucia, Gabriella; Jablonka, Pascale; Rudnick, Gregory; Saglia, Roberto; Zaritsky, Dennis</p> <p>2011-01-01</p> <p>In this paper we study the colour-magnitude relation (CMR) for a sample of 172 morphologically classified <span class="hlt">elliptical</span> and S0 cluster galaxies from the ESO Distant Cluster Survey (EDisCS) at 0.4 ≲z≲ 0.8. The <span class="hlt">intrinsic</span> colour scatter about the CMR is very small (<σint>= 0.076) in rest-frame U-V. However, there is a small minority of faint early-type galaxies (7 per cent) that are significantly bluer than the CMR. We observe no significant dependence of σint with redshift or cluster velocity dispersion. Because our sample is strictly morphologically selected, this implies that by the time cluster <span class="hlt">elliptical</span> and S0 galaxies achieve their morphology, the vast majority have already joined the red sequence. The only exception seems to be the very small fraction of faint blue early types. Assuming that the <span class="hlt">intrinsic</span> colour scatter is due to differences in stellar population ages, we estimate the galaxy formation redshift zF of each cluster and find that zF does not depend on the cluster velocity dispersion. However, zF increases weakly with cluster redshift within the EDisCS sample. This trend becomes very clear when higher redshift clusters from the literature are included. This suggests that, at any given redshift, in order to have a population of fully formed <span class="hlt">ellipticals</span> and S0s they needed to have formed most of their stars ≃2-4 Gyr prior to observation. That does not mean that all early-type galaxies in all clusters formed at these high redshifts. It means that the ones we see already having early-type morphologies also have reasonably old stellar populations. This is partly a manifestation of the `progenitor bias', but also a consequence of the fact that the vast majority of the early-type galaxies in clusters (in particular the massive galaxies) were already red (i.e. already had old stellar populations) by the time they achieved their morphology. <span class="hlt">Elliptical</span> and S0 galaxies exhibit very similar colour scatter, implying similar stellar population ages. The</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/1998IAUS..191P.530V','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/1998IAUS..191P.530V"><span id="translatedtitle">Extrinsic and <span class="hlt">intrinsic</span> S stars in the Henize sample</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Van Eck, Sophie; Jorissen, Alain; Mayor, Michel; Udry, Stephane; Burnet, Michel</p> <p></p> <p>Previous studies have identified two distinct families among S stars: <span class="hlt">intrinsic</span> S stars exhibiting Tc lines in their spectrum, and extrinsic S stars lacking Tc lines. Extrinsic S stars were found to be binaries, and probably owe their chemical peculiarities to mass transfer in the binary system. On the contrary, <span class="hlt">intrinsic</span> S stars are thermally-pulsating AGB stars where the third dredge-up brought heavy elements to the surface. The Henize sample of 205 S stars south of declination -25^circ is especially well suited for inferring the relative frequency of extrinsic/<span class="hlt">intrinsic</span> S stars, since it is not biased towards low galactic latitudes where <span class="hlt">intrinsic</span> S stars tend to concentrate. Each star has been measured 3 or 4 times over a period of 5 years with the spectrovelocimeter CORAVEL. The search for binaries is complicated by the fact that Mira-type pulsations are frequent among <span class="hlt">intrinsic</span> S stars. Fortunately, radial-velocity variations due to atmospheric motions are generally associated with very broad and asymmetric CORAVEL cross-<span class="hlt">correlation</span> profiles [see also poster P2-14!]. Therefore extrinsic and <span class="hlt">intrinsic</span> S stars can be distinguished thanks to (1) radial velocity variations, (2) the shape of the CORAVEL cross-<span class="hlt">correlation</span> profiles, (3) the presence or absence of the radioactive element Tc, as derived from high-resolution spectroscopy, (4) photometric variability, as derived from a survey in the Geneva photometric system. These criteria <span class="hlt">correlate</span> in a nice way and allow to derive the frequency of <span class="hlt">intrinsic</span>-genuine AGB-S stars. The galactic distributions of the two families of S stars are clearly distinct, <span class="hlt">intrinsic</span> S stars being much more concentrated along the galactic plane that extrinsic S stars. High-resolution spectroscopy led to the discovery of two symbiotic stars among the Henize sample (symbiotic stars are interacting binary systems in which a hot compact object accretes matter ejected by a cool (super)giant). The physical parameters responsible for the</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/925292','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/925292"><span id="translatedtitle"><span class="hlt">Elliptic</span> flow in Au+Au collisions at RHIC.</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Back, B. B.; Baker, M. D.; Ballintijn, M.; Barton, D. S.; Betts, R. R.; George, N.; Wuosmaa, A.; Physics; Massachusetts Inst. of Tech.; BNL; Univ. of Illinois at Chicago</p> <p>2005-01-01</p> <p><span class="hlt">Elliptic</span> flow is an interesting probe of the dynamical evolution of the dense system formed in the ultrarelativistic heavy ion collisions at the relativistic heavy ion collider (RHIC). The <span class="hlt">elliptic</span> flow dependences on transverse momentum, centrality and pseudorapidity were measured using data collected by the PHOBOS detector, which offers a unique opportunity to study the azimuthal anisotropies of charged particles over a wide range of pseudorapidity. These measurements are presented, together with an overview of the analysis methods and a discussion of the results.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/pages/biblio/1197880-plastic-deformation-profile-coated-elliptical-kb-mirrors','SCIGOV-DOEP'); return false;" href="https://www.osti.gov/pages/biblio/1197880-plastic-deformation-profile-coated-elliptical-kb-mirrors"><span id="translatedtitle">Plastic Deformation in Profile-Coated <span class="hlt">Elliptical</span> KB Mirrors</span></a></p> <p><a target="_blank" href="http://www.osti.gov/pages">DOE PAGES</a></p> <p>Liu, Chian; Conley, R.; Qian, J.; ...</p> <p>2012-01-01</p> <p>Profile coating has been successfully applied to produce <span class="hlt">elliptical</span> Kirkpatrick-Baez (KB) mirrors using both cylindrical and flat Si substrates. Previously, focusing widths of 70 nm with 15-keV monochromatic and 80 nm with white beam were achieved using a flat Si substrate. Now, precision <span class="hlt">elliptical</span> KB mirrors with sub-nm figure errors are produced with both Au and Pt coatings on flat substrates. Recent studies of bare Si-, Au-, and Pt-coated KB mirrors under prolonged synchrotron X-ray radiation and low-temperature vacuum annealing will be discussed in terms of film stress relaxation and Si plastic deformation.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2003PhRvL..90l4501F','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2003PhRvL..90l4501F"><span id="translatedtitle">Mean Effects of Turbulence on <span class="hlt">Elliptic</span> Instability in Fluids</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Fabijonas, Bruce R.; Holm, Darryl D.</p> <p>2003-03-01</p> <p><span class="hlt">Elliptic</span> instability in fluids is discussed in the context of the Lagrangian-averaged Navier-Stokes-alpha (LANS-α) turbulence model. This model preserves the Craik-Criminale (CC) family of solutions consisting of a columnar eddy and a Kelvin wave. The LANS-α model is shown to preserve <span class="hlt">elliptic</span> instability. However, the model shifts the critical stability angle. This shift increases (decreases) the maximum growth rate for long (short) waves. It also introduces a band of stable CC solutions for short waves.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19920012389','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19920012389"><span id="translatedtitle"><span class="hlt">Elliptical</span> flux vortices in YBa2Cu3O7</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Hickman, H.; Dekker, A. J.; Chen, T. M.</p> <p>1991-01-01</p> <p>The most energetically favorable vortex in YBa2Cu3O7 forms perpendicular to an anisotropic plane. This vortex is <span class="hlt">elliptical</span> in shape and is distinguished by an effective interchange of London penetration depths from one axis of the ellipse to another. By generalizing qualitatively from the isotropic to the anisotropic case, we suggest that the flux flow resistivity for the vortex that forms perpendicular to an anistropic plane should have a preferred direction. Similar reasoning indicates that the Kosterlitz-Thouless transition temperature for a vortex mediated transition should be lower if the vortex is <span class="hlt">elliptical</span> in shape.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19930091699','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19930091699"><span id="translatedtitle">Two-dimensional subsonic compressible flow past <span class="hlt">elliptic</span> cylinders</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Kaplan, Carl</p> <p>1938-01-01</p> <p>The method of Poggi is used to calculate, for perfect fluids, the effect of compressibility upon the flow on the surface of an <span class="hlt">elliptic</span> cylinder at zero angle of attack and with no circulation. The result is expressed in a closed form and represents a rigorous determination of the velocity of the fluid at the surface of the obstacle insofar as the second approximation is concerned. Comparison is made with Hooker's treatment of the same problem according to the method of Janzen and Rayleight and it is found that, for thick <span class="hlt">elliptic</span> cylinders, the two methods agree very well. The labor of computation is considerably reduced by the present solution.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016PhRvE..94b2210T','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016PhRvE..94b2210T"><span id="translatedtitle"><span class="hlt">Intrinsic</span> periodic and aperiodic stochastic resonance in an electrochemical cell</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Tiwari, Ishant; Phogat, Richa; Parmananda, P.; Ocampo-Espindola, J. L.; Rivera, M.</p> <p>2016-08-01</p> <p>In this paper we show the interaction of a composite of a periodic or aperiodic signal and <span class="hlt">intrinsic</span> electrochemical noise with the nonlinear dynamics of an electrochemical cell configured to study the corrosion of iron in an acidic media. The anodic voltage setpoint (V0) in the cell is chosen such that the anodic current (I ) exhibits excitable fixed point behavior in the absence of noise. The subthreshold periodic (aperiodic) signal consists of a train of rectangular pulses with a fixed amplitude and width, separated by regular (irregular) time intervals. The irregular time intervals chosen are of deterministic and stochastic origins. The amplitude of the <span class="hlt">intrinsic</span> internal noise, regulated by the concentration of chloride ions, is then monotonically increased, and the provoked dynamics are analyzed. The signal to noise ratio and the cross-<span class="hlt">correlation</span> coefficient versus the chloride ions' concentration curves have a unimodal shape indicating the emergence of an <span class="hlt">intrinsic</span> periodic or aperiodic stochastic resonance. The abscissa for the maxima of these unimodal curves correspond to the optimum value of <span class="hlt">intrinsic</span> noise where maximum regularity of the invoked dynamics is observed. In the particular case of the <span class="hlt">intrinsic</span> periodic stochastic resonance, the scanning electron microscope images for the electrode metal surfaces are shown for certain values of chloride ions' concentrations. These images, qualitatively, corroborate the emergence of order as a result of the interaction between the nonlinear dynamics and the composite signal.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/26386901','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/26386901"><span id="translatedtitle"><span class="hlt">Intrinsic</span> motivation and amotivation in first episode and prolonged psychosis.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Luther, Lauren; Lysaker, Paul H; Firmin, Ruth L; Breier, Alan; Vohs, Jenifer L</p> <p>2015-12-01</p> <p>The deleterious functional implications of motivation deficits in psychosis have generated interest in examining dimensions of the construct. However, there remains a paucity of data regarding whether dimensions of motivation differ over the course of psychosis. Therefore, this study examined two motivation dimensions, trait-like <span class="hlt">intrinsic</span> motivation, and the negative symptom of amotivation, and tested the impact of illness phase on the 1) levels of these dimensions and 2) relationship between these dimensions. Participants with first episode psychosis (FEP; n=40) and prolonged psychosis (n=66) completed clinician-rated measures of <span class="hlt">intrinsic</span> motivation and amotivation. Analyses revealed that when controlling for group differences in gender and education, the FEP group had significantly more <span class="hlt">intrinsic</span> motivation and lower amotivation than the prolonged psychosis group. Moreover, <span class="hlt">intrinsic</span> motivation was negatively <span class="hlt">correlated</span> with amotivation in both FEP and prolonged psychosis, but the magnitude of the relationship did not statistically differ between groups. These findings suggest that motivation deficits are more severe later in the course of psychosis and that low <span class="hlt">intrinsic</span> motivation may be partially independent of amotivation in both first episode and prolonged psychosis. Clinically, these results highlight the importance of targeting motivation in early intervention services.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/22369861','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/22369861"><span id="translatedtitle">Cosmological information in the <span class="hlt">intrinsic</span> alignments of luminous red galaxies</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Chisari, Nora Elisa; Dvorkin, Cora E-mail: cdvorkin@ias.edu</p> <p>2013-12-01</p> <p>The <span class="hlt">intrinsic</span> alignments of galaxies are usually regarded as a contaminant to weak gravitational lensing observables. The alignment of Luminous Red Galaxies, detected unambiguously in observations from the Sloan Digital Sky Survey, can be reproduced by the linear tidal alignment model of Catelan, Kamionkowski and Blandford (2001) on large scales. In this work, we explore the cosmological information encoded in the <span class="hlt">intrinsic</span> alignments of red galaxies. We make forecasts for the ability of current and future spectroscopic surveys to constrain local primordial non-Gaussianity and Baryon Acoustic Oscillations (BAO) in the cross-<span class="hlt">correlation</span> function of <span class="hlt">intrinsic</span> alignments and the galaxy density field. For the Baryon Oscillation Spectroscopic Survey, we find that the BAO signal in the <span class="hlt">intrinsic</span> alignments is marginally significant with a signal-to-noise ratio of 1.8 and 2.2 with the current LOWZ and CMASS samples of galaxies, respectively, and increasing to 2.3 and 2.7 once the survey is completed. For the Dark Energy Spectroscopic Instrument and for a spectroscopic survey following the EUCLID redshift selection function, we find signal-to-noise ratios of 12 and 15, respectively. Local type primordial non-Gaussianity, parametrized by f{sub NL} = 10, is only marginally significant in the <span class="hlt">intrinsic</span> alignments signal with signal-to-noise ratios < 2 for the three surveys considered.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/21878781','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/21878781"><span id="translatedtitle"><span class="hlt">Intrinsic</span> motivation as a predictor of work outcome after vocational rehabilitation in schizophrenia.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Saperstein, Alice M; Fiszdon, Joanna M; Bell, Morris D</p> <p>2011-09-01</p> <p><span class="hlt">Intrinsic</span> motivation is a construct commonly used in explaining goal-directed behavior. In people with schizophrenia, <span class="hlt">intrinsic</span> motivation is usually subsumed as a feature of negative symptoms or underlying neurocognitive dysfunction. A growing literature reflects an interest in defining and measuring motivational impairment in schizophrenia and in delineating the specific role of <span class="hlt">intrinsic</span> motivation as both an independent predictor and a mediator of psychosocial functioning. This cross-sectional study examined <span class="hlt">intrinsic</span> motivation as a predictor of vocational outcomes for 145 individuals with schizophrenia and schizoaffective disorder participating in a 6-month work rehabilitation trial. <span class="hlt">Correlation</span> and mediation analyses examined baseline <span class="hlt">intrinsic</span> motivation and negative symptoms in relation to work hours and work performance. Data support a significant relationship between <span class="hlt">intrinsic</span> motivation and negative symptoms and significant <span class="hlt">correlations</span> with outcome variables, such that lower negative symptoms and greater <span class="hlt">intrinsic</span> motivation were associated with better work functioning. Moreover, in this sample, <span class="hlt">intrinsic</span> motivation fully mediated the relationships between negative symptoms, work productivity, and work performance. These results have significant implications on the design of work rehabilitation interventions for people with schizophrenia and support a role for targeting <span class="hlt">intrinsic</span> motivation directly to influence vocational functioning. Future directions for research and intervention are discussed.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/21506758','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/21506758"><span id="translatedtitle">Nuclear Filtering of <span class="hlt">Intrinsic</span> Charm</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Kopeliovich, B. Z.; Potashnikova, I. K.; Schmidt, Ivan</p> <p>2010-11-12</p> <p>Nuclei are transparent for a heavy <span class="hlt">intrinsic</span> charm (IC) component of the beam hadrons, what leads to an enhanced nuclear dependence of open charm production at large Feynman x{sub F}. Indeed, such an effect is supported by data from the SELEX experiment published recently [1]. Our calculations reproduce well the data, providing strong support for the presence of IC in hadrons in amount less than 1%. Moreover, we performed an analysis of nuclear effects in J/{Psi} production and found at large x{sub F} a similar, albeit weaker effect, which does not contradict data.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/25401561','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/25401561"><span id="translatedtitle">Optics <span class="hlt">ellipticity</span> performance of an unobscured off-axis space telescope.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Zeng, Fei; Zhang, Xin; Zhang, Jianping; Shi, Guangwei; Wu, Hongbo</p> <p>2014-10-20</p> <p>With the development of astronomy, more and more attention is paid to the survey of dark matter. Dark matter cannot be seen directly but can be detected by weak gravitational lensing measurement. <span class="hlt">Ellipticity</span> is an important parameter used to define the shape of a galaxy. Galaxy <span class="hlt">ellipticity</span> changes with weak gravitational lensing and nonideal optics. With our design of an unobscured off-axis telescope, we implement the simulation and calculation of optics <span class="hlt">ellipticity</span>. With an accurate model of optics PSF, the characteristic of <span class="hlt">ellipticity</span> is modeled and analyzed. It is shown that with good optical design, the full field <span class="hlt">ellipticity</span> can be quite small. The spatial <span class="hlt">ellipticity</span> change can be modeled by cubic interpolation with very high accuracy. We also modeled the <span class="hlt">ellipticity</span> variance with time and analyzed the tolerance. It is shown that the unobscured off-axis telescope has good <span class="hlt">ellipticity</span> performance and fulfills the requirement of dark matter survey.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/1999MNRAS.309..481L','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/1999MNRAS.309..481L"><span id="translatedtitle">The specific entropy of <span class="hlt">elliptical</span> galaxies: an explanation for profile-shape distance indicators?</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Lima Neto, G. B.; Gerbal, D.; Márquez, I.</p> <p>1999-10-01</p> <p>Dynamical systems in equilibrium have a stationary entropy; we suggest that <span class="hlt">elliptical</span> galaxies, as stellar systems in a stage of quasi-equilibrium, may have in principle a unique specific entropy. This uniqueness, a priori unknown, should be reflected in <span class="hlt">correlations</span> between the fundamental parameters describing the mass (light) distribution in galaxies. Following recent photometrical work on <span class="hlt">elliptical</span> galaxies by Caon et al., Graham & Colless and Prugniel & Simien, we use the Sérsic law to describe the light profile and an analytical approximation to its three-dimensional deprojection. The specific entropy is then calculated, supposing that the galaxy behaves as a spherical, isotropic, one-component system in hydrostatic equilibrium, obeying the ideal-gas equations of state. We predict a relation between the three parameters of the Sérsic law linked to the specific entropy, defining a surface in the parameter space, an `Entropic Plane', by analogy with the well-known Fundamental Plane. We have analysed <span class="hlt">elliptical</span> galaxies in two rich clusters of galaxies (Coma and ABCG 85) and a group of galaxies (associated with NGC 4839, near Coma). We show that, for a given cluster, the galaxies follow closely a relation predicted by the constant specific entropy hypothesis with a typical dispersion (one standard deviation) of 9.5per cent around the mean value of the specific entropy. Moreover, assuming that the specific entropy is also the same for galaxies of different clusters, we are able to derive relative distances between Coma, ABGC 85, and the group of NGC 4839. If the errors are due only to the determination of the specific entropy (about 10per cent), then the error in the relative distance determination should be less than 20per cent for rich clusters. We suggest that the unique specific entropy may provide a physical explanation for the distance indicators based on the Sérsic profile put forward by Young & Currie and recently discussed by Binggeli & Jerjen.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/24606139','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/24606139"><span id="translatedtitle"><span class="hlt">Intrinsically</span> disordered proteins and <span class="hlt">intrinsically</span> disordered protein regions.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Oldfield, Christopher J; Dunker, A Keith</p> <p>2014-01-01</p> <p><span class="hlt">Intrinsically</span> disordered proteins (IDPs) and IDP regions fail to form a stable structure, yet they exhibit biological activities. Their mobile flexibility and structural instability are encoded by their amino acid sequences. They recognize proteins, nucleic acids, and other types of partners; they accelerate interactions and chemical reactions between bound partners; and they help accommodate posttranslational modifications, alternative splicing, protein fusions, and insertions or deletions. Overall, IDP-associated biological activities complement those of structured proteins. Recently, there has been an explosion of studies on IDP regions and their functions, yet the discovery and investigation of these proteins have a long, mostly ignored history. Along with recent discoveries, we present several early examples and the mechanisms by which IDPs contribute to function, which we hope will encourage comprehensive discussion of IDPs and IDP regions in biochemistry textbooks. Finally, we propose future directions for IDP research.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2015CMMPh..55.1290D','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2015CMMPh..55.1290D"><span id="translatedtitle">On an algorithm for solving parabolic and <span class="hlt">elliptic</span> equations</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>D'Ascenzo, N.; Saveliev, V. I.; Chetverushkin, B. N.</p> <p>2015-08-01</p> <p>The present-day rapid growth of computer power, in particular, parallel computing systems of ultrahigh performance requires a new approach to the creation of models and solution algorithms for major problems. An algorithm for solving parabolic and <span class="hlt">elliptic</span> equations is proposed. The capabilities of the method are demonstrated by solving astrophysical problems on high-performance computer systems with massive parallelism.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/22036632','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/22036632"><span id="translatedtitle">Spectroscopic ellipsometer based on direct measurement of polarization <span class="hlt">ellipticity</span></span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Watkins, Lionel R.</p> <p>2011-06-20</p> <p>A polarizer-sample-Wollaston prism analyzer ellipsometer is described in which the ellipsometric angles {psi} and {Delta} are determined by direct measurement of the <span class="hlt">elliptically</span> polarized light reflected from the sample. With the Wollaston prism initially set to transmit p- and s-polarized light, the azimuthal angle P of the polarizer is adjusted until the two beams have equal intensity. This condition yields {psi}={+-}P and ensures that the reflected <span class="hlt">elliptically</span> polarized light has an azimuthal angle of {+-}45 deg. and maximum <span class="hlt">ellipticity</span>. Rotating the Wollaston prism through 45 deg. and adjusting the analyzer azimuth until the two beams again have equal intensity yields the <span class="hlt">ellipticity</span> that allows {Delta} to be determined via a simple linear relationship. The errors produced by nonideal components are analyzed. We show that the polarizer dominates these errors but that for most practical purposes, the error in {psi} is negligible and the error in {Delta} may be corrected exactly. A native oxide layer on a silicon substrate was measured at a single wavelength and multiple angles of incidence and spectroscopically at a single angle of incidence. The best fit film thicknesses obtained were in excellent agreement with those determined using a traditional null ellipsometer.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19830035772&hterms=1052&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D40%26Ntt%3D%2526%25231052','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19830035772&hterms=1052&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D40%26Ntt%3D%2526%25231052"><span id="translatedtitle">The infrared emission from the <span class="hlt">elliptical</span> galaxy NGC 1052</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Becklin, E. E.; Tokunaga, A. T.; Wynn-Williams, C. G.</p> <p>1982-01-01</p> <p>Multi-aperture IR photometry of the <span class="hlt">elliptical</span> galaxy NGC 1052 shows that its IR excess is confined to a region smaller than 2 arc sec (300 pc) in diameter coincident with the visible nucleus. It is suggested that the emission in the 5-20 micron range arises from dust heated by the nonthermal source seen at other wavelengths.</p> </li> </ol> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_13");'>13</a></li> <li><a href="#" onclick='return showDiv("page_14");'>14</a></li> <li class="active"><span>15</span></li> <li><a href="#" onclick='return showDiv("page_16");'>16</a></li> <li><a href="#" onclick='return showDiv("page_17");'>17</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div><!-- col-sm-12 --> </div><!-- row --> </div><!-- page_15 --> <div id="page_16" class="hiddenDiv"> <div class="row"> <div class="col-sm-12"> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_14");'>14</a></li> <li><a href="#" onclick='return showDiv("page_15");'>15</a></li> <li class="active"><span>16</span></li> <li><a href="#" onclick='return showDiv("page_17");'>17</a></li> <li><a href="#" onclick='return showDiv("page_18");'>18</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div> </div> <div class="row"> <div class="col-sm-12"> <ol class="result-class" start="301"> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19730012555','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19730012555"><span id="translatedtitle">Supersonic flow calculations for a cone with an <span class="hlt">elliptic</span> flare</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Lehrhaupt, H.</p> <p>1970-01-01</p> <p>A three-dimensional supersonic flow program is presented for calculating the flow field about a cone at zero angle of attack with an <span class="hlt">elliptical</span> flare. The program is irrotational, and results remain valid in the region ahead of the first relected characteristic from the points of shock where the shock is no longer axisymmetric.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2007JCoAM.206.1082T','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2007JCoAM.206.1082T"><span id="translatedtitle">An <span class="hlt">elliptic</span> singularly perturbed problem with two parameters I</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Teofanov, Lj.; Roos, H. G.</p> <p>2007-09-01</p> <p>In this paper we consider a singularly perturbed <span class="hlt">elliptic</span> problem with two small parameters posed on the unit square. Its solution may have exponential, parabolic and corner layers. We give a decomposition of the solution into regular and layer components and derive pointwise bounds on the components and their derivatives. The estimates are obtained by the analysis of appropriate problems on unbounded domains.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://eric.ed.gov/?q=force+AND+motion&pg=5&id=EJ843924','ERIC'); return false;" href="http://eric.ed.gov/?q=force+AND+motion&pg=5&id=EJ843924"><span id="translatedtitle">A Primer on <span class="hlt">Elliptic</span> Functions with Applications in Classical Mechanics</span></a></p> <p><a target="_blank" href="http://www.eric.ed.gov/ERICWebPortal/search/extended.jsp?_pageLabel=advanced">ERIC Educational Resources Information Center</a></p> <p>Brizard, Alain J.</p> <p>2009-01-01</p> <p>The Jacobi and Weierstrass <span class="hlt">elliptic</span> functions used to be part of the standard mathematical arsenal of physics students. They appear as solutions of many important problems in classical mechanics: the motion of a planar pendulum (Jacobi), the motion of a force-free asymmetric top (Jacobi), the motion of a spherical pendulum (Weierstrass) and the…</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://www.dtic.mil/docs/citations/ADA626966','DTIC-ST'); return false;" href="http://www.dtic.mil/docs/citations/ADA626966"><span id="translatedtitle">On Fibonacci Numbers Which Are <span class="hlt">Elliptic</span> Korselt Numbers</span></a></p> <p><a target="_blank" href="https://publicaccess.dtic.mil/psm/api/service/search/search">DTIC Science & Technology</a></p> <p></p> <p>2014-11-17</p> <p>On Fibonacci numbers which are <span class="hlt">elliptic</span> Korselt numbers Florian Luca School of Mathematics University of the Witwatersrand P. O. Box Wits 2050, South... Witwatersrand . This author thanks this institution for hospitality. 6 References [1] W. R. Alford, A. Granville and C. Pomerance, “There are infinitely</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016IJMPB..3050192M','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016IJMPB..3050192M"><span id="translatedtitle">Micromagnetic simulation of hysteresis loop of <span class="hlt">elliptic</span> permalloy nanorings</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Mishra, Amaresh Chandra</p> <p>2016-09-01</p> <p>Magnetic hysteresis behavior of isotropic permalloy <span class="hlt">elliptic</span> nanorings of outer semi-major axis length (aout) 100 nm and thickness (t) 20 nm were studied with respect to the variation of two parameters: outer semiminor axis length (bout) and the difference between outer and inner dimensions (r). The outer semiminor axis length (bout) varied from 90 nm to 20 nm which covers from nearly circular nanoring to <span class="hlt">elliptic</span> nanoring of high aspect ratio. The value of r varied in steps of 10 nm. Micromagnetic simulation of in-plane hysteresis curve of these nanorings revealed that the remanent state of all of these <span class="hlt">elliptic</span> rings are onion states if the magnetic field is applied along the longer side of the <span class="hlt">elliptic</span> rings. If the magnetic field is applied along the shorter side, then the remanent states turn out to be vortex state. The hysteresis loss indicated by area of the hysteresis loop was found to be decreasing gradually with the increment of either r or bout. On the other hand, the remanent magnetization increased with increment of r but decreased with the increment of bout. The changes were attributed to three parameters mainly: inner curvature, exchange energy and demagnetization energy. The changes in loop area were discussed in light of variation of these three parameters.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19830021441','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19830021441"><span id="translatedtitle">Elastohydrodynamics of <span class="hlt">elliptical</span> contacts for materials of low elastic modulus</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Hamrock, B. J.; Dowson, D.</p> <p>1983-01-01</p> <p>The influence of the <span class="hlt">ellipticity</span> parameter k and the dimensionless speed U, load W, and materials G parameters on minimum film thickness for materials of low elastic modulus was investigated. The <span class="hlt">ellipticity</span> parameter was varied from 1 (a ball-on-plane configuration) to 12 (a configuration approaching a line contact); U and W were each varied by one order of magnitude. Seventeen cases were used to generate the minimum- and central-film-thickness relations. The influence of lubricant starvation on minimum film thickness in starved <span class="hlt">elliptical</span>, elastohydrodynamic configurations was also investigated for materials of low elastic modulus. Lubricant starvation was studied simply by moving the inlet boundary closer to the center of the conjunction in the numerical solutions. Contour plots of pressure and film thickness in and around the contact were presented for both fully flooded and starved lubrication conditions. It is evident from these figures that the inlet pressure contours become less circular and closer to the edge of the Hertzian contact zone and that the film thickness decreases substantially as the serverity of starvation increases. The results presented reveal the essential features of both fully flooded and starved, <span class="hlt">elliptical</span>, elastohydrodynamic conjunctions for materials of low elastic modulus.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2014APS..MAR.Q7013K','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2014APS..MAR.Q7013K"><span id="translatedtitle">Effect of curvature on domain wall motion in <span class="hlt">elliptical</span> nanorings</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Kaya, Fikriye Idil; Bickel, Jessica; Aidala, Katherine</p> <p>2014-03-01</p> <p>Understanding domain wall (DW) motion in ferromagnetic nanostructures is important to realize proposed magnetic data storage and logic devices. We investigate the effect of curvature on DW pinning and motion by studying <span class="hlt">elliptical</span> rings using micromagnetic simulations. <span class="hlt">Elliptical</span> rings with constant width have varying curvature, with the lowest curvature at the minor axis, and the greatest curvature at the major axis. DWs can be created at any angular position within the ellipse by the application of an appropriate uniform magnetic field. However, only some of these positions are stable when the field is removed. We study the stability and depinning of the DWs by applying a slowly increasing <span class="hlt">elliptical</span> magnetic field to determine the magnitude of the field at which the DWs begin to move. By varying the major to minor axis ratio, we examine the effect of curvature on DW pinning. A larger field is required to move DWs in regions of higher curvature (near the major axis) than lower curvature (near the minor axis). Overall, we see that increasing the major to minor axis ratio of <span class="hlt">elliptical</span> nanorings requires increasing field strength to depin the DWs along the major axis. Work supported in part by NSF DMR-1207924 and NSF CMMI-1025020. Simulations performed at the CNS computational facilities at Harvard University, a member of the NNIN supported by NSF Award No. ECS-0335765.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2015IJASE...7....1K','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2015IJASE...7....1K"><span id="translatedtitle">Buckling characteristic of multi-laminated composite <span class="hlt">elliptical</span> cylindrical shells</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Kassegne, Samuel Kinde; Chun, Kyoung-Sik</p> <p>2015-03-01</p> <p>Fiber-reinforced composite materials continue to experience increased adoption in aerospace, marine, automobile, and civil structures due to their high specific strength, high stiffness, and light weight. This increased use has been accompanied by applications involving non-traditional configurations such as compression members with <span class="hlt">elliptical</span> cross-sections. To model such shapes, we develop and report an improved generalized shell element called 4EAS-FS through a combination of enhanced assumed strain and the substitute shear strain fields. A flat shell element has been developed by combining a membrane element with drilling degree-of-freedom and a plate bending element. We use the element developed to determine specifically buckling loads and mode shapes of composite laminates with <span class="hlt">elliptical</span> cross-section including transverse shear deformations. The combined influence of shell geometry and <span class="hlt">elliptical</span> cross-sectional parameters, fiber angle, and lay-up on the buckling loads of an <span class="hlt">elliptical</span> cylinder is examined. It is hoped that the critical buckling loads and mode shapes presented here will serve as a benchmark for future investigations.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://eric.ed.gov/?q=nonlinear&pg=4&id=EJ963907','ERIC'); return false;" href="http://eric.ed.gov/?q=nonlinear&pg=4&id=EJ963907"><span id="translatedtitle">Exploring Strange Nonchaotic Attractors through Jacobian <span class="hlt">Elliptic</span> Functions</span></a></p> <p><a target="_blank" href="http://www.eric.ed.gov/ERICWebPortal/search/extended.jsp?_pageLabel=advanced">ERIC Educational Resources Information Center</a></p> <p>Garcia-Hoz, A. Martinez; Chacon, R.</p> <p>2011-01-01</p> <p>We demonstrate the effectiveness of Jacobian <span class="hlt">elliptic</span> functions (JEFs) for inquiring into the reshaping effect of quasiperiodic forces in nonlinear nonautonomous systems exhibiting strange nonchaotic attractors (SNAs). Specifically, we characterize analytically and numerically some reshaping-induced transitions starting from SNAs in the context of…</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016JGRD..12114456K','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016JGRD..12114456K"><span id="translatedtitle">Deep convection in <span class="hlt">elliptical</span> and polygonal eyewalls of tropical cyclones</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Kuo, Hung-Chi; Cheng, Wei-Yi; Yang, Yi-Ting; Hendricks, Eric A.; Peng, Melinda S.</p> <p>2016-12-01</p> <p>In observations, tropical cyclones with cyclonically rotating <span class="hlt">elliptical</span> eyewalls are often characterized by wave number 2 (WN2) deep convection located at the edge of the major axis. A simple modeling framework is used to understand this phenomenon, where a nondivergent barotropic model (NBM) is employed to represent the <span class="hlt">elliptical</span> vortex in the free atmosphere, and an asymmetric slab boundary layer (SBL) model is used to simulate the frictional boundary layer (BL) underneath the free atmosphere. The interaction is one way in that the overlying cyclonic flow drives the BL, but the BL pumping does not feed back to the overlying flow. The nonlinear-balanced pressure field from the NBM drives the winds in the SBL model, which then causes BL convergence and pumping near the eyewall. The strong updrafts at the edge of the major axis for the <span class="hlt">elliptic</span> vortex in the BL are induced by the larger convergent radial wind from the asymmetric distribution of the pressure fields of the free atmosphere with noncircular vortex. The large radial inflow maintains the supergradient wind at the edge of the <span class="hlt">elliptical</span> vortex. The results emphasize the cyclonic rotation of the WN2 feature of strong updrafts at the top of the BL from the local shock-like BL radial wind structure. Similar radial profiles and strong BL top updrafts occur at the edges of higher-order polygonal eyewalls with the magnitude of the peak updraft decreasing as the wave number structure of the vortex increases.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/22348031','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/22348031"><span id="translatedtitle">The dynamical fingerprint of core scouring in massive <span class="hlt">elliptical</span> galaxies</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Thomas, J.; Saglia, R. P.; Bender, R.; Erwin, P.; Fabricius, M.</p> <p>2014-02-10</p> <p>The most massive <span class="hlt">elliptical</span> galaxies have low-density centers or cores that differ dramatically from the high-density centers of less massive <span class="hlt">ellipticals</span> and bulges of disk galaxies. These cores have been interpreted as the result of mergers of supermassive black hole binaries, which depopulate galaxy centers by gravitationally slingshotting central stars toward large radii. Such binaries naturally form in mergers of luminous galaxies. Here, we analyze the population of central stellar orbits in 11 massive <span class="hlt">elliptical</span> galaxies that we observed with the integral field spectrograph SINFONI at the European Southern Observatory Very Large Telescope. Our dynamical analysis is orbit-based and includes the effects of a central black hole, the mass distribution of the stars, and a dark matter halo. We show that the use of integral field kinematics and the inclusion of dark matter is important to conclude on the distribution of stellar orbits in galaxy centers. Six of our galaxies are core galaxies. In these six galaxies, but not in the galaxies without cores, we detect a coherent lack of stars on radial orbits in the core region and a uniform excess of radial orbits outside of it: when scaled by the core radius r{sub b} , the radial profiles of the classical anisotropy parameter β(r) are nearly identical in core galaxies. Moreover, they quantitatively match the predictions of black hole binary simulations, providing the first convincing dynamical evidence for core scouring in the most massive <span class="hlt">elliptical</span> galaxies.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/1999MeScT..10...25L','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/1999MeScT..10...25L"><span id="translatedtitle"><span class="hlt">Elliptical</span> polarization effects in a chromatically addressed Faraday current sensor</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Li, G. D.; Aspey, R. A.; Kong, M. G.; Gibson, J. R.; Jones, G. R.</p> <p>1999-01-01</p> <p>Optical polarization processes in a parallel-sided glass element used in a Faraday rotation current sensor have been considered. In such sensors the path length necessary to produce sufficient rotation of the plane of polarization is produced by a multiplicity of reflections within the glass element. It is shown that such reflections induce <span class="hlt">ellipticity</span> of polarization and that this affects the current-sensing performance of the sensor. Two reflection cases, corresponding to total internal reflections at a glass-air interface and reflections by aluminium-coated surfaces, are considered. The latter are shown to produce higher optical attenuation but a lower degree of <span class="hlt">elliptical</span> polarization. The implications of the induced <span class="hlt">elliptical</span> polarization in relation to chromatically modulated polychromatic light are considered. It is shown that the resolution of the Faraday sensing is improved by minimizing the <span class="hlt">ellipticity</span> of the polarization with the aluminium-coated reflections. However a greater dynamic range and signal strength may be achievable with the total internal reflection element.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/22279950','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/22279950"><span id="translatedtitle"><span class="hlt">Elliptical</span> galaxies kinematics within general relativity with renormalization group effects</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Rodrigues, Davi C.</p> <p>2012-09-01</p> <p>The renormalization group framework can be applied to Quantum Field Theory on curved space-time, but there is no proof whether the beta-function of the gravitational coupling indeed goes to zero in the far infrared or not. In a recent paper [1] we have shown that the amount of dark matter inside spiral galaxies may be negligible if a small running of the General Relativity coupling G is present (δG/G{sub 0}∼<10{sup −7} across a galaxy). Here we extend the proposed model to <span class="hlt">elliptical</span> galaxies and present a detailed analysis on the modeling of NGC 4494 (an ordinary <span class="hlt">elliptical</span>) and NGC 4374 (a giant <span class="hlt">elliptical</span>). In order to compare our results to a well known alternative model to the standard dark matter picture, we also evaluate NGC 4374 with MOND. In this galaxy MOND leads to a significative discrepancy with the observed velocity dispersion curve and has a significative tendency towards tangential anisotropy. On the other hand, the approach based on the renormalization group and general relativity (RGGR) could be applied with good results to these <span class="hlt">elliptical</span> galaxies and is compatible with lower mass-to-light ratios (of about the Kroupa IMF type)</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2010NIMPA.624..162B','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2010NIMPA.624..162B"><span id="translatedtitle">Shielding of <span class="hlt">elliptic</span> guides with direct sight to the moderator</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Böni, P.; Grünauer, F.; Schanzer, C.</p> <p>2010-12-01</p> <p>With the invention of <span class="hlt">elliptic</span> guides, the neutron flux at instruments can be increased significantly even without sacrificing resolution. In addition, the phase space homogeneity of the delivered neutrons is improved. Using superpolished metal substrates that are coated with supermirror, it is now possible to install neutron guides close to the moderator thus decreasing the illumination losses of the guide and reducing the background because the entrance window of the <span class="hlt">elliptic</span> guide can be decreased significantly. We have performed Monte Carlo simulations using the program package MCNP5 to calculate the shielding requirements for an <span class="hlt">elliptic</span> guide geometry assuming that the initial guide section elements are composed of Al substrates. We show that shielding made from heavy concrete shields the neutron and γ-radiation effectively to levels below 1 μSv/h. It is shown that the <span class="hlt">elliptic</span> geometry allows to match the phase space of the transported neutrons easily to the needs of the instruments to be installed. In particular it is possible to maintain a compact phase space during the transport of the neutrons because the reflection losses are strongly reduced.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2000JPhA...33.6279A','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2000JPhA...33.6279A"><span id="translatedtitle">Towards a cladistics of double Yangians and <span class="hlt">elliptic</span> algebras*</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Arnaudon, D.; Avan, J.; Frappat, L.; Ragoucy, E.; Rossi, M.</p> <p>2000-09-01</p> <p>A self-contained description of algebraic structures, obtained by combinations of various limit procedures applied to vertex and face sl(2) <span class="hlt">elliptic</span> quantum affine algebras, is given. New double Yangian structures of dynamical type are defined. Connections between these structures are established. A number of them take the form of twist-like actions. These are conjectured to be evaluations of universal twists.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19680013892','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19680013892"><span id="translatedtitle"><span class="hlt">Elliptic</span> Capture Orbits for Missions to the Near Planets</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Casal, Federico G.; Swenson, Byron L.; Mascy, Alfred C.</p> <p>1968-01-01</p> <p><span class="hlt">Elliptic</span> capture orbits around Mars and Venus have often been considered as means for reducing arrival and departure energy requirements for two-way missions. It had also generally been feared that the energy savings obtained by capturing a spacecraft into a highly <span class="hlt">elliptical</span> orbit (rather than a near circular orbit of the same periapsis) would largely be offset by the penalties incurred in aligning the semi-major axis of the ellipse in such a way as to obtain the proper orientation of the departure hyperbola. This paper, presents the results of an analysis which takes into consideration the penalties arising from the requirement to match the orientation of the <span class="hlt">elliptical</span> orbit with the asymptote of the departure hyperbola. The scientific aspects of <span class="hlt">elliptical</span> orbits around the target planet are discussed, and it is shown that such orbits exhibit characteristics which may be considered advantageous or disadvantageous depending on the purpose of the mission. Alignment of ' the semi-major axis of the capture, ellipse relative to the, asymptote of the escape hyperbola was found not to be a critical requirement since the kinetic energy remains high over a substantial portion of the <span class="hlt">elliptical</span> capture orbit. This 'means that the escape stage can operate efficiently even when ignited at some angle from the true periapsis point. Considerable freedom in choosing this angle is available at little propulsive cost. The resulting latitude in the choice of angles between arrival and escape asymptotes makes it possible to consider a wide variety of interplanetary transfers and planetary staytimes without the need for separate propulsive maneuvers to realign the capture ellipse before departure., Special consideration has also been g1ven to plane change maneuvers around the planet. These may be required for reasons of orbit dynamics or scientific experimentation and are not uniquely tied to <span class="hlt">elliptical</span> captures. The sensitivity of the mass of the excursion module to the</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2014SPIE.9283E..04L','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2014SPIE.9283E..04L"><span id="translatedtitle">Experimental study on <span class="hlt">elliptical</span> vibration cutting for optical microstructures</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Li, Guo; Che, Lin; Wang, Bo; Ding, Fei; Zhang, Chen Feng</p> <p>2014-08-01</p> <p>In the processing technology of optical microstructure, mechanical processing with high efficiency and quality is still dominating. However, with microstructure surface quality higher and higher, the precision and ultra precision cutting technology has been difficult to meet the needs of reality, and it still remains a big issue in production efficiency and cost. In this case, the <span class="hlt">elliptical</span> vibration cutting method is created. At present, research on the effect of <span class="hlt">elliptical</span> vibration cutting on surface quality of microstructures with special optical properties such as V-groove, micro pyramid and sinusoidal grid surface is rarely seen. This paper focuses on the <span class="hlt">elliptical</span> vibration cutting process of arc groove and V-groove, aiming at finding the discipline of various parameters (frequency, amplitude, feed rate) and analyzing the surface quality through experiments. Firstly, the principle of <span class="hlt">elliptical</span> vibration cutting is introduced, the cutting mechanism and the theoretical error are analyzed, and a vibration cutting system is designed for precision machining. Because the surface quality and burr play have a huge impact on optical microstructure, effects of the vibration frequency (0-2kHz), amplitude (0.5-2.5μm) as well as feed rate (6-30mm/min) on surface quality and burr suppression are analyzed. The experimental results show that compared to normal cutting, <span class="hlt">elliptical</span> vibration cutting has obvious advantages. With the increases of the frequency and amplitude, the surface quality improves significantly, the surface roughness is changed from 61.5nm to 25.3nm, and burr has been suppressed to some extent.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/21691433','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/21691433"><span id="translatedtitle">MIB method for <span class="hlt">elliptic</span> equations with multi-material interfaces.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Xia, Kelin; Zhan, Meng; Wei, Guo-Wei</p> <p>2011-06-01</p> <p><span class="hlt">Elliptic</span> partial differential equations (PDEs) are widely used to model real-world problems. Due to the heterogeneous characteristics of many naturally occurring materials and man-made structures, devices, and equipments, one frequently needs to solve <span class="hlt">elliptic</span> PDEs with discontinuous coefficients and singular sources. The development of high-order <span class="hlt">elliptic</span> interface schemes has been an active research field for decades. However, challenges remain in the construction of high-order schemes and particularly, for nonsmooth interfaces, i.e., interfaces with geometric singularities. The challenge of geometric singularities is amplified when they are originated from two or more material interfaces joining together or crossing each other. High-order methods for <span class="hlt">elliptic</span> equations with multi-material interfaces have not been reported in the literature to our knowledge. The present work develops matched interface and boundary (MIB) method based schemes for solving two-dimensional (2D) <span class="hlt">elliptic</span> PDEs with geometric singularities of multi-material interfaces. A number of new MIB schemes are constructed to account for all possible topological variations due to two-material interfaces. The geometric singularities of three-material interfaces are significantly more difficult to handle. Three new MIB schemes are designed to handle a variety of geometric situations and topological variations, although not all of them. The performance of the proposed new MIB schemes is validated by numerical experiments with a wide range of coefficient contrasts, geometric singularities, and solution types. Extensive numerical studies confirm the designed second order accuracy of the MIB method for multi-material interfaces, including a case where the derivative of the solution diverges.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/20653047','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/20653047"><span id="translatedtitle">From Flat Substrate to <span class="hlt">Elliptical</span> KB Mirror by Profile Coating</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Liu Chian; Conley, R.; Assoufid, L.; Cai, Z.; Qian, J.; Macrander, A.T.</p> <p>2004-05-12</p> <p>For microfocusing x-ray mirrors, an <span class="hlt">elliptical</span> shape is essential for aberration-free optics. However, it is difficult to polish <span class="hlt">elliptical</span> mirrors to x-ray-quality smoothness. Profile coatings have been applied on both cylindrical and flat Si substrates to make the desired <span class="hlt">elliptical</span> shape. In a profile-coating process, the sputter source power is kept constant, while the substrate is passed over a contoured mask at a constant speed to obtain a desired profile along the direction perpendicular to the substrate-moving direction. The shape of the contour was derived from a desired profile and the thickness distribution of the coating material at the substrate level. The thickness distribution was measured on films coated on Si wafers using a spectroscopic ellipsometer with computer-controlled X-Y translation stages. The mirror coating profile is determined from the difference between the ideal surface figure of a focusing ellipse and the surface figure obtained from a long trace profiler measurement on the substrate. The number of passes and the moving speed of the substrate are determined according to the required thickness and the growth-rate calibration of a test run. A KB mirror pair was made using Au as a coating material and cylindrically polished mirrors as substrates. Synchrotron x-ray results using this KB mirror pair showed a focused spot size of 0.4 x 0.4 {mu}m2. This technique has also been applied for making <span class="hlt">elliptical</span> KB mirrors from flat Si substrates. The challenges and solutions associated with <span class="hlt">elliptical</span> profile coating on flat substrates will be discussed.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2004AIPC..705..704L','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2004AIPC..705..704L"><span id="translatedtitle">From Flat Substrate to <span class="hlt">Elliptical</span> KB Mirror by Profile Coating</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Liu, Chian; Conley, R.; Assoufid, L.; Cai, Z.; Qian, J.; Macrander, A. T.</p> <p>2004-05-01</p> <p>For microfocusing x-ray mirrors, an <span class="hlt">elliptical</span> shape is essential for aberration-free optics. However, it is difficult to polish <span class="hlt">elliptical</span> mirrors to x-ray-quality smoothness. Profile coatings have been applied on both cylindrical and flat Si substrates to make the desired <span class="hlt">elliptical</span> shape. In a profile-coating process, the sputter source power is kept constant, while the substrate is passed over a contoured mask at a constant speed to obtain a desired profile along the direction perpendicular to the substrate-moving direction. The shape of the contour was derived from a desired profile and the thickness distribution of the coating material at the substrate level. The thickness distribution was measured on films coated on Si wafers using a spectroscopic ellipsometer with computer-controlled X-Y translation stages. The mirror coating profile is determined from the difference between the ideal surface figure of a focusing ellipse and the surface figure obtained from a long trace profiler measurement on the substrate. The number of passes and the moving speed of the substrate are determined according to the required thickness and the growth-rate calibration of a test run. A KB mirror pair was made using Au as a coating material and cylindrically polished mirrors as substrates. Synchrotron x-ray results using this KB mirror pair showed a focused spot size of 0.4 × 0.4 μm2. This technique has also been applied for making <span class="hlt">elliptical</span> KB mirrors from flat Si substrates. The challenges and solutions associated with <span class="hlt">elliptical</span> profile coating on flat substrates will be discussed.</p> </li> </ol> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_14");'>14</a></li> <li><a href="#" onclick='return showDiv("page_15");'>15</a></li> <li class="active"><span>16</span></li> <li><a href="#" onclick='return showDiv("page_17");'>17</a></li> <li><a href="#" onclick='return showDiv("page_18");'>18</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div><!-- col-sm-12 --> </div><!-- row --> </div><!-- page_16 --> <div id="page_17" class="hiddenDiv"> <div class="row"> <div class="col-sm-12"> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_15");'>15</a></li> <li><a href="#" onclick='return showDiv("page_16");'>16</a></li> <li class="active"><span>17</span></li> <li><a href="#" onclick='return showDiv("page_18");'>18</a></li> <li><a href="#" onclick='return showDiv("page_19");'>19</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div> </div> <div class="row"> <div class="col-sm-12"> <ol class="result-class" start="321"> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3117633','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3117633"><span id="translatedtitle">MIB method for <span class="hlt">elliptic</span> equations with multi-material interfaces</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Xia, Kelin; Zhan, Meng; Wei, Guo-Wei</p> <p>2011-01-01</p> <p><span class="hlt">Elliptic</span> partial differential equations (PDEs) are widely used to model real-world problems. Due to the heterogeneous characteristics of many naturally occurring materials and man-made structures, devices, and equipments, one frequently needs to solve <span class="hlt">elliptic</span> PDEs with discontinuous coefficients and singular sources. The development of high-order <span class="hlt">elliptic</span> interface schemes has been an active research field for decades. However, challenges remain in the construction of high-order schemes and particularly, for nonsmooth interfaces, i.e., interfaces with geometric singularities. The challenge of geometric singularities is amplified when they are originated from two or more material interfaces joining together or crossing each other. High-order methods for <span class="hlt">elliptic</span> equations with multi-material interfaces have not been reported in the literature to our knowledge. The present work develops matched interface and boundary (MIB) method based schemes for solving two-dimensional (2D) <span class="hlt">elliptic</span> PDEs with geometric singularities of multi-material interfaces. A number of new MIB schemes are constructed to account for all possible topological variations due to two-material interfaces. The geometric singularities of three-material interfaces are significantly more difficult to handle. Three new MIB schemes are designed to handle a variety of geometric situations and topological variations, although not all of them. The performance of the proposed new MIB schemes is validated by numerical experiments with a wide range of coefficient contrasts, geometric singularities, and solution types. Extensive numerical studies confirm the designed second order accuracy of the MIB method for multi-material interfaces, including a case where the derivative of the solution diverges. PMID:21691433</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/16689620','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/16689620"><span id="translatedtitle">Development of a submaximal test to predict <span class="hlt">elliptical</span> cross-trainer VO2max.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Dalleck, Lance C; Kravitz, Len; Robergs, Robert A</p> <p>2006-05-01</p> <p>The purpose of this study was to develop an equation to predict VO2max from a submaximal <span class="hlt">elliptical</span> cross-trainer test. Fifty-four apparently healthy subjects (25 men and 29 women, mean +/- SD age: 29.5 +/- 7.1 years, height: 173.3 +/- 12.6 cm, weight: 72.3 +/- 7.9 kg, percent body fat: 17.3 +/- 5.0%, and <span class="hlt">elliptical</span> cross-trainer VO2max: 43.9 +/- 7.2 ml x kg(-1) x min(-1)) participated in the study and were randomly assigned to an original sample group (n = 40) and a cross-validation group (n = 14). Each subject completed an <span class="hlt">elliptical</span> cross-trainer submaximal (3 5-minute submaximal stages) and a VO2max test on the same day, with a 15-minute rest period in between. Stepwise multiple regression analyses were used to develop an equation for estimating <span class="hlt">elliptical</span> cross-trainer VO2max from the data of the original sample group. The accuracy of the equation was tested by using data from the cross-validation group. Because there was no shrinkage in R2 between the original sample group and the cross-validation group, data were combined in the final prediction equation (R2 = 0.732, standard error of the estimate = 3.91 ml x kg(-1) x min(-1), p < 0.05): VO2max = 73.676 + 7.383(gender) - 0.317(weight) + 0.003957(age x cadence) - 0.006452(age x heart rate at stage 2). The <span class="hlt">correlation</span> coefficient between the predicted and measured VO2max values was r = 0.86. Dependent t-tests resulted in no significant differences (p > 0.05) between predicted (43.8 ml x kg(-1) x min(-1)) and measured (43.9 ml x kg(-1) x min(-1)) VO2max measurements. Results indicate that the protocol and equation developed in the current study can be used by exercise professionals to provide acceptably accurate estimates of VO2max in non-laboratory-based settings.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/21904246','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/21904246"><span id="translatedtitle">Mechanically braked <span class="hlt">elliptical</span> Wingate test: modification considerations, load optimization, and reliability.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Ozkaya, Ozgur; Colakoglu, Muzaffer; Kuzucu, Erinc O; Yildiztepe, Engin</p> <p>2012-05-01</p> <p>The 30-second, all-out Wingate test evaluates anaerobic performance using an upper or lower body cycle ergometer (cycle Wingate test). A recent study showed that using a modified electromagnetically braked <span class="hlt">elliptical</span> trainer for Wingate testing (EWT) leads to greater power outcomes because of larger muscle group recruitment. The main purpose of this study was to modify an <span class="hlt">elliptical</span> trainer using an easily understandable mechanical brake system instead of an electromagnetically braked modification. Our secondary aim was to determine a proper test load for the EWT to reveal the most efficient anaerobic test outcomes such as peak power (PP), average power (AP), minimum power (MP), power drop (PD), and fatigue index ratio (FI%) and to evaluate the retest reliability of the selected test load. Delta lactate responses (ΔLa) were also analyzed to confirm all the anaerobic performance of the athletes. Thirty healthy and well-trained male university athletes were selected to participate in the study. By analysis of variance, an 18% body mass workload yielded significantly greater test outcomes (PP = 19.5 ± 2.4 W·kg, AP = 13.7 ± 1.7 W·kg, PD = 27.9 ± 5 W·s, FI% = 58.4 ± 3.3%, and ΔLa = 15.4 ± 1.7 mM) than the other (12-24% body mass) tested loads (p < 0.05). Test and retest results for relative PP, AP, MP, PD, FI%, and ΔLa were highly <span class="hlt">correlated</span> (r = 0.97, 0.98, 0.94, 0.91, 0.81, and 0.95, respectively). In conclusion, it was found that the mechanically braked modification of an <span class="hlt">elliptical</span> trainer successfully estimated anaerobic power and capacity. A workload of 18% body mass was optimal for measuring maximal and reliable anaerobic power outcomes. Anaerobic testing using an EWT may be more useful to athletes and coaches than traditional cycle ergometers because a greater proportion of muscle groups are worked during exercise on an <span class="hlt">elliptical</span> trainer.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/22465658','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/22465658"><span id="translatedtitle">A model and variance reduction method for computing statistical outputs of stochastic <span class="hlt">elliptic</span> partial differential equations</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Vidal-Codina, F.; Nguyen, N.C.; Giles, M.B.; Peraire, J.</p> <p>2015-09-15</p> <p>We present a model and variance reduction method for the fast and reliable computation of statistical outputs of stochastic <span class="hlt">elliptic</span> partial differential equations. Our method consists of three main ingredients: (1) the hybridizable discontinuous Galerkin (HDG) discretization of <span class="hlt">elliptic</span> partial differential equations (PDEs), which allows us to obtain high-order accurate solutions of the governing PDE; (2) the reduced basis method for a new HDG discretization of the underlying PDE to enable real-time solution of the parameterized PDE in the presence of stochastic parameters; and (3) a multilevel variance reduction method that exploits the statistical <span class="hlt">correlation</span> among the different reduced basis approximations and the high-fidelity HDG discretization to accelerate the convergence of the Monte Carlo simulations. The multilevel variance reduction method provides efficient computation of the statistical outputs by shifting most of the computational burden from the high-fidelity HDG approximation to the reduced basis approximations. Furthermore, we develop a posteriori error estimates for our approximations of the statistical outputs. Based on these error estimates, we propose an algorithm for optimally choosing both the dimensions of the reduced basis approximations and the sizes of Monte Carlo samples to achieve a given error tolerance. We provide numerical examples to demonstrate the performance of the proposed method.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2015JCoPh.297..700V','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2015JCoPh.297..700V"><span id="translatedtitle">A model and variance reduction method for computing statistical outputs of stochastic <span class="hlt">elliptic</span> partial differential equations</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Vidal-Codina, F.; Nguyen, N. C.; Giles, M. B.; Peraire, J.</p> <p>2015-09-01</p> <p>We present a model and variance reduction method for the fast and reliable computation of statistical outputs of stochastic <span class="hlt">elliptic</span> partial differential equations. Our method consists of three main ingredients: (1) the hybridizable discontinuous Galerkin (HDG) discretization of <span class="hlt">elliptic</span> partial differential equations (PDEs), which allows us to obtain high-order accurate solutions of the governing PDE; (2) the reduced basis method for a new HDG discretization of the underlying PDE to enable real-time solution of the parameterized PDE in the presence of stochastic parameters; and (3) a multilevel variance reduction method that exploits the statistical <span class="hlt">correlation</span> among the different reduced basis approximations and the high-fidelity HDG discretization to accelerate the convergence of the Monte Carlo simulations. The multilevel variance reduction method provides efficient computation of the statistical outputs by shifting most of the computational burden from the high-fidelity HDG approximation to the reduced basis approximations. Furthermore, we develop a posteriori error estimates for our approximations of the statistical outputs. Based on these error estimates, we propose an algorithm for optimally choosing both the dimensions of the reduced basis approximations and the sizes of Monte Carlo samples to achieve a given error tolerance. We provide numerical examples to demonstrate the performance of the proposed method.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2015JHEP...06..190A','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2015JHEP...06..190A"><span id="translatedtitle"><span class="hlt">Elliptic</span> flow of identified hadrons in Pb-Pb collisions at TeV</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Abelev, B.; Adam, J.; Adamová, D.; Aggarwal, M. M.; Agnello, M.; Agostinelli, A.; Agrawal, N.; Ahammed, Z.; Ahmad, N.; Ahmed, I.; Ahn, S. U.; Ahn, S. A.; Aimo, I.; Aiola, S.; Ajaz, M.; Akindinov, A.; Alam, S. N.; Aleksandrov, D.; Alessandro, B.; Alexandre, D.; Alici, A.; Alkin, A.; Alme, J.; Alt, T.; Altinpinar, S.; Altsybeev, I.; Alves Garcia Prado, C.; Andrei, C.; Andronic, A.; Anguelov, V.; Anielski, J.; Antičić, T.; Antinori, F.; Antonioli, P.; Aphecetche, L.; Appelshäuser, H.; Arcelli, S.; Armesto, N.; Arnaldi, R.; Aronsson, T.; Arsene, I. C.; Arslandok, M.; Augustinus, A.; Averbeck, R.; Awes, T. C.; Azmi, M. D.; Bach, M.; Badalà, A.; Baek, Y. W.; Bagnasco, S.; Bailhache, R.; Bala, R.; Baldisseri, A.; Baltasar Dos Santos Pedrosa, F.; Baral, R. C.; Barbera, R.; Barile, F.; Barnaföldi, G. G.; Barnby, L. S.; Barret, V.; Bartke, J.; Basile, M.; Bastid, N.; Basu, S.; Bathen, B.; Batigne, G.; Batista Camejo, A.; Batyunya, B.; Batzing, P. C.; Baumann, C.; Bearden, I. G.; Beck, H.; Bedda, C.; Behera, N. K.; Belikov, I.; Bellini, F.; Bellwied, R.; Belmont-Moreno, E.; Belmont, R.; Belyaev, V.; Bencedi, G.; Beole, S.; Berceanu, I.; Bercuci, A.; Berdnikov, Y.; Berenyi, D.; Berger, M. E.; Bertens, R. A.; Berzano, D.; Betev, L.; Bhasin, A.; Bhat, I. R.; Bhati, A. K.; Bhattacharjee, B.; Bhom, J.; Bianchi, L.; Bianchi, N.; Bianchin, C.; Bielčík, J.; Bielčíková, J.; Bilandzic, A.; Bjelogrlic, S.; Blanco, F.; Blau, D.; Blume, C.; Bock, F.; Bogdanov, A.; Bøggild, H.; Bogolyubsky, M.; Böhmer, F. V.; Boldizsár, L.; Bombara, M.; Book, J.; Borel, H.; Borissov, A.; Bossú, F.; Botje, M.; Botta, E.; Böttger, S.; Braun-Munzinger, P.; Bregant, M.; Breitner, T.; Broker, T. A.; Browning, T. A.; Broz, M.; Bruna, E.; Bruno, G. E.; Budnikov, D.; Buesching, H.; Bufalino, S.; Buncic, P.; Busch, O.; Buthelezi, Z.; Caffarri, D.; Cai, X.; Caines, H.; Calero Diaz, L.; Caliva, A.; Calvo Villar, E.; Camerini, P.; Carena, F.; Carena, W.; Castillo Castellanos, J.; Casula, E. A. R.; Catanescu, V.; Cavicchioli, C.; Ceballos Sanchez, C.; Cepila, J.; Cerello, P.; Chang, B.; Chapeland, S.; Charvet, J. L.; Chattopadhyay, S.; Chattopadhyay, S.; Chelnokov, V.; Cherney, M.; Cheshkov, C.; Cheynis, B.; Chibante Barroso, V.; Chinellato, D. D.; Chochula, P.; Chojnacki, M.; Choudhury, S.; Christakoglou, P.; Christensen, C. H.; Christiansen, P.; Chujo, T.; Chung, S. U.; Cicalo, C.; Cifarelli, L.; Cindolo, F.; Cleymans, J.; Colamaria, F.; Colella, D.; Collu, A.; Colocci, M.; Conesa Balbastre, G.; Conesa del Valle, Z.; Connors, M. E.; Contreras, J. G.; Cormier, T. M.; Corrales Morales, Y.; Cortese, P.; Cortés Maldonado, I.; Cosentino, M. R.; Costa, F.; Crochet, P.; Cruz Albino, R.; Cuautle, E.; Cunqueiro, L.; Dainese, A.; Dang, R.; Danu, A.; Das, D.; Das, I.; Das, K.; Das, S.; Dash, A.; Dash, S.; De, S.; Delagrange, H.; Deloff, A.; Dénes, E.; D'Erasmo, G.; De Caro, A.; de Cataldo, G.; de Cuveland, J.; De Falco, A.; De Gruttola, D.; De Marco, N.; De Pasquale, S.; de Rooij, R.; Diaz Corchero, M. A.; Dietel, T.; Dillenseger, P.; Divià, R.; Di Bari, D.; Di Liberto, S.; Di Mauro, A.; Di Nezza, P.; Djuvsland, Ø.; Dobrin, A.; Dobrowolski, T.; Domenicis Gimenez, D.; Dönigus, B.; Dordic, O.; Dørheim, S.; Dubey, A. K.; Dubla, A.; Ducroux, L.; Dupieux, P.; Dutta Majumdar, A. K.; Hilden, T. E.; Ehlers, R. J.; Elia, D.; Engel, H.; Erazmus, B.; Erdal, H. A.; Eschweiler, D.; Espagnon, B.; Esposito, M.; Estienne, M.; Esumi, S.; Evans, D.; Evdokimov, S.; Fabris, D.; Faivre, J.; Falchieri, D.; Fantoni, A.; Fasel, M.; Fehlker, D.; Feldkamp, L.; Felea, D.; Feliciello, A.; Feofilov, G.; Ferencei, J.; Fernández Téllez, A.; Ferreiro, E. G.; Ferretti, A.; Festanti, A.; Figiel, J.; Figueredo, M. A. S.; Filchagin, S.; Finogeev, D.; Fionda, F. M.; Fiore, E. M.; Floratos, E.; Floris, M.; Foertsch, S.; Foka, P.; Fokin, S.; Fragiacomo, E.; Francescon, A.; Frankenfeld, U.; Fuchs, U.; Furget, C.; Fusco Girard, M.; Gaardhøje, J. J.; Gagliardi, M.; Gago, A. M.; Gallio, M.; Gangadharan, D. R.; Ganoti, P.; Garabatos, C.; Garcia-Solis, E.; Gargiulo, C.; Garishvili, I.; Gerhard, J.; Germain, M.; Gheata, A.; Gheata, M.; Ghidini, B.; Ghosh, P.; Ghosh, S. K.; Gianotti, P.; Giubellino, P.; Gladysz-Dziadus, E.; Glässel, P.; Gomez Ramirez, A.; González-Zamora, P.; Gorbunov, S.; Görlich, L.; Gotovac, S.; Graczykowski, L. K.; Grelli, A.; Grigoras, A.; Grigoras, C.; Grigoriev, V.; Grigoryan, A.; Grigoryan, S.; Grinyov, B.; Grion, N.; Grosse-Oetringhaus, J. F.; Grossiord, J.-Y.; Grosso, R.; Guber, F.; Guernane, R.; Guerzoni, B.; Guilbaud, M.; Gulbrandsen, K.; Gulkanyan, H.; Gumbo, M.; Gunji, T.; Gupta, A.; Gupta, R.; Khan, K. H.; Haake, R.; Haaland, Ø.; Hadjidakis, C.; Haiduc, M.; Hamagaki, H.; Hamar, G.; Hanratty, L. D.; Hansen, A.; Harris, J. W.; Hartmann, H.; Harton, A.; Hatzifotiadou, D.; Hayashi, S.; Heckel, S. T.; Heide, M.; Helstrup, H.; Herghelegiu, A.; Herrera Corral, G.; Hess, B. A.; Hetland, K. F.; Hippolyte, B.; Hladky, J.; Hristov, P.; Huang, M.; Humanic, T. J.; Hussain, N.; Hutter, D.; Hwang, D. S.; Ilkaev, R.; Ilkiv, I.; Inaba, M.; Innocenti, G. M.; Ionita, C.; Ippolitov, M.; Irfan, M.; Ivanov, M.; Ivanov, V.; Jacholkowski, A.; Jacobs, P. M.; Jahnke, C.; Jang, H. J.; Janik, M. A.; Jayarathna, P. H. S. Y.; Jena, C.; Jena, S.; Jimenez Bustamante, R. T.; Jones, P. G.; Jung, H.; Jusko, A.; Kadyshevskiy, V.; Kalcher, S.; Kalinak, P.; Kalweit, A.; Kamin, J.; Kang, J. H.; Kaplin, V.; Kar, S.; Karasu Uysal, A.; Karavichev, O.; Karavicheva, T.; Karpechev, E.; Kebschull, U.; Keidel, R.; Keijdener, D. L. D.; Keil SVN, M.; Khan, M. M.; Khan, P.; Khan, S. A.; Khanzadeev, A.; Kharlov, Y.; Kileng, B.; Kim, B.; Kim, D. W.; Kim, D. J.; Kim, J. S.; Kim, M.; Kim, M.; Kim, S.; Kim, T.; Kirsch, S.; Kisel, I.; Kiselev, S.; Kisiel, A.; Kiss, G.; Klay, J. L.; Klein, J.; Klein-Bösing, C.; Kluge, A.; Knichel, M. L.; Knospe, A. G.; Kobdaj, C.; Kofarago, M.; Köhler, M. K.; Kollegger, T.; Kolojvari, A.; Kondratiev, V.; Kondratyeva, N.; Konevskikh, A.; Kovalenko, V.; Kowalski, M.; Kox, S.; Koyithatta Meethaleveedu, G.; Kral, J.; Králik, I.; Kramer, F.; Kravčáková, A.; Krelina, M.; Kretz, M.; Krivda, M.; Krizek, F.; Kryshen, E.; Krzewicki, M.; Kučera, V.; Kucheriaev, Y.; Kugathasan, T.; Kuhn, C.; Kuijer, P. G.; Kulakov, I.; Kumar, J.; Kurashvili, P.; Kurepin, A.; Kurepin, A. B.; Kuryakin, A.; Kushpil, S.; Kweon, M. J.; Kwon, Y.; Ladron de Guevara, P.; Lagana Fernandes, C.; Lakomov, I.; Langoy, R.; Lara, C.; Lardeux, A.; Lattuca, A.; La Pointe, S. L.; La Rocca, P.; Lea, R.; Leardini, L.; Lee, G. R.; Legrand, I.; Lehnert, J.; Lemmon, R. C.; Lenti, V.; Leogrande, E.; Leoncino, M.; León Monzón, I.; Lévai, P.; Li, S.; Lien, J.; Lietava, R.; Lindal, S.; Lindenstruth, V.; Lippmann, C.; Lisa, M. A.; Ljunggren, H. M.; Lodato, D. F.; Loenne, P. I.; Loggins, V. R.; Loginov, V.; Lohner, D.; Loizides, C.; Lopez, X.; López Torres, E.; Lu, X.-G.; Luettig, P.; Lunardon, M.; Luparello, G.; Ma, R.; Maevskaya, A.; Mager, M.; Mahapatra, D. P.; Mahmood, S. M.; Maire, A.; Majka, R. D.; Malaev, M.; Maldonado Cervantes, I.; Malinina, L.; Mal'Kevich, D.; Malzacher, P.; Mamonov, A.; Manceau, L.; Manko, V.; Manso, F.; Manzari, V.; Marchisone, M.; Mareš, J.; Margagliotti, G. V.; Margotti, A.; Marín, A.; Markert, C.; Marquard, M.; Martashvili, I.; Martin, N. A.; Martinengo, P.; Martínez, M. I.; Martínez García, G.; Martin Blanco, J.; Martynov, Y.; Mas, A.; Masciocchi, S.; Masera, M.; Masoni, A.; Massacrier, L.; Mastroserio, A.; Matyja, A.; Mayer, C.; Mazer, J.; Mazzoni, M. A.; Meddi, F.; Menchaca-Rocha, A.; Mercado Pérez, J.; Meres, M.; Miake, Y.; Mikhaylov, K.; Milano, L.; Milosevic, J.; Mischke, A.; Mishra, A. N.; Miskowiec, D.; Mitra, J.; Mitu, C. M.; Mlynarz, J.; Mohammadi, N.; Mohanty, B.; Molnar, L.; Montaño Zetina, L.; Montes, E.; Morando, M.; Moreira De Godoy, D. A.; Moretto, S.; Morsch, A.; Muccifora, V.; Mudnic, E.; Mühlheim, D.; Muhuri, S.; Mukherjee, M.; Müller, H.; Munhoz, M. G.; Murray, S.; Musa, L.; Musinsky, J.; Nandi, B. K.; Nania, R.; Nappi, E.; Nattrass, C.; Nayak, K.; Nayak, T. K.; Nazarenko, S.; Nedosekin, A.; Nicassio, M.; Niculescu, M.; Nielsen, B. S.; Nikolaev, S.; Nikulin, S.; Nikulin, V.; Nilsen, B. S.; Noferini, F.; Nomokonov, P.; Nooren, G.; Norman, J.; Nyanin, A.; Nystrand, J.; Oeschler, H.; Oh, S.; Oh, S. K.; Okatan, A.; Olah, L.; Oleniacz, J.; Oliveira Da Silva, A. C.; Onderwaater, J.; Oppedisano, C.; Ortiz Velasquez, A.; Oskarsson, A.; Otwinowski, J.; Oyama, K.; Sahoo, P.; Pachmayer, Y.; Pachr, M.; Pagano, P.; Paić, G.; Painke, F.; Pajares, C.; Pal, S. K.; Palmeri, A.; Pant, D.; Papikyan, V.; Pappalardo, G. S.; Pareek, P.; Park, W. J.; Parmar, S.; Passfeld, A.; Patalakha, D. I.; Paticchio, V.; Paul, B.; Pawlak, T.; Peitzmann, T.; Pereira Da Costa, H.; Pereira De Oliveira Filho, E.; Peresunko, D.; Pérez Lara, C. E.; Pesci, A.; Peskov, V.; Pestov, Y.; Petráček, V.; Petran, M.; Petris, M.; Petrovici, M.; Petta, C.; Piano, S.; Pikna, M.; Pillot, P.; Pinazza, O.; Pinsky, L.; Piyarathna, D. B.; Ploskon, M.; Planinic, M.; Pluta, J.; Pochybova, S.; Podesta-Lerma, P. L. M.; Poghosyan, M. G.; Pohjoisaho, E. H. O.; Polichtchouk, B.; Poljak, N.; Pop, A.; Porteboeuf-Houssais, S.; Porter, J.; Potukuchi, B.; Prasad, S. K.; Preghenella, R.; Prino, F.; Pruneau, C. A.; Pshenichnov, I.; Puddu, G.; Pujahari, P.; Punin, V.; Putschke, J.; Qvigstad, H.; Rachevski, A.; Raha, S.; Rak, J.; Rakotozafindrabe, A.; Ramello, L.; Raniwala, R.; Raniwala, S.; Räsänen, S. S.; Rascanu, B. T.; Rathee, D.; Rauf, A. W.; Razazi, V.; Read, K. F.; Real, J. S.; Redlich, K.; Reed, R. J.; Rehman, A.; Reichelt, P.; Reicher, M.; Reidt, F.; Renfordt, R.; Reolon, A. R.; Reshetin, A.; Rettig, F.; Revol, J.-P.; Reygers, K.; Riabov, V.; Ricci, R. A.; Richert, T.; Richter, M.; Riedler, P.; Riegler, W.; Riggi, F.; Rivetti, A.; Rocco, E.; Rodríguez Cahuantzi, M.; Rodriguez Manso, A.; Røed, K.; Rogochaya, E.; Rohni, S.; Rohr, D.; Röhrich, D.; Romita, R.; Ronchetti, F.; Ronflette, L.; Rosnet, P.; Rossi, A.; Roukoutakis, F.; Roy, A.; Roy, C.; Roy, P.; Rubio Montero, A. J.; Rui, R.; Russo, R.; Ryabinkin, E.; Ryabov, Y.; Rybicki, A.; Sadovsky, S.; Šafařík, K.; Sahlmuller, B.; Sahoo, R.; Sahu, P. K.; Saini, J.; Sakai, S.; Salgado, C. A.; Salzwedel, J.; Sambyal, S.; Samsonov, V.; Sanchez Castro, X.; Sánchez Rodríguez, F. J.; Šándor, L.; Sandoval, A.; Sano, M.; Santagati, G.; Sarkar, D.; Scapparone, E.; Scarlassara, F.; Scharenberg, R. P.; Schiaua, C.; Schicker, R.; Schmidt, C.; Schmidt, H. R.; Schuchmann, S.; Schukraft, J.; Schulc, M.; Schuster, T.; Schutz, Y.; Schwarz, K.; Schweda, K.; Scioli, G.; Scomparin, E.; Scott, R.; Segato, G.; Seger, J. E.; Sekiguchi, Y.; Selyuzhenkov, I.; Seo, J.; Serradilla, E.; Sevcenco, A.; Shabetai, A.; Shabratova, G.; Shahoyan, R.; Shangaraev, A.; Sharma, N.; Sharma, S.; Shigaki, K.; Shtejer, K.; Sibiriak, Y.; Siddhanta, S.; Siemiarczuk, T.; Silvermyr, D.; Silvestre, C.; Simatovic, G.; Singaraju, R.; Singh, R.; Singha, S.; Singhal, V.; Sinha, B. C.; Sinha, T.; Sitar, B.; Sitta, M.; Skaali, T. B.; Skjerdal, K.; Slupecki, M.; Smirnov, N.; Snellings, R. J. M.; Søgaard, C.; Soltz, R.; Song, J.; Song, M.; Soramel, F.; Sorensen, S.; Spacek, M.; Spiriti, E.; Sputowska, I.; Spyropoulou-Stassinaki, M.; Srivastava, B. K.; Stachel, J.; Stan, I.; Stefanek, G.; Steinpreis, M.; Stenlund, E.; Steyn, G.; Stiller, J. H.; Stocco, D.; Stolpovskiy, M.; Strmen, P.; Suaide, A. A. P.; Sugitate, T.; Suire, C.; Suleymanov, M.; Sultanov, R.; Šumbera, M.; Susa, T.; Symons, T. J. M.; Szabo, A.; Szanto de Toledo, A.; Szarka, I.; Szczepankiewicz, A.; Szymanski, M.; Takahashi, J.; Tangaro, M. A.; Tapia Takaki, J. D.; Tarantola Peloni, A.; Tarazona Martinez, A.; Tarzila, M. G.; Tauro, A.; Tejeda Muñoz, G.; Telesca, A.; Terrevoli, C.; Thäder, J.; Thomas, D.; Tieulent, R.; Timmins, A. R.; Toia, A.; Trubnikov, V.; Trzaska, W. H.; Tsuji, T.; Tumkin, A.; Turrisi, R.; Tveter, T. S.; Ullaland, K.; Uras, A.; Usai, G. L.; Vajzer, M.; Vala, M.; Valencia Palomo, L.; Vallero, S.; Vande Vyvre, P.; Van Der Maarel, J.; Van Hoorne, J. W.; van Leeuwen, M.; Vargas, A.; Vargyas, M.; Varma, R.; Vasileiou, M.; Vasiliev, A.; Vechernin, V.; Veldhoen, M.; Velure, A.; Venaruzzo, M.; Vercellin, E.; Vergara Limón, S.; Vernet, R.; Verweij, M.; Vickovic, L.; Viesti, G.; Viinikainen, J.; Vilakazi, Z.; Villalobos Baillie, O.; Vinogradov, A.; Vinogradov, L.; Vinogradov, Y.; Virgili, T.; Viyogi, Y. P.; Vodopyanov, A.; Völkl, M. A.; Voloshin, K.; Voloshin, S. A.; Volpe, G.; von Haller, B.; Vorobyev, I.; Vranic, D.; Vrláková, J.; Vulpescu, B.; Vyushin, A.; Wagner, B.; Wagner, J.; Wagner, V.; Wang, M.; Wang, Y.; Watanabe, D.; Weber, M.; Wessels, J. P.; Westerhoff, U.; Wiechula, J.; Wikne, J.; Wilde, M.; Wilk, G.; Wilkinson, J.; Williams, M. C. S.; Windelband, B.; Winn, M.; Yaldo, C. G.; Yamaguchi, Y.; Yang, H.; Yang, P.; Yang, S.; Yano, S.; Yasnopolskiy, S.; Yi, J.; Yin, Z.; Yoo, I.-K.; Yushmanov, I.; Zaccolo, V.; Zach, C.; Zaman, A.; Zampolli, C.; Zaporozhets, S.; Zarochentsev, A.; Závada, P.; Zaviyalov, N.; Zbroszczyk, H.; Zgura, I. S.; Zhalov, M.; Zhang, H.; Zhang, X.; Zhang, Y.; Zhao, C.; Zhigareva, N.; Zhou, D.; Zhou, F.; Zhou, Y.; Zhou, Zhuo; Zhu, H.; Zhu, J.; Zhu, X.; Zichichi, A.; Zimmermann, A.; Zimmermann, M. B.; Zinovjev, G.; Zoccarato, Y.; Zyzak, M.</p> <p>2015-06-01</p> <p>The <span class="hlt">elliptic</span> flow coefficient ( v 2) of identified particles in Pb-Pb collisions at TeV was measured with the ALICE detector at the Large Hadron Collider (LHC). The results were obtained with the Scalar Product method, a two-particle <span class="hlt">correlation</span> technique, using a pseudo-rapidity gap of |Δ η| > 0 .9 between the identified hadron under study and the reference particles. The v 2 is reported for π ±, K±, K{S/0}, , ϕ, , and in several collision centralities. In the low transverse momentum ( p T) region, p T < 3 GeV/ c, v 2( p T) exhibits a particle mass dependence consistent with <span class="hlt">elliptic</span> flow accompanied by the transverse radial expansion of the system with a common velocity field. The experimental data for π ± and the combined K± and K{S/0} results, are described fairly well by hydrodynamic calculations coupled to a hadronic cascade model (VISHNU) for central collisions. However, the same calculations fail to reproduce the v 2( p T) for , ϕ, and . For transverse momentum values larger than about 3 GeV/ c, particles tend to group according to their type, i.e. mesons and baryons. The present measurements exhibit deviations from the number of constituent quark (NCQ) scaling at the level of ±20% for p T > 3 GeV/ c. [Figure not available: see fulltext.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017NatSR...744370S','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017NatSR...744370S"><span id="translatedtitle"><span class="hlt">Intrinsic</span> optimization using stochastic nanomagnets</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Sutton, Brian; Camsari, Kerem Yunus; Behin-Aein, Behtash; Datta, Supriyo</p> <p>2017-03-01</p> <p>This paper draws attention to a hardware system which can be engineered so that its <span class="hlt">intrinsic</span> physics is described by the generalized Ising model and can encode the solution to many important NP-hard problems as its ground state. The basic constituents are stochastic nanomagnets which switch randomly between the ±1 Ising states and can be monitored continuously with standard electronics. Their mutual interactions can be short or long range, and their strengths can be reconfigured as needed to solve specific problems and to anneal the system at room temperature. The natural laws of statistical mechanics guide the network of stochastic nanomagnets at GHz speeds through the collective states with an emphasis on the low energy states that represent optimal solutions. As proof-of-concept, we present simulation results for standard NP-complete examples including a 16-city traveling salesman problem using experimentally benchmarked models for spin-transfer torque driven stochastic nanomagnets.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=5353626','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=5353626"><span id="translatedtitle"><span class="hlt">Intrinsic</span> optimization using stochastic nanomagnets</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Sutton, Brian; Camsari, Kerem Yunus; Behin-Aein, Behtash; Datta, Supriyo</p> <p>2017-01-01</p> <p>This paper draws attention to a hardware system which can be engineered so that its <span class="hlt">intrinsic</span> physics is described by the generalized Ising model and can encode the solution to many important NP-hard problems as its ground state. The basic constituents are stochastic nanomagnets which switch randomly between the ±1 Ising states and can be monitored continuously with standard electronics. Their mutual interactions can be short or long range, and their strengths can be reconfigured as needed to solve specific problems and to anneal the system at room temperature. The natural laws of statistical mechanics guide the network of stochastic nanomagnets at GHz speeds through the collective states with an emphasis on the low energy states that represent optimal solutions. As proof-of-concept, we present simulation results for standard NP-complete examples including a 16-city traveling salesman problem using experimentally benchmarked models for spin-transfer torque driven stochastic nanomagnets. PMID:28295053</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/443449','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/443449"><span id="translatedtitle">Profibus features <span class="hlt">intrinsic</span> safety, interoperability</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Bryant, M.</p> <p>1996-11-01</p> <p>The newest member of the Profibus (process fieldbus) family of interoperable field-bus protocols is {open_quotes}PA{close_quotes}, an <span class="hlt">intrinsically</span> safe (IS) standard released more than a year ago. IS and non-IS plants using PA for process chemicals, energy production, and food manufacturing are coming online. PA was developed by vendor and user members of the Profibus standards community to meet the needs of customers in the process industries. PA complies with IEC 1158-2, which, among non-IS capabilities, specifies a low-speed, <span class="hlt">intrinsically</span> safe fieldbus for automating explosive chemical manufacturing. PA thus provides all H1, or {open_quotes}hunk{close_quotes} 1, IS and non-IS services. Importantly, it also provides all H2, or {open_quotes}hunk{close_quotes} 2, services. As the newest segment of the site-proven system of fieldbus protocols, Profibus-PA defines by example the concepts of interoperability and interchangeability. It is a field instrument network that automatically interoperates with a large installed base of fieldbus nodes. As low-speed networks, PA and its competitor, Foundation fieldbus H1 comply with the same standard. They do the same job; auxiliary power to the application, with a data rate of 31.25 kbit/sec. Similarities include a function-block-based architecture and a device description language (DDL). They use the same physical layer for digital data transfer. A casual observer would find PA and H1 virtually the same. The key differences are in the protocol implementations. Although PA and H1 could be wired together, the messages delivered by one would make no sense to the other. At least not yet. PA protocols are capable of both IS and non-IS operations. This opens the door to a wide range of interoperable process-manufacturing requirements. 1 fig., 1 tab.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/26427063','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/26427063"><span id="translatedtitle"><span class="hlt">Intrinsic</span> Multi-Scale Dynamic Behaviors of Complex Financial Systems.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Ouyang, Fang-Yan; Zheng, Bo; Jiang, Xiong-Fei</p> <p>2015-01-01</p> <p>The empirical mode decomposition is applied to analyze the <span class="hlt">intrinsic</span> multi-scale dynamic behaviors of complex financial systems. In this approach, the time series of the price returns of each stock is decomposed into a small number of <span class="hlt">intrinsic</span> mode functions, which represent the price motion from high frequency to low frequency. These <span class="hlt">intrinsic</span> mode functions are then grouped into three modes, i.e., the fast mode, medium mode and slow mode. The probability distribution of returns and auto-<span class="hlt">correlation</span> of volatilities for the fast and medium modes exhibit similar behaviors as those of the full time series, i.e., these characteristics are rather robust in multi time scale. However, the cross-<span class="hlt">correlation</span> between individual stocks and the return-volatility <span class="hlt">correlation</span> are time scale dependent. The structure of business sectors is mainly governed by the fast mode when returns are sampled at a couple of days, while by the medium mode when returns are sampled at dozens of days. More importantly, the leverage and anti-leverage effects are dominated by the medium mode.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=2680293','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=2680293"><span id="translatedtitle">Dissociable <span class="hlt">Intrinsic</span> Connectivity Networks for Salience Processing and Executive Control</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Seeley, William W.; Menon, Vinod; Schatzberg, Alan F.; Keller, Jennifer; Glover, Gary H.; Kenna, Heather; Reiss, Allan L.; Greicius, Michael D.</p> <p>2008-01-01</p> <p>Variations in neural circuitry, inherited or acquired, may underlie important individual differences in thought, feeling, and action patterns. Here, we used task-free connectivity analyses to isolate and characterize two distinct networks typically coactivated during functional MRI tasks. We identified a “salience network,” anchored by dorsal anterior cingulate (dACC) and orbital frontoinsular cortices with robust connectivity to subcortical and limbic structures, and an “executive-control network” that links dorsolateral frontal and parietal neocortices. These <span class="hlt">intrinsic</span> connectivity networks showed dissociable <span class="hlt">correlations</span> with functions measured outside the scanner. Prescan anxiety ratings <span class="hlt">correlated</span> with <span class="hlt">intrinsic</span> functional connectivity of the dACC node of the salience network, but with no region in the executive-control network, whereas executive task performance <span class="hlt">correlated</span> with lateral parietal nodes of the executive-control network, but with no region in the salience network. Our findings suggest that task-free analysis of <span class="hlt">intrinsic</span> connectivity networks may help elucidate the neural architectures that support fundamental aspects of human behavior. PMID:17329432</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/23602010','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/23602010"><span id="translatedtitle">Relationship between placental traits and maternal <span class="hlt">intrinsic</span> factors in sheep.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Ocak, S; Ogun, S; Onder, H</p> <p>2013-06-01</p> <p>The relationship between maternal <span class="hlt">intrinsic</span> factors and placental traits was investigated on three Southern Mediterranean breed of sheep; Cukurova Assaf (CA), Cukurova (C) and Cukurova Meat Sheep (CMS). The effect of parity and birth type were also considered in the study as a potential influencing factor. Our hypothesis was to show that while differences in placental traits between breed, parity and birth type affected lamb condition and survivability, its <span class="hlt">correlation</span> to maternal <span class="hlt">intrinsic</span> behavioral factors may also be a strong indicator. The study found breed related differences of maternal behavioral factors and also showed significant <span class="hlt">correlation</span> of these behavioral patterns to various placental traits. It confirmed earlier findings that parity played a major role in the refinement of these behavioral patterns. Significant differences in birth weight (P<0.05), placental weight (P<0.05), number of cotyledons (P<0.01) and cotyledon length (P<0.05) was seen between breeds. Cotyledon weight (P<0.05), width (P<0.01) and length (P<0.05) were found to differ by parity. Breed and parity interaction significantly influenced cotyledon quantity. While we detected breed specific differences in relation to maternal <span class="hlt">intrinsic</span> factors we also noticed significant variance within breeds to these behavioral patterns when linked to placental traits. Further study is required on the <span class="hlt">correlation</span> between placental traits and postnatal behavior on not just the ewes but also on their lambs. This could have a significant bearing on how producers manage and maximize lamb survivability.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4591268','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4591268"><span id="translatedtitle"><span class="hlt">Intrinsic</span> Multi-Scale Dynamic Behaviors of Complex Financial Systems</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Ouyang, Fang-Yan; Zheng, Bo; Jiang, Xiong-Fei</p> <p>2015-01-01</p> <p>The empirical mode decomposition is applied to analyze the <span class="hlt">intrinsic</span> multi-scale dynamic behaviors of complex financial systems. In this approach, the time series of the price returns of each stock is decomposed into a small number of <span class="hlt">intrinsic</span> mode functions, which represent the price motion from high frequency to low frequency. These <span class="hlt">intrinsic</span> mode functions are then grouped into three modes, i.e., the fast mode, medium mode and slow mode. The probability distribution of returns and auto-<span class="hlt">correlation</span> of volatilities for the fast and medium modes exhibit similar behaviors as those of the full time series, i.e., these characteristics are rather robust in multi time scale. However, the cross-<span class="hlt">correlation</span> between individual stocks and the return-volatility <span class="hlt">correlation</span> are time scale dependent. The structure of business sectors is mainly governed by the fast mode when returns are sampled at a couple of days, while by the medium mode when returns are sampled at dozens of days. More importantly, the leverage and anti-leverage effects are dominated by the medium mode. PMID:26427063</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/23037070','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/23037070"><span id="translatedtitle">Imprints of the molecular-orbital geometry on the high-harmonic <span class="hlt">ellipticity</span>.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Qin, Meiyan; Zhu, Xiaosong; Liu, Kunlong; Zhang, Qingbin; Lu, Peixiang</p> <p>2012-08-27</p> <p>The influence of the orbital symmetry on the <span class="hlt">ellipticity</span> of the high-order harmonics is investigated. It is found that the <span class="hlt">ellipticity</span> maps have distinct shapes for the molecular orbitals with different symmetry. Our analysis shows that the feature of the harmonic <span class="hlt">ellipticity</span> map is essentially determined by the nodal structure of the nonsymmetric orbital. The results indicate that the molecular-orbital geometry is imprinted on the <span class="hlt">ellipticity</span> of the high-order harmonics, which invites the use of <span class="hlt">ellipticity</span> measurements as a probe of the orbital structure for polar molecules.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/25426508','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/25426508"><span id="translatedtitle">Validity of arm-leg <span class="hlt">elliptical</span> ergometer for VO2max analysis.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Brown, Andrew B; Kueffner, Tannin E; OʼMahony, Erin C; Lockard, Michael M</p> <p>2015-06-01</p> <p>Maximal oxygen consumption ((Equation is included in full-text article.)) can be determined through multiple exercise modalities intended to elicit an individual's maximal aerobic exertion. Uphill treadmill running is considered the best modality for measuring (Equation is included in full-text article.). Previous studies have examined <span class="hlt">correlations</span> between treadmill and <span class="hlt">elliptical</span> ergometer tests as well as the cycle ergometer, but none of the studies use an arm-leg <span class="hlt">elliptical</span> ergometer (ALE). The purpose of this study was to develop an ALE (Equation is included in full-text article.)testing protocol and determine whether ALE produces valid (Equation is included in full-text article.)values as compared with the treadmill. Twelve undergraduate students (mean age: 20.8 years) completed 2 (Equation is included in full-text article.)tests, 1 on a treadmill and 1 on ALE. (Equation is included in full-text article.)<span class="hlt">correlation</span> between ALE and treadmill was examined, and paired t-tests were run for (Equation is included in full-text article.)and maximum heart rate (HRmax). A strong positive <span class="hlt">correlation</span> was found between ALE and treadmill (Equation is included in full-text article.)values (r = 0.84; p < 0.001). There were no differences between (Equation is included in full-text article.)values; however, HRmax values were higher on the treadmill than ALE (p = 0.003). Although future research is needed to examine the observed differences in HRmax between the 2 testing modalities and gender differences in muscle recruitment patterns, the results of this study suggest that ALE is a valid modality for (Equation is included in full-text article.)testing. This will be particularly valuable as a clinical tool to assess (Equation is included in full-text article.)in populations requiring low-impact exercise.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://files.eric.ed.gov/fulltext/ED341080.pdf','ERIC'); return false;" href="http://files.eric.ed.gov/fulltext/ED341080.pdf"><span id="translatedtitle">Back to the Definitions Themselves: The Pragmatics of <span class="hlt">Intrinsic</span> Justification.</span></a></p> <p><a target="_blank" href="http://www.eric.ed.gov/ERICWebPortal/search/extended.jsp?_pageLabel=advanced">ERIC Educational Resources Information Center</a></p> <p>Bahm, Kenneth</p> <p></p> <p>Such terms as "<span class="hlt">intrinsic</span> justification,""<span class="hlt">intrinsicness</span>," and "<span class="hlt">intrinsicality</span>" are increasingly being heard in academic debate circles. <span class="hlt">Intrinsic</span> justification consists of an argument which focuses evaluation of a resolutional term on the term's definitional contours. Essential qualities are defining characteristics…</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2012JAMDS...6..498L','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2012JAMDS...6..498L"><span id="translatedtitle">Vibration and Noise Characteristics of <span class="hlt">Elliptical</span> Gears due to Non-Uniform Rotation</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Liu, Xing; Nagamura, Kazuteru; Ikejo, Kiyotaka</p> <p></p> <p><span class="hlt">Elliptical</span> gear is a typical non-circular gear, which transmits a variable-ratio rotation and power simultaneously. Due to the non-uniform rotation, the vibration and noise of <span class="hlt">elliptical</span> gears demonstrate particular characteristics which should be paid attention to in practical application. In this paper, two <span class="hlt">elliptical</span> gears, which are a single <span class="hlt">elliptical</span> gear and a double <span class="hlt">elliptical</span> gear, have been investigated to analyze the vibration and noise characteristics of <span class="hlt">elliptical</span> gears. The corresponding circular gears for comparison are also investigated. General factors including the torque, the rotation speed, the gear vibration acceleration and the gear noise of the four test gears are measured by running test. The root mean square of the Circumferential Vibration Acceleration (CVA) and the sound pressure level of the noise of <span class="hlt">elliptical</span> gears are obtained from the measured results and compared with those of circular gears to clarify the vibration and noise characteristics of <span class="hlt">elliptical</span> gears. Furthermore, the frequency analysis of the CVA of <span class="hlt">elliptical</span> gears is conducted by Fast Fourier Transform Algorithm (FFT) and compared with that of circular gears. The main vibration component of <span class="hlt">elliptical</span> gear is uncovered according to the obtained frequency spectra. In addition, the Critical Rotation Speeds of Tooth Separation (CRSTS) of <span class="hlt">elliptical</span> gear is obtained and its relation with load torque is unveiled.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/19251339','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/19251339"><span id="translatedtitle">Buying into conservation: <span class="hlt">intrinsic</span> versus instrumental value.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Justus, James; Colyvan, Mark; Regan, Helen; Maguire, Lynn</p> <p>2009-04-01</p> <p>Many conservation biologists believe the best ethical basis for conserving natural entities is their claimed <span class="hlt">intrinsic</span> value, not their instrumental value for humans. But there is significant confusion about what <span class="hlt">intrinsic</span> value is and how it could govern conservation decision making. After examining what <span class="hlt">intrinsic</span> value is supposed to be, we argue that it cannot guide the decision making conservation requires. An adequate ethical basis for conservation must do this, and instrumental value does it best.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2014JOpt...16g5704Z','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2014JOpt...16g5704Z"><span id="translatedtitle">Random source generating far field with <span class="hlt">elliptical</span> flat-topped beam profile</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Zhang, Yongtao; Cai, Yangjian</p> <p>2014-07-01</p> <p>Circular and rectangular multi-Gaussian Schell-model (MGSM) sources which generate far fields with circular and rectangular flat-topped beam profiles were introduced just recently (Sahin and Korotkova 2012 Opt. Lett. 37 2970; Korotkova 2014 Opt. Lett. 39 64). In this paper, a random source named an <span class="hlt">elliptical</span> MGSM source is introduced. An analytical expression for the propagation factor of an <span class="hlt">elliptical</span> MGSM beam is derived. Furthermore, an analytical propagation formula for an <span class="hlt">elliptical</span> MGSM beam passing through a stigmatic ABCD optical system is derived, and its propagation properties in free space are studied. It is interesting to find that an <span class="hlt">elliptical</span> MGSM source generates a far field with an <span class="hlt">elliptical</span> flat-topped beam profile, being qualitatively different from that of circular and rectangular MGSM sources. The <span class="hlt">ellipticity</span> and the flatness of the <span class="hlt">elliptical</span> flat-topped beam profile in the far field are determined by the initial coherence widths and the beam index, respectively.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://www.osti.gov/scitech/servlets/purl/762126','SCIGOV-STC'); return false;" href="http://www.osti.gov/scitech/servlets/purl/762126"><span id="translatedtitle">Issues in Purchasing and Maintaining <span class="hlt">Intrinsic</span> Standards</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>PETTIT,RICHARD B.; JAEGER,KLAUS; EHRLICH,CHARLES D.</p> <p>2000-09-12</p> <p><span class="hlt">Intrinsic</span> standards are widely used in the metrology community because they realize the best level uncertainty for many metrology parameters. For some <span class="hlt">intrinsic</span> standards, recommended practices have been developed to assist metrologists in the selection of equipment and the development of appropriate procedures in order to realize the <span class="hlt">intrinsic</span> standard. As with the addition of any new standard, the metrology laboratory should consider the pros and cons relative to their needs before purchasing the standard so that the laboratory obtains the maximum benefit from setting up and maintaining these standards. While the specific issues that need to be addressed depend upon the specific <span class="hlt">intrinsic</span> standard and the level of realization, general issues that should be considered include ensuring that the <span class="hlt">intrinsic</span> standard is compatible with the laboratory environment, that the standard is compatible with the current and future workload, and whether additional support standards will be required in order to properly maintain the <span class="hlt">intrinsic</span> standard. When <span class="hlt">intrinsic</span> standards are used to realize the best level of uncertainty for a specific metrology parameter, they usually require critical and important maintenance activities. These activities can including training of staff in the system operation, as well as safety procedures; performing periodic characterization measurements to ensure proper system operation; carrying out periodic intercomparisons with similar <span class="hlt">intrinsic</span> standards so that proper operation is demonstrated; and maintaining control or trend charts of system performance. This paper has summarized many of these important issues and therefore should be beneficial to any laboratory that is considering the purchase of an <span class="hlt">intrinsic</span> standard.</p> </li> </ol> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_15");'>15</a></li> <li><a href="#" onclick='return showDiv("page_16");'>16</a></li> <li class="active"><span>17</span></li> <li><a href="#" onclick='return showDiv("page_18");'>18</a></li> <li><a href="#" onclick='return showDiv("page_19");'>19</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div><!-- col-sm-12 --> </div><!-- row --> </div><!-- page_17 --> <div id="page_18" class="hiddenDiv"> <div class="row"> <div class="col-sm-12"> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_16");'>16</a></li> <li><a href="#" onclick='return showDiv("page_17");'>17</a></li> <li class="active"><span>18</span></li> <li><a href="#" onclick='return showDiv("page_19");'>19</a></li> <li><a href="#" onclick='return showDiv("page_20");'>20</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div> </div> <div class="row"> <div class="col-sm-12"> <ol class="result-class" start="341"> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2004AAS...205.9205S','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2004AAS...205.9205S"><span id="translatedtitle">The Observability of Abundance Ratio Effects in <span class="hlt">Elliptical</span> Galaxies</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Serven, J. L.; Worthey, G.; Briley, M. M.</p> <p>2004-12-01</p> <p>Using synthetic spectra we construct a simple model of an <span class="hlt">elliptical</span> galaxy, with a velocity dispersion σ = 200 km s-1. Absorption feature indices are defined for C, N, O, Na, Mg, Al, Si, S, K, Ca, Sc, Ti, V, Cr, Mn, Fe, Co, Ni, Cu, Zn, Sr, Ba, and Eu as a first step in determining the abundances of these elements in stellar populations, such as <span class="hlt">elliptical</span> galaxies, for which integrated light spectra are available. Then using these indices and assuming a photon error such that S/N = 100 around 5000 Å , the feasibility of measuring individual elements in real galaxies is assessed. Of the elements studied only S, K, Cu, Zn, and Eu appear to be difficult to determine; the rest appear to be at least feasible.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016JOpt...18b5602A','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016JOpt...18b5602A"><span id="translatedtitle">Propagation of light in a circular array of <span class="hlt">elliptical</span> fibres</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Alexeyev, C. N.; Milione, G.; Pogrebnaya, A. O.; Yavorsky, M. A.</p> <p>2016-02-01</p> <p>We have studied transformation of discrete light beams in circular arrays of <span class="hlt">elliptical</span> fibres, in which the orientation of ellipses' axes linearly depends on the angular position of the fibre in the array and makes an half-integer number p of full rotations while tracing along its contour. We have derived analytical expressions for the spectra and supermodes that allow for evanescent coupling between the fibres in the next-neighbour approximation. We have studied the transformative properties of such an array and shown that it can generate cylindrical vector beams (CVBs) of TE and TM types. We have shown that the type of generated beam depends on the orientation of linear polarization of the incident beam. In this way, the circular array of strongly <span class="hlt">elliptical</span> fibres enables polarization control over the type of the generated CVB. We have also shown that such arrays can change the topological charge of an incoming discrete optical vortex by the doubled array's index p.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/975435','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/975435"><span id="translatedtitle">Tailoring the magnetization reversal of <span class="hlt">elliptical</span> dots using exchange bias.</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Sort, J.; Buchanan, K. S.; Pearson, J. E.; Hoffmann, A.; Menendez, E.; Salazar-Alvarez, G.; Baro, M. D.; Miron, M.; Rodamcq, B.; Dieny, B.; ICREA; Univ. Autonoma of Barcelona; Insti. Catala de Nanotecnologia; SPINTEC</p> <p>2008-01-01</p> <p>Exchange bias effects have been studied in <span class="hlt">elliptical</span> dots composed of ferromagnetic Ni{sub 80}Fe{sub 20}-antiferromagnetic Ir{sub 20}Mn{sub 80} bilayers. The magnetization reversal mechanisms and magnetic configurations have been investigated by magneto-optic Kerr effect and magnetic force microscopy. Although the obtained bias fields in these dots are relatively small, the magnetization reversal is found to be influenced by the ferromagnetic-antiferromagnetic coupling. Namely, for some off-axis angles of measurement, the magnetization reversal mechanism of the Ni{sub 80}Fe{sub 20}-Ir{sub 20}Mn{sub 80} ellipses depends on whether exchange bias is induced along the minor or major axis of the ellipses. Hence, exchange bias is shown to be an effective means for tailoring the magnetization reversal of <span class="hlt">elliptical</span> dots after sample fabrication.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4926562','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4926562"><span id="translatedtitle">Is the Capsular Bag Perimeter Round or <span class="hlt">Elliptical</span>?</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Amigó, Alfredo; Bonaque-González, Sergio</p> <p>2016-01-01</p> <p>Purpose: To report findings that could suggest an <span class="hlt">elliptical</span> shape of the capsular bag. Methods: Five eyes of three patients with axial length greater than 24 mm underwent phacoemulsification cataract surgery with plate-haptic multifocal toric intraocular lens (IOL) implantation oriented in the vertical meridian. Results: In all cases, correct orientation of the IOLs was verified 30 minutes after surgery. After 24 hours, all eyes demonstrated unwanted rotation of the IOLs ranging from 15 to 45 degrees. The IOLs remained stable in the new position in all cases until adhesion of the capsular bag took place. Conclusion: These observations could suggest that the perimeter of the capsular bag has an <span class="hlt">elliptical</span> shape. Therefore, the IOL tends to become fixated in a meridian of the capsular bag that best fits the diagonal diameter of the IOL. PMID:27413495</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017IJMPB..3150244Y','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017IJMPB..3150244Y"><span id="translatedtitle">Design of <span class="hlt">elliptic</span> cylindrical thermal cloak with layered structure</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Yuan, Xuebo; Lin, Guochang; Wang, Youshan</p> <p>2017-01-01</p> <p>Thermal cloak has potential applications in thermal protection and sensing. Based on the theories of spatial transformation and effective medium, layered structure of <span class="hlt">elliptic</span> cylindrical thermal cloak was designed. According to theoretical analysis and numerical simulation, the layered structure has typical characteristics of perfect thermal cloak. The external temperature field remains unchanged, while the internal temperature gradient decreases obviously. Meanwhile, the cloaking effect is stable in any direction. The cloaking effect can be improved by increasing the number of discretization layers or reducing the cloak thickness. The <span class="hlt">elliptic</span> cylindrical cloak can be considered as cylindrical cloak when the focal distance is close to zero. This study has provided an effective way for realizing thermal cloak with more complex shapes.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2012ascl.soft03008T','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2012ascl.soft03008T"><span id="translatedtitle">MegaLUT: Correcting <span class="hlt">ellipticity</span> measurements of galaxies</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Tewes, Malte; Cantale, Nicolas; Courbin, Frédéric; Kitching, Thomas; Meylan, Georges</p> <p>2012-03-01</p> <p>MegaLUT is a simple and fast method to correct <span class="hlt">ellipticity</span> measurements of galaxies from the distortion by the instrumental and atmospheric point spread function (PSF), in view of weak lensing shear measurements. The method performs a classification of galaxies and associated PSFs according to measured shape parameters, and builds a lookup table of <span class="hlt">ellipticity</span> corrections by supervised learning. This new method has been applied to the GREAT10 image analysis challenge, and demonstrates a refined solution that obtains the highly competitive quality factor of Q = 142, without any power spectrum denoising or training. Of particular interest is the efficiency of the method, with a processing time below 3 ms per galaxy on an ordinary CPU.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4851091','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4851091"><span id="translatedtitle">A New <span class="hlt">Elliptical</span> Model for Device-Free Localization</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Lei, Qian; Zhang, Haijian; Sun, Hong; Tang, Linling</p> <p>2016-01-01</p> <p>Device-free localization (DFL) based on wireless sensor networks (WSNs) is expected to detect and locate a person without the need for any wireless devices. Radio tomographic imaging (RTI) has attracted wide attention from researchers as an emerging important technology in WSNs. However, there is much room for improvement in localization estimation accuracy. In this paper, we propose a geometry-based <span class="hlt">elliptical</span> model and adopt the orthogonal matching pursuit (OMP) algorithm. The new <span class="hlt">elliptical</span> model uses not only line-of-sight information, but also non-line-of-sight information, which divides one ellipse into several areas with different weights. Meanwhile the OMP, which can eliminate extra bright spots in image reconstruction, is used to derive an image estimator. The experimental results demonstrate that the proposed algorithm could improve the accuracy of positioning by up to 23.8% for one person and 33.3% for two persons over some state-of-the-art RTI methods. PMID:27110788</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/227912','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/227912"><span id="translatedtitle">Power loss in electrical steel under <span class="hlt">elliptically</span> rotating flux conditions</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Salz, W.; Hempel, K.A.</p> <p>1996-03-01</p> <p>The power loss of electrical steel sheet given in the data sheets of the steel manufacturers is related to linearly alternating flux conditions, measured with an Epstein frame or a single sheet tester, respectively. In the application of the material in electrical machines, the authors find large areas with rotational flux conditions, i.e., in the T-joint region of three-phase power transformers or above the stator teeth of three-phase motors and generators. The most general description of the magnetization process in this case is an <span class="hlt">elliptically</span> rotating flux. The paper outlines the magnetic behavior of steel sheet under these flux conditions, and finally defines a simple method to predict the total power loss under <span class="hlt">elliptically</span> rotating flux from data measured under linearly alternating and circularly rotating flux conditions only.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/6931781','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/6931781"><span id="translatedtitle">Analysis of multigrid algorithms for nonsymmetric and indefinite <span class="hlt">elliptic</span> problems</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Bramble, J.H.; Pasciak, J.E.; Xu, J.</p> <p>1988-10-01</p> <p>We prove some new estimates for the convergence of multigrid algorithms applied to nonsymmetric and indefinite <span class="hlt">elliptic</span> boundary value problems. We provide results for the so-called 'symmetric' multigrid schemes. We show that for the variable V-script-cycle and the W-script-cycle schemes, multigrid algorithms with any amount of smoothing on the finest grid converge at a rate that is independent of the number of levels or unknowns, provided that the initial grid is sufficiently fine. We show that the V-script-cycle algorithm also converges (under appropriate assumptions on the coarsest grid) but at a rate which may deteriorate as the number of levels increases. This deterioration for the V-script-cycle may occur even in the case of full <span class="hlt">elliptic</span> regularity. Finally, the results of numerical experiments are given which illustrate the convergence behavior suggested by the theory.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/17359084','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/17359084"><span id="translatedtitle">Void <span class="hlt">ellipticity</span> distribution as a probe of cosmology.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Park, Daeseong; Lee, Jounghun</p> <p>2007-02-23</p> <p>Cosmic voids refer to the large empty regions in the Universe with a very low number density of galaxies. Voids are likely to be severely disturbed by the tidal effect from the surrounding dark matter. We derive a completely analytic model for the void <span class="hlt">ellipticity</span> distribution from physical principles. We use the spatial distribution of galaxies in a void as a measure of its shape, tracking the trajectory of the void galaxies under the influence of the tidal field using Lagrangian perturbation theory. Our model implies that the void <span class="hlt">ellipticity</span> distribution depends sensitively on the cosmological parameters. Testing our model against the high-resolution Millennium Run simulation, we find excellent quantitative agreements of the analytic predictions with the numerical results.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2010IEITF..93.1140D','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2010IEITF..93.1140D"><span id="translatedtitle">Sole Inversion Precomputation for <span class="hlt">Elliptic</span> Curve Scalar Multiplications</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Dahmen, Erik; Okeya, Katsuyuki</p> <p></p> <p>This paper presents a new approach to precompute points [3]P, [5]P, ..., [2k-1]P, for some k ≥ 2 on an <span class="hlt">elliptic</span> curve over \\mathbb{F}_p. Those points are required for the efficient evaluation of a scalar multiplication, the most important operation in <span class="hlt">elliptic</span> curve cryptography. The proposed method precomputes the points in affine coordinates and needs only one single field inversion for the computation. The new method is superior to all known methods that also use one field inversion, if the required memory is taken into consideration. Compared to methods that require several field inversions for the precomputation, the proposed method is faster for a broad range of ratios of field inversions and field multiplications. The proposed method benefits especially from ratios as they occur on smart cards.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2013hsa7.conf..455P','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2013hsa7.conf..455P"><span id="translatedtitle">Contribution of minor mergers to the growth of <span class="hlt">elliptical</span> galaxies</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Peralta de Arriba, L.; Balcells, M.; Trujillo, I.; Falcón-Barroso, J.</p> <p>2013-05-01</p> <p>Size evolution studies have shown that the structural properties of the <span class="hlt">elliptical</span> galaxies dramatically changed with cosmic time (e. g. Trujillo et al. 2007). This result challenges the ideas developed from the detailed analyses of the stellar populations of these galaxies in the nearby universe. The study of the local <span class="hlt">elliptical</span> galaxies has revealed their stars are old, and formed over short-timescales (see the review by Renzini 2006). In order to resolve this discrepancy, it has been hypothesized that new material continuously accretes in minor merger events (Naab et al. 2007). Index-index diagrams are a promising way to probe the minor merger scenario. However, a large sample of galaxies is required for this goal. In this poster we present our preliminary index measurements of a subsample of galaxies studied by Trujillo et al. (2007) using the spectra published by the DEEP2 DR4 survey (Newman et al. 2012).</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2012RJMP...19..405A','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2012RJMP...19..405A"><span id="translatedtitle">Remarks on strongly <span class="hlt">elliptic</span> systems in Lipschitz domains</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Agranovich, M. S.</p> <p>2012-10-01</p> <p>We present some remarks to the general theory of strongly <span class="hlt">elliptic</span> second-order systems in bounded Lipschitz domains. The most important remarks are related to the use of the "Weyl decomposition" of the solution space. In particular, we suggest a simplified approach to the unique choice of the right-hand side of the system and the conormal derivative in the Neumann problem and obtain two-sided a priori estimates for the solutions. We consider the transmission problem for two systems in domains with a common Lipschitz boundary without the assumption that the coefficients do not have jumps on that boundary. We construct examples of strongly <span class="hlt">elliptic</span> second-order systems for which the Neumann problem is not Fredholm.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4676062','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4676062"><span id="translatedtitle"><span class="hlt">Intrinsic</span> Localized Modes in Proteins</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Nicolaï, Adrien; Delarue, Patrice; Senet, Patrick</p> <p>2015-01-01</p> <p>Protein dynamics is essential for proteins to function. Here we predicted the existence of rare, large nonlinear excitations, termed <span class="hlt">intrinsic</span> localized modes (ILMs), of the main chain of proteins based on all-atom molecular dynamics simulations of two fast-folder proteins and of a rigid α/β protein at 300 K and at 380 K in solution. These nonlinear excitations arise from the anharmonicity of the protein dynamics. The ILMs were detected by computing the Shannon entropy of the protein main-chain fluctuations. In the non-native state (significantly explored at 380 K), the probability of their excitation was increased by a factor between 9 and 28 for the fast-folder proteins and by a factor 2 for the rigid protein. This enhancement in the non-native state was due to glycine, as demonstrated by simulations in which glycine was mutated to alanine. These ILMs might play a functional role in the flexible regions of proteins and in proteins in a non-native state (i.e. misfolded or unfolded states). PMID:26658321</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/21560502','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/21560502"><span id="translatedtitle">RELATION BETWEEN GLOBULAR CLUSTERS AND SUPERMASSIVE BLACK HOLES IN <span class="hlt">ELLIPTICALS</span> AS A MANIFESTATION OF THE BLACK HOLE FUNDAMENTAL PLANE</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Snyder, Gregory F.; Hernquist, Lars; Hopkins, Philip F.</p> <p>2011-02-10</p> <p>We analyze the relation between the mass of the central supermassive black hole (M{sub BH}) and the number of globular clusters (N{sub GC}) in <span class="hlt">elliptical</span> galaxies and bulges as a ramification of the black hole fundamental plane, the theoretically predicted and observed multi-variable <span class="hlt">correlation</span> between M{sub BH} and bulge binding energy. Although the tightness of the M{sub BH}-N{sub GC} <span class="hlt">correlation</span> suggests an unlikely causal link between supermassive black holes and globular clusters (GCs), such a correspondence can exhibit small scatter even if the physical relationship is indirect. We show that the relatively small scatter of the M{sub BH}-N{sub GC} relation owes to the mutual residual <span class="hlt">correlation</span> of M{sub BH} and N{sub GC} with stellar mass when the velocity dispersion is held fixed. Thus, present observations lend evidence for feedback-regulated models in which the bulge binding energy is most important; they do not necessarily imply any 'special' connection between GCs and M{sub BH}. This raises the question of why N{sub GC} traces the formation of <span class="hlt">ellipticals</span> and bulges sufficiently well to be <span class="hlt">correlated</span> with binding energy.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2005SPIE.5699....9B','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2005SPIE.5699....9B"><span id="translatedtitle">Rapid identification of microorganisms by <span class="hlt">intrinsic</span> fluorescence</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Bhatta, Hemant; Goldys, Ewa M.; Learmonth, Robert</p> <p>2005-03-01</p> <p>Microbial contamination has serious consequences for the industries that use fermentation processes. Common contaminants such as faster growing lactic acid bacteria or wild yeast can rapidly outnumber inoculated culture yeast and produce undesirable end products. Our study focuses on a rapid method of identification of such contaminants based on autofluorescence spectroscopy of bacterial and yeast species. Lactic acid bacteria (Lac-tobacillus casei), and yeast (Saccharomyces cerevisiae) were cultured under controlled conditions and studied for variations in their autofluorescence. We observed spectral differences in the spectral range representative of tryptophan residues of proteins, with excitation at 290 nm and emission scanned in the 300 nm - 440 nm range. Excitation scans between 240 nm and 310 nm were also performed for the emission at 340 nm. Moreover, we observed clearly pronounced differences in the excitation and emission in the visible range, with 410 nm excitation. These results demonstrate that bacterial and yeast species can be differentiated using their <span class="hlt">intrinsic</span> fluorescence both in UV and in the visible region. The comparative spectroscopic study of selected strains of Saccharomyces yeast showed clear differences between strains. Spectrally-resolved laser scanning microscopy was carried out to link the results obtained using ensembles of cells with spectral properties of individual cells. Strongly fluorescent subpopulation were observed for all yeast strains with excitation at 405 nm. The fluorescence spectra showed variations <span class="hlt">correlated</span> with cell brightness. The presented results demonstrate that using autofluorescence, it is possible to differentiate between yeast and lactic acid bacteria and between different yeast species.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2005JMAA..305..367L','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2005JMAA..305..367L"><span id="translatedtitle">Multiple solutions for resonant semilinear <span class="hlt">elliptic</span> problems in</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>López Garza, Gabriel; Rumbos, Adolfo J.</p> <p>2005-05-01</p> <p>We prove the existence of multiple nontrivial solutions for the semilinear <span class="hlt">elliptic</span> problem -[Delta]u=h([lambda]u+g(u)) in , , where h[set membership, variant]L1[intersection]L[alpha] for [alpha]>N/2, N[greater-or-equal, slanted]3, g is a function that has at most linear growth at infinity, g(0)=0, and [lambda] is an eigenvalue of the corresponding linear problem -[Delta]u=[lambda]hu in , . Existence of multiple solutions, for certain values of g'(0), is obtained by imposing a generalized Landesman-Lazer type condition. We use the saddle point theorem of Ambrosetti and Rabinowitz and the mountain pass theorem, as well as a Morse-index result of Ambrosetti [A. Ambrosetti, Differential Equations with Multiple Solutions and Nonlinear Functional Analysis, Equadiff 82, Lecture Notes in Math., vol. 1017, Springer-Verlag, Berlin, 1983] and a Leray-Schauder index theorem for mountain pass type critical points due to Hofer [H. Hofer, A note on the Topological Degree at a critical Point of Mountain Pass Type, Proc. Amer. Math. Soc. 90 (1984) 309-315]. The results of this paper are based upon multiplicity results for resonant problems on bounded domains in [E. Landesman, S. Robinson, A. Rumbos, Multiple solutions of semilinear <span class="hlt">elliptic</span> problems at resonance, Nonlinear Anal. 24 (1995) 1049-1059] and [S. Robinson, Multiple solutions for semilinear <span class="hlt">elliptic</span> boundary value problems at resonance, Electron. J. Differential Equations 1995 (1995) 1-14], and complement a previous existence result by the authors in [G. López Garza, A. Rumbos, Resonance and strong resonance for semilinear <span class="hlt">elliptic</span> equations in , Electron. J. Differential Equations 2003 (2003) 1-22] for resonant problems in in which g was assumed to be bounded.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/20645916','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/20645916"><span id="translatedtitle">Mott scattering in an <span class="hlt">elliptically</span> polarized laser field</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Attaourti, Y.; Manaut, B.; Taj, S.</p> <p>2004-08-01</p> <p>We study Mott scattering in the presence of a strong <span class="hlt">elliptically</span> polarized field. Using the first Born approximation and the Dirac-Volkov states for the electron, we obtain an analytic formula for the unpolarized differential cross section. This generalizes the results found for the linearly polarized field by Li et al. [ 67, 063409 (2003)] and for the circularly polarized field by Attaourti and Manaut [ 68, 067401 (2003)].</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19920015169','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19920015169"><span id="translatedtitle">Towards a theory of automated <span class="hlt">elliptic</span> mesh generation</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Cordova, J. Q.</p> <p>1992-01-01</p> <p>The theory of <span class="hlt">elliptic</span> mesh generation is reviewed and the fundamental problem of constructing computational space is discussed. It is argued that the construction of computational space is an NP-Complete problem and therefore requires a nonstandard approach for its solution. This leads to the development of graph-theoretic, combinatorial optimization and integer programming algorithms. Methods for the construction of two dimensional computational space are presented.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://www.dtic.mil/docs/citations/ADA395092','DTIC-ST'); return false;" href="http://www.dtic.mil/docs/citations/ADA395092"><span id="translatedtitle"><span class="hlt">Elliptic</span> Curve Cryptography on Smart Cards Without Coprocessors</span></a></p> <p><a target="_blank" href="https://publicaccess.dtic.mil/psm/api/service/search/search">DTIC Science & Technology</a></p> <p></p> <p>2000-09-20</p> <p><span class="hlt">ELLIPTIC</span> CURVE CRYPTOGRAPHY ON SMART CARDS WITHOUT COPROCESSORS Adam D. Woodbury Electrical and Computer Engineering Department adw@ece.wpi.edu...christof@ece.wpi.edu Worcester Polytechnic Institute Worcester, MA 01609 USA The Fourth Smart Card Research and Advanced Applications (CARDIS 2000...cost microprocessors with reasonable performance. We focus in this paper on the Intel 8051 family of microcontrollers popular in smart cards and other</p> </li> </ol> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_16");'>16</a></li> <li><a href="#" onclick='return showDiv("page_17");'>17</a></li> <li class="active"><span>18</span></li> <li><a href="#" onclick='return showDiv("page_19");'>19</a></li> <li><a href="#" onclick='return showDiv("page_20");'>20</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div><!-- col-sm-12 --> </div><!-- row --> </div><!-- page_18 --> <div id="page_19" class="hiddenDiv"> <div class="row"> <div class="col-sm-12"> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_17");'>17</a></li> <li><a href="#" onclick='return showDiv("page_18");'>18</a></li> <li class="active"><span>19</span></li> <li><a href="#" onclick='return showDiv("page_20");'>20</a></li> <li><a href="#" onclick='return showDiv("page_21");'>21</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div> </div> <div class="row"> <div class="col-sm-12"> <ol class="result-class" start="361"> <li> <p><a target="_blank" onclick="trackOutboundLink('http://www.osti.gov/scitech/servlets/purl/6548702','SCIGOV-STC'); return false;" href="http://www.osti.gov/scitech/servlets/purl/6548702"><span id="translatedtitle">Instability of a supersonic shock free <span class="hlt">elliptic</span> jet</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Baty, R.S. ); Seiner, J.M.; Ponton, M.K. . Langley Research Center)</p> <p>1990-01-01</p> <p>This paper presents a comparison of the measured and the computed spatial stability properties of an aspect ratio 2 supersonic shock free <span class="hlt">elliptic</span> jet. The shock free nature of the <span class="hlt">elliptic</span> jet provides an ideal test of validity of modeling the large scale coherent structures in the initial mixing region of noncircular supersonic jets with linear hydrodynamic stability theory. Both aerodynamic and acoustic data were measured. The data are used to compute the mean velocity profiles and to provide a description of the spatial composition of pressure waves in the <span class="hlt">elliptic</span> jet. A hybrid numerical scheme is applied to solve the Rayleigh problem governing the inviscid linear spatial stability of the jet. The measured mean velocity profiles are used to provide a qualitative model for the cross sectional geometry and the smooth velocity profiles used in the stability analysis. Computational results are presented for several modes of instability at two jet cross sections. The acoustic measurements show that a varicose instability is the jet's perferred mode of motion. The stability analysis predicts that the Strouhal number varies linearly as a function of axial distance in the jet's initial mixing region, which is in good qualitative agreement with previous measurements. 18 refs., 18 figs., 1 tab.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19950022339','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19950022339"><span id="translatedtitle"><span class="hlt">Elliptic</span> surface grid generation on minimal and parmetrized surfaces</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Spekreijse, S. P.; Nijhuis, G. H.; Boerstoel, J. W.</p> <p>1995-01-01</p> <p>An <span class="hlt">elliptic</span> grid generation method is presented which generates excellent boundary conforming grids in domains in 2D physical space. The method is based on the composition of an algebraic and <span class="hlt">elliptic</span> transformation. The composite mapping obeys the familiar Poisson grid generation system with control functions specified by the algebraic transformation. New expressions are given for the control functions. Grid orthogonality at the boundary is achieved by modification of the algebraic transformation. It is shown that grid generation on a minimal surface in 3D physical space is in fact equivalent to grid generation in a domain in 2D physical space. A second <span class="hlt">elliptic</span> grid generation method is presented which generates excellent boundary conforming grids on smooth surfaces. It is assumed that the surfaces are parametrized and that the grid only depends on the shape of the surface and is independent of the parametrization. Concerning surface modeling, it is shown that bicubic Hermite interpolation is an excellent method to generate a smooth surface which is passing through a given discrete set of control points. In contrast to bicubic spline interpolation, there is extra freedom to model the tangent and twist vectors such that spurious oscillations are prevented.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017FlDyR..49b5510A','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017FlDyR..49b5510A"><span id="translatedtitle"><span class="hlt">Elliptic</span> nozzle aspect ratio effect on controlled jet propagation</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Aravindh Kumar, S. M.; Rathakrishnan, Ethirajan</p> <p>2017-04-01</p> <p>The present study deals with the control of a Mach 2 <span class="hlt">elliptic</span> jet from a convergent–divergent <span class="hlt">elliptic</span> nozzle of aspect ratio 4 using tabs at the nozzle exit. The experiments were carried out for rectangular and triangular tabs of the same blockage, placed along the major and minor axes of the nozzle exit, at different levels of nozzle expansion. The triangular tabs along the minor axis promoted superior mixing compared to the other controlled jets and caused substantial core length reduction at all the nozzle pressure ratios studied. The rectangular tabs along the minor axis caused core length reduction at all pressure ratios, but the values were minimal compared to that of triangular tabs along the minor axis. For all the test conditions, the mixing promotion caused by tabs along the major axis was inferior to that of tabs along the minor axis. The waves present in the core of controlled jets were visualized using a shadowgraph. Comparison of the present results with the results of a controlled Mach 2 <span class="hlt">elliptic</span> jet of aspect ratio 2 (Aravindh Kumar and Sathakrishnan 2016 J. Propulsion Power 32 121–33, Aravindh Kumar and Rathakrishnan 2016 J. Aerospace Eng. at press (doi:10.1177/0954410016652921)) show that for all levels of expansion, the mixing effectiveness of triangular tabs along the minor axis of an aspect ratio 4 nozzle is better than rectangular or triangular tabs along the minor axis of an aspect ratio 2 nozzle.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/28213868','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/28213868"><span id="translatedtitle"><span class="hlt">Elliptical</span> Fourier analysis: fundamentals, applications, and value for forensic anthropology.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Caple, Jodi; Byrd, John; Stephan, Carl N</p> <p>2017-02-17</p> <p>The numerical description of skeletal morphology enables forensic anthropologists to conduct objective, reproducible, and structured tests, with the added capability of verifying morphoscopic-based analyses. One technique that permits comprehensive quantification of outline shape is <span class="hlt">elliptical</span> Fourier analysis. This curve fitting technique allows a form's outline to be approximated via the sum of multiple sine and cosine waves, permitting the profile perimeter of an object to be described in a dense (continuous) manner at a user-defined level of precision. A large amount of shape information (the entire perimeter) can thereby be collected in contrast to other methods relying on sparsely located landmarks where information falling in between the landmarks fails to be acquired. First published in 1982, <span class="hlt">elliptical</span> Fourier analysis employment in forensic anthropology from 2000 onwards reflects a slow uptake despite large computing power that makes its calculations easy to conduct. Without hurdles arising from calculation speed or quantity, the slow uptake may partly reside with the underlying mathematics that on first glance is extensive and potentially intimidating. In this paper, we aim to bridge this gap by pictorially illustrating how <span class="hlt">elliptical</span> Fourier harmonics work in a simple step-by-step visual fashion to facilitate universal understanding and as geared towards increased use in forensic anthropology. We additionally provide a short review of the method's utility for osteology, a summary of past uses in forensic anthropology, and software options for calculations that largely save the user the trouble of coding customized routines.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/22080385','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/22080385"><span id="translatedtitle">Casimir force between a microfabricated <span class="hlt">elliptic</span> cylinder and a plate</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Decca, R. S.; Fischbach, E.; Klimchitskaya, G. L.; Krause, D. E.; Lopez, D.; Mostepanenko, V. M.</p> <p>2011-10-15</p> <p>We investigate the Casimir force between a microfabricated <span class="hlt">elliptic</span> cylinder (cylindrical lens) and a plate made of real materials. After a brief discussion of the fabrication procedure, which typically results in <span class="hlt">elliptic</span> rather than circular cylinders, the Lifshitz-type formulas for the Casimir force and for its gradient are derived. In the specific case of equal semiaxes, the resulting formulas coincide with those derived previously for circular cylinders. The nanofabrication procedure may also result in asymmetric cylindrical lenses obtained from parts of two different cylinders, or rotated through some angle about the axis of the cylinder. In these cases, the Lifshitz-type formulas for the Casimir force between a lens and a plate and for its gradient are also derived, and the influence of lens asymmetry is determined. Additionally, we obtain an expression for the shift of the natural frequency of a micromachined oscillator with an attached <span class="hlt">elliptic</span> cylindrical lens interacting with a plate via the Casimir force in a nonlinear regime.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/pages/biblio/1203556-shape-measurement-biases-from-underfitting-ellipticity-gradients','SCIGOV-DOEP'); return false;" href="https://www.osti.gov/pages/biblio/1203556-shape-measurement-biases-from-underfitting-ellipticity-gradients"><span id="translatedtitle">Shape measurement biases from underfitting and <span class="hlt">ellipticity</span> gradients</span></a></p> <p><a target="_blank" href="http://www.osti.gov/pages">DOE PAGES</a></p> <p>Bernstein, Gary M.</p> <p>2010-08-21</p> <p>With this study, precision weak gravitational lensing experiments require measurements of galaxy shapes accurate to <1 part in 1000. We investigate measurement biases, noted by Voigt and Bridle (2009) and Melchior et al. (2009), that are common to shape measurement methodologies that rely upon fitting <span class="hlt">elliptical</span>-isophote galaxy models to observed data. The first bias arises when the true galaxy shapes do not match the models being fit. We show that this "underfitting bias" is due, at root, to these methods' attempts to use information at high spatial frequencies that has been destroyed by the convolution with the point-spread function (PSF)more » and/or by sampling. We propose a new shape-measurement technique that is explicitly confined to observable regions of k-space. A second bias arises for galaxies whose <span class="hlt">ellipticity</span> varies with radius. For most shape-measurement methods, such galaxies are subject to "<span class="hlt">ellipticity</span> gradient bias". We show how to reduce such biases by factors of 20–100 within the new shape-measurement method. The resulting shear estimator has multiplicative errors < 1 part in 103 for high-S/N images, even for highly asymmetric galaxies. Without any training or recalibration, the new method obtains Q = 3000 in the GREAT08 Challenge of blind shear reconstruction on low-noise galaxies, several times better than any previous method.« less</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19910004100','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19910004100"><span id="translatedtitle">Instability of a supersonic shock free <span class="hlt">elliptic</span> jet</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Baty, Roy S.; Seiner, John M.; Ponton, Michael K.</p> <p>1990-01-01</p> <p>This paper presents a comparison of the measured and the computed spatial stability properties of an aspect ratio 2 supersonic shock free <span class="hlt">elliptic</span> jet. The shock free nature of the <span class="hlt">elliptic</span> jet provides an ideal test of validity of modeling the large scale coherent structures in the initial mixing region of noncircular supersonic jets with linear hydrodynamic stability theory. Both aerodynamic and acoustic data were measured. The data are used to compute the mean velocity profiles and to provide a description of the spatial composition of pressure waves in the <span class="hlt">elliptic</span> jet. A hybrid numerical scheme is applied to solve the Rayleigh problem governing the inviscid linear spatial stability of the jet. The measured mean velocity profiles are used to provide a qualitative model for the cross sectional geometry and the smooth velocity profiles used in the stability analysis. Computational results are presented for several modes of instability at two jet cross sections. The acoustic measurements show that a varicose instability is the jet's perferred mode of motion. The stability analysis predicts that the Strouhal number varies linearly as a function of axial distance in the jet's initial mixing region, which is in good qualitative agreement with previous measurements.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19910015568','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19910015568"><span id="translatedtitle">Anisotropic <span class="hlt">elliptic</span> optical fibers. Ph.D. Thesis</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Kang, Soon Ahm</p> <p>1991-01-01</p> <p>The exact characteristic equation for an anisotropic <span class="hlt">elliptic</span> optical fiber is obtained for odd and even hybrid modes in terms of infinite determinants utilizing Mathieu and modified Mathieu functions. A simplified characteristic equation is obtained by applying the weakly guiding approximation such that the difference in the refractive indices of the core and the cladding is small. The simplified characteristic equation is used to compute the normalized guide wavelength for an <span class="hlt">elliptical</span> fiber. When the anisotropic parameter is equal to unity, the results are compared with the previous research and they are in close agreement. For a fixed value normalized cross-section area or major axis, the normalized guide wavelength lambda/lambda(sub 0) for an anisotropic <span class="hlt">elliptic</span> fiber is small for the larger value of anisotropy. This condition indicates that more energy is carried inside of the fiber. However, the geometry and anisotropy of the fiber have a smaller effect when the normalized cross-section area is very small or very large.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19830005187','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19830005187"><span id="translatedtitle">Theoretical results for fully flooded, <span class="hlt">elliptical</span> hydrodynamic contacts</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Hamrock, B. J.; Dowson, D.</p> <p>1982-01-01</p> <p>The influence of the <span class="hlt">ellipticity</span> parameter and the dimensionless speed, load, and materials parameters on minimum film thickness was investigated. The <span class="hlt">ellipticity</span> parameter was varied from 1 (a ball-on-plate configuration) to 8 (a configuration approaching a line contact). The dimensionless speed parameter was varied over a range of nearly two orders of magnitude. Conditions corresponding to the use of solid materials of bronze, steel, and silicon nitride and lubricants of praffinic and naphthemic mineral oils were considered in obtaining the exponent in the dimensionless materials parameter. Thirty-four different cases were used in obtaining the minimum film thickness formula H min = 3.63U to the 0.68 power G to the 0.49 power W to the -0.073 power 1-e to the 0.68K power). A simplified expression for the <span class="hlt">ellipticity</span> parameter was found where k = 1.03 (r(y)/r(x)) to the 0.64 power. Contour plots were also shown which indicate in detail the pressure spike and two side lobes in which the minimum film thickness occurs. These theoretical solutions of film thickness have all the essential features of the previously reported experimental observations based upon optical interferometry.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://www.osti.gov/scitech/servlets/purl/1203556','SCIGOV-STC'); return false;" href="http://www.osti.gov/scitech/servlets/purl/1203556"><span id="translatedtitle">Shape measurement biases from underfitting and <span class="hlt">ellipticity</span> gradients</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Bernstein, Gary M.</p> <p>2010-08-21</p> <p>With this study, precision weak gravitational lensing experiments require measurements of galaxy shapes accurate to <1 part in 1000. We investigate measurement biases, noted by Voigt and Bridle (2009) and Melchior et al. (2009), that are common to shape measurement methodologies that rely upon fitting <span class="hlt">elliptical</span>-isophote galaxy models to observed data. The first bias arises when the true galaxy shapes do not match the models being fit. We show that this "underfitting bias" is due, at root, to these methods' attempts to use information at high spatial frequencies that has been destroyed by the convolution with the point-spread function (PSF) and/or by sampling. We propose a new shape-measurement technique that is explicitly confined to observable regions of k-space. A second bias arises for galaxies whose <span class="hlt">ellipticity</span> varies with radius. For most shape-measurement methods, such galaxies are subject to "<span class="hlt">ellipticity</span> gradient bias". We show how to reduce such biases by factors of 20–100 within the new shape-measurement method. The resulting shear estimator has multiplicative errors < 1 part in 10<sup>3</sup> for high-S/N images, even for highly asymmetric galaxies. Without any training or recalibration, the new method obtains Q = 3000 in the GREAT08 Challenge of blind shear reconstruction on low-noise galaxies, several times better than any previous method.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/16193046','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/16193046"><span id="translatedtitle">Lost and found dark matter in <span class="hlt">elliptical</span> galaxies.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Dekel, A; Stoehr, F; Mamon, G A; Cox, T J; Novak, G S; Primack, J R</p> <p>2005-09-29</p> <p>There is strong evidence that the mass of the Universe is dominated by dark matter, which exerts gravitational attraction but whose exact nature is unknown. In particular, all galaxies are believed to be embedded in massive haloes of dark matter. This view has recently been challenged by the observation of surprisingly low random stellar velocities in the outskirts of ordinary <span class="hlt">elliptical</span> galaxies, which has been interpreted as indicating a lack of dark matter. Here we show that the low velocities are in fact compatible with galaxy formation in dark-matter haloes. Using numerical simulations of disk-galaxy mergers, we find that the stellar orbits in the outer regions of the resulting <span class="hlt">ellipticals</span> are very elongated. These stars were torn by tidal forces from their original galaxies during the first close passage and put on outgoing trajectories. The elongated orbits, combined with the steeply falling density profile of the observed tracers, explain the observed low velocities even in the presence of large amounts of dark matter. Projection effects when viewing a triaxial <span class="hlt">elliptical</span> can lead to even lower observed velocities along certain lines of sight.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2006APS..DPPBP1025P','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2006APS..DPPBP1025P"><span id="translatedtitle"><span class="hlt">Ellipticity</span> and triangularity effects in tokamak Alfven spectrum</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Puerta, Julio; Martin, Pablo; Castro, Enrique; Valdeblanquez, Eder</p> <p>2006-10-01</p> <p>Plasma configurations with <span class="hlt">ellipticity</span> and triangularity are usual in tokamak experiments. These plasmas can be studied using a new system of coordinates of recent publications. Here this method has been applied to study Alfven spectrum in axisymmetric tokamaks with different values of <span class="hlt">ellipticity</span> and triangularity [1-3]. Previous authors have developed numerical methods to obtain the Alfven spectrum using the Shafranov-Solove'v equilibrium flux function where the parameter <span class="hlt">ellipticity</span> is also included [3]. Here more general configurations are treated and compared with the results of these authors, as well as those derived for the geometric optics or WKBJ approximation. The Alfven wave dispersion relation is obtained by the linearization of the MHD equations around a stationary equilibrium and the results are obtained by numerical calculations. [1] P. Martin, M. G. Haines and E. Castro, Phys. Plasma 12, 082506 (2005) [2] L. L. Lao, S. P. Hishman and R. M. Wieland, Phys. Fluids 24, 1431 (1981); H. Weitzner's Appendix. [3] G. O. Ludwig, Plasma Phys. Controlled Fusion 37, 633 (1995) [4] S. Novo, M. N'uñez and J. Rojo, Phys. Fluids B 3, 2967 (1991)</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/22308991','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/22308991"><span id="translatedtitle">An electronic criterion for assessing <span class="hlt">intrinsic</span> brittleness of metallic glasses</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Wang, X. F.; Jones, T. E.; Wu, Y.; Lu, Z. P.; Halas, S.; Durakiewicz, T.; Eberhart, M. E.</p> <p>2014-07-14</p> <p>Bulk metallic glasses (BMGs) are characterized by a number of remarkable physical and mechanical properties. Unfortunately, these same materials are often <span class="hlt">intrinsically</span> brittle, which limits their utility. Consequently, considerable effort has been expended searching for <span class="hlt">correlations</span> between the phenomenologically complex mechanical properties of metallic glasses and more basic properties, such <span class="hlt">correlations</span> might provide insight into the structure and bonding controlling the deformation properties of BMGs. While conducting such a search, we uncovered a weak <span class="hlt">correlation</span> between a BMG’s work function and its susceptibility to brittle behavior. We argue that the basis for this <span class="hlt">correlation</span> is a consequence of a component of the work function – the surface dipole – and a fundamental bond property related to the shape of the charge density at a bond critical point. Together these observations suggest that simple first principle calculations might be useful in the search for tougher BMGs.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/25028023','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/25028023"><span id="translatedtitle">An electronic criterion for assessing <span class="hlt">intrinsic</span> brittleness of metallic glasses.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Wang, X F; Jones, T E; Wu, Y; Lu, Z P; Halas, S; Durakiewicz, T; Eberhart, M E</p> <p>2014-07-14</p> <p>Bulk metallic glasses (BMGs) are characterized by a number of remarkable physical and mechanical properties. Unfortunately, these same materials are often <span class="hlt">intrinsically</span> brittle, which limits their utility. Consequently, considerable effort has been expended searching for <span class="hlt">correlations</span> between the phenomenologically complex mechanical properties of metallic glasses and more basic properties, such <span class="hlt">correlations</span> might provide insight into the structure and bonding controlling the deformation properties of BMGs. While conducting such a search, we uncovered a weak <span class="hlt">correlation</span> between a BMG's work function and its susceptibility to brittle behavior. We argue that the basis for this <span class="hlt">correlation</span> is a consequence of a component of the work function - the surface dipole - and a fundamental bond property related to the shape of the charge density at a bond critical point. Together these observations suggest that simple first principle calculations might be useful in the search for tougher BMGs.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://www.osti.gov/scitech/servlets/purl/392725','SCIGOV-STC'); return false;" href="http://www.osti.gov/scitech/servlets/purl/392725"><span id="translatedtitle"><span class="hlt">Intrinsic</span> Tamper Indicating Device (TID) Program</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Haag, W.E.</p> <p>1996-09-01</p> <p>The Los Alamos National Laboratory (LANL) <span class="hlt">Intrinsic</span> Tamper Indicating Device (TID) Program has recently been developed in conjunction with the regular LANL TID Program to assist groups who perform measurements using sealed sources or store difficult-to-measure items. The program was then expanded to include other types of sealed sources and items processed for long-term storage in the Nuclear Material Packaging and Repackaging Program. The <span class="hlt">Intrinsic</span> TID Program encompasses both Special Nuclear Material (SNM) and Nuclear Material (NM) items that have <span class="hlt">intrinsic</span> characteristics that would immediately indicate tampering upon visual inspection. Items determined to be <span class="hlt">intrinsically</span> sealed do not need to be sealed with authorized tamper indicating devices. Under the program, an identified <span class="hlt">intrinsic</span> item receives the same safeguards credits as other tamper-sealed items already in the TID Program. The major benefits of the <span class="hlt">Intrinsic</span> TID Program include reducing verification measurements on <span class="hlt">intrinsically</span> identified inventory items and reducing exposure to operators working in highly irradiated environments. <span class="hlt">Intrinsic</span> TIDs should be combined with other safeguards requirements, and items should have defensible measurements as well as visual inspections. Several groups at LANL are already implementing the program and providing feedback so that we can tailor it to better meet the customers` needs.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://www.osti.gov/scitech/servlets/purl/565414','SCIGOV-STC'); return false;" href="http://www.osti.gov/scitech/servlets/purl/565414"><span id="translatedtitle"><span class="hlt">Intrinsic</span> bioremediation of landfills interim report</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Brigmon, R.L.; Fliermans, C.B.</p> <p>1997-07-14</p> <p><span class="hlt">Intrinsic</span> bioremediation is a risk management option that relies on natural biological and physical processes to contain the spread of contamination from a source. Evidence is presented in this report that <span class="hlt">intrinsic</span> bioremediation is occurring at the Sanitary Landfill is fundamental to support incorportion into a Corrective Action Plan (CAP).</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4107036','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4107036"><span id="translatedtitle">Development of <span class="hlt">Intrinsically</span> Photoluminescent and Photostable Polylactones</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Xie, Zhiwei; Zhang, Yi; Liu, Li; Weng, Hong; Mason, Ralph P.; Tang, Liping; Nguyen, Kytai T.; Hsieh, Jer-Tsong</p> <p>2014-01-01</p> <p>A method of introducing <span class="hlt">intrinsically</span> photoluminescent properties to biodegradable polymer was introduced, exemplified by the synthesis of <span class="hlt">intrinsically</span> photoluminescent polylactones that enable non-invasively monitoring and tracking material degradation in vivo in real-time and the formation of theranostic nanoparticles for cancer imaging and drug delivery. PMID:24668888</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017PhRvB..95a4202W','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017PhRvB..95a4202W"><span id="translatedtitle"><span class="hlt">Intrinsic</span> decoherence in isolated quantum systems</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Wu, Yang-Le; Deng, Dong-Ling; Li, Xiaopeng; Das Sarma, S.</p> <p>2017-01-01</p> <p>We study the <span class="hlt">intrinsic</span>, disorder-induced decoherence of an isolated quantum system under its own dynamics. Specifically, we investigate the characteristic time scale (i.e., the decoherence time) associated with an interacting many-body system losing the memory of its initial state. To characterize the erasure of the initial state memory, we define a time scale, the <span class="hlt">intrinsic</span> decoherence time, by thresholding the gradual decay of the disorder-averaged return probability. We demonstrate the system-size independence of the <span class="hlt">intrinsic</span> decoherence time in different models, and we study its dependence on the disorder strength. We find that the <span class="hlt">intrinsic</span> decoherence time increases monotonically as the disorder strength increases in accordance with the relaxation of locally measurable quantities. We investigate several interacting spin (e.g., Ising and Heisenberg) and fermion (e.g., Anderson and Aubry-André) models to obtain the <span class="hlt">intrinsic</span> decoherence time as a function of disorder and interaction strength.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4268557','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4268557"><span id="translatedtitle"><span class="hlt">Intrinsic</span> Coupling Modes in Source-Reconstructed Electroencephalography</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Breakspear, Michael; Britz, Juliane; Boonstra, Tjeerd W.</p> <p>2014-01-01</p> <p>Abstract <span class="hlt">Intrinsic</span> coupling of neuronal assemblies constitutes a key feature of ongoing brain activity, yielding the rich spatiotemporal patterns observed in neuroimaging data and putatively supporting cognitive processes. <span class="hlt">Intrinsic</span> coupling has been investigated in electrophysiological recordings using two types of functional connectivity measures: amplitude and phase coupling. These two coupling modes differ in their likely causes and functions, and have been proposed to provide complementary insights into <span class="hlt">intrinsic</span> neuronal interactions. Here, we investigate the relationship between amplitude and phase coupling in source-reconstructed electroencephalography (EEG). Volume conduction is a key obstacle for connectivity analysis in EEG—we therefore also test the envelope <span class="hlt">correlation</span> of orthogonalized signals and the phase lag index. Functional connectivity between six seed source regions (bilateral visual, sensorimotor, and auditory cortices) and all other cortical voxels was computed. For all four measures, coupling between homologous sensory areas in both hemispheres was significantly higher than with other voxels at the same physical distance. The frequency of significant coupling differed between sensory areas: 10 Hz for visual, 30 Hz for auditory, and 40 Hz for sensorimotor cortices. By contrasting envelope <span class="hlt">correlations</span> and phase locking values, we observed two distinct clusters of voxels showing a different relationship between amplitude and phase coupling. Large clusters contiguous to the seed regions showed an identity (1:1) relationship between amplitude and phase coupling, whereas a cluster located around the contralateral homologous regions showed higher phase than amplitude coupling. These results show a relationship between <span class="hlt">intrinsic</span> coupling modes that is distinct from the effect of volume conduction. PMID:25230358</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/21231580','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/21231580"><span id="translatedtitle"><span class="hlt">Elliptic</span> flow of charged particles in Pb-Pb collisions at sqrt[S(NN)] = 2.76 TeV.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Aamodt, K; Abelev, B; Quintana, A Abrahantes; Adamová, D; Adare, A M; Aggarwal, M M; Rinella, G Aglieri; Agocs, A G; Salazar, S Aguilar; Ahammed, Z; Masoodi, A Ahmad; Ahmad, N; Ahn, S U; Akindinov, A; Aleksandrov, D; Alessandro, B; Molina, R Alfaro; Alici, A; Alkin, A; Aviña, E Almaráz; Alt, T; Altini, V; Altinpinar, S; Altsybeev, I; Andrei, C; Andronic, A; Anguelov, V; Anson, C; Antičić, T; Antinori, F; Antonioli, P; Aphecetche, L; Appelshäuser, H; Arbor, N; Arcelli, S; Arend, A; Armesto, N; Arnaldi, R; Aronsson, T; Arsene, I C; Asryan, A; Augustinus, A; Averbeck, R; Awes, T C; Aystö, J; Azmi, M D; Bach, M; Badalà, A; Baek, Y W; Bagnasco, S; Bailhache, R; Bala, R; Ferroli, R Baldini; Baldisseri, A; Baldit, A; Pedrosa, F Baltasar Dos Santos; Bán, J; Barbera, R; Barile, F; Barnaföldi, G G; Barnby, L S; Barret, V; Bartke, J; Basile, M; Bastid, N; Bathen, B; Batigne, G; Batyunya, B; Baumann, C; Bearden, I G; Beck, H; Belikov, I; Bellini, F; Bellwied, R; Belmont-Moreno, E; Beole, S; Berceanu, I; Bercuci, A; Berdermann, E; Berdnikov, Y; Bergmann, C; Betev, L; Bhasin, A; Bhati, A K; Bianchi, L; Bianchi, N; Bianchin, C; Bielčík, J; Bielčíková, J; Bilandzic, A; Biolcati, E; Blanc, A; Blanco, F; Blanco, F; Blau, D; Blume, C; Boccioli, M; Bock, N; Bogdanov, A; Bøggild, H; Bogolyubsky, M; Boldizsár, L; Bombara, M; Bombonati, C; Book, J; Borel, H; Borissov, A; Bortolin, C; Bose, S; Bossú, F; Botje, M; Böttger, S; Boyer, B; Braun-Munzinger, P; Bravina, L; Bregant, M; Breitner, T; Broz, M; Brun, R; Bruna, E; Bruno, G E; Budnikov, D; Buesching, H; Bugaiev, K; Busch, O; Buthelezi, Z; Caffarri, D; Cai, X; Caines, H; Villar, E Calvo; Camerini, P; Canoa Roman, V; Romeo, G Cara; Carena, F; Carena, W; Carminati, F; Díaz, A Casanova; Caselle, M; Castellanos, J Castillo; Catanescu, V; Cavicchioli, C; Cepila, J; Cerello, P; Chang, B; Chapeland, S; Charvet, J L; Chattopadhyay, S; Chattopadhyay, S; Cherney, M; Cheshkov, C; Cheynis, B; Chiavassa, E; Barroso, V Chibante; Chinellato, D D; Chochula, P; Chojnacki, M; Christakoglou, P; Christensen, C H; Christiansen, P; Chujo, T; Cicalo, C; Cifarelli, L; Cindolo, F; Cleymans, J; Coccetti, F; Coffin, J-P; Coli, S; Balbastre, G Conesa; del Valle, Z Conesa; Constantin, P; Contin, G; Contreras, J G; Cormier, T M; Morales, Y Corrales; Maldonado, I Cortés; Cortese, P; Cosentino, M R; Costa, F; Cotallo, M E; Crescio, E; Crochet, P; Cuautle, E; Cunqueiro, L; Erasmo, G D; Dainese, A; Dalsgaard, H H; Danu, A; Das, D; Das, I; Das, K; Dash, A; Dash, S; De, S; Moregula, A De Azevedo; de Barros, G O V; De Caro, A; 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Fuchs, U; Furano, F; Furget, C; Girard, M Fusco; Gaardhøje, J J; Gadrat, S; Gagliardi, M; Gago, A; Gallio, M; Gangadharan, D R; Ganoti, P; Ganti, M S; Garabatos, C; Garcia-Solis, E; Garishvili, I; Gemme, R; Gerhard, J; Germain, M; Geuna, C; Gheata, A; Gheata, M; Ghidini, B; Ghosh, P; Gianotti, P; Girard, M R; Giraudo, G; Giubellino, P; Gladysz-Dziadus, E; Glässel, P; Gomez, R; Ferreiro, E G; Santos, H González; González-Trueba, L H; González-Zamora, P; Gorbunov, S; Gotovac, S; Grabski, V; Grajcarek, R; Grelli, A; Grigoras, A; Grigoras, C; Grigoriev, V; Grigoryan, A; Grigoryan, S; Grinyov, B; Grion, N; Gros, P; Grosse-Oetringhaus, J F; Grossiord, J-Y; Grosso, R; Guber, F; Guernane, R; Gutierrez, C Guerra; Guerzoni, B; Gulbrandsen, K; Gunji, T; Gupta, A; Gupta, R; Gutbrod, H; Haaland, Ø; Hadjidakis, C; Haiduc, M; Hamagaki, H; Hamar, G; Harris, J W; Hartig, M; Hasch, D; Hasegan, D; Hatzifotiadou, D; Hayrapetyan, A; Heide, M; Heinz, M; Helstrup, H; Herghelegiu, A; Hernández, C; Corral, G Herrera; Herrmann, N; Hetland, K F; Hicks, B; Hille, P T; Hippolyte, B; Horaguchi, T; Hori, Y; Hristov, P; Hřivnáčová, I; Huang, M; Huber, S; Humanic, T J; Hwang, D S; Ichou, R; Ilkaev, R; Ilkiv, I; Inaba, M; Incani, E; Innocenti, G M; Innocenti, P G; Ippolitov, M; Irfan, M; Ivan, C; Ivanov, A; Ivanov, M; Ivanov, V; Jachołkowski, A; Jacobs, P M; Jancurová, L; Jangal, S; Janik, R; Jena, S; Jirden, L; Jones, G T; Jones, P G; Jovanović, P; Jung, H; Jung, W; Jusko, A; Kalcher, S; Kaliňák, P; Kalisky, M; Kalliokoski, T; Kalweit, A; Kamermans, R; Kanaki, K; Kang, E; Kang, J H; Kaplin, V; Karavichev, O; Karavicheva, T; Karpechev, E; Kazantsev, A; Kebschull, U; Keidel, R; Khan, M M; Khan, S A; Khanzadeev, A; Kharlov, Y; Kileng, B; Kim, D J; Kim, D S; Kim, D W; Kim, H N; Kim, J H; Kim, J S; Kim, M; Kim, M; Kim, S; Kim, S H; Kirsch, S; Kisel, I; Kiselev, S; Kisiel, A; Klay, J L; Klein, J; Klein-Bösing, C; Kliemant, M; Klovning, A; Kluge, A; Knichel, M L; Koch, K; Köhler, M K; Kolevatov, R; Kolojvari, A; Kondratiev, V; Kondratyeva, N; Konevskih, A; Kornaś, E; Don, C Kottachchi Kankanamge; Kour, R; Kowalski, M; Kox, S; Meethaleveedu, G Koyithatta; Kozlov, K; Kral, J; Králik, I; Kramer, F; Kraus, I; Krawutschke, T; Kretz, M; Krivda, M; Krizek, F; Krumbhorn, D; Krus, M; Kryshen, E; Krzewicki, M; Kucheriaev, Y; Kuhn, C; Kuijer, P G; Kurashvili, P; Kurepin, A; Kurepin, A B; Kuryakin, A; Kushpil, S; Kushpil, V; Kweon, M J; Kwon, Y; La Rocca, P; Ladrón de Guevara, P; Lafage, V; Lara, C; Lardeux, A; Larsen, D T; Lazzeroni, C; Le Bornec, Y; Lea, R; Lee, K S; Lee, S C; Lefèvre, F; Lehnert, J; Leistam, L; Lenhardt, M; Lenti, V; Monzón, I León; Vargas, H León; Lévai, P; Li, X; Lien, J; Lietava, R; Lindal, S; Lindenstruth, V; Lippmann, C; Lisa, M A; Liu, L; Loenne, P I; Loggins, V R; Loginov, V; Lohn, S; Loizides, C; Loo, K K; Lopez, X; Noriega, M López; Torres, E López; Løvhøiden, G; Lu, X-G; Luettig, P; Lunardon, M; Luparello, G; Luquin, L; Luzzi, C; Ma, K; Ma, R; Madagodahettige-Don, D M; Maevskaya, A; Mager, M; Mahapatra, D P; Maire, A; Mal'Kevich, D; Malaev, M; Cervantes, I Maldonado; Malinina, L; Malzacher, P; Mamonov, A; Manceau, L; Mangotra, L; Manko, V; Manso, F; Manzari, V; Mao, Y; Mareš, J; Margagliotti, G V; Margotti, A; Marín, A; Markert, C; Martashvili, I; Martinengo, P; Martínez, M I; Davalos, A Martínez; García, G Martínez; Martynov, Y; Masciocchi, S; Masera, M; Masoni, A; Massacrier, L; Mastromarco, M; Mastroserio, A; Matthews, Z L; Matyja, A; Mayani, D; Mayer, C; Mazza, G; Mazzoni, M A; Meddi, F; Menchaca-Rocha, A; Lorenzo, P Mendez; Menis, I; Pérez, J Mercado; Meres, M; Mereu, P; Miake, Y; Midori, J; Milano, L; Milosevic, J; Mischke, A; Miśkowiec, D; Mitu, C; Mlynarz, J; Mohanty, A K; Mohanty, B; Molnar, L; Zetina, L Montaño; Monteno, M; Montes, E; Morando, M; De Godoy, D A Moreira; Moretto, S; Morsch, A; Muccifora, V; Mudnic, E; Muhuri, S; Müller, H; Munhoz, M G; Munoz, J; Musa, L; Musso, A; Nandi, B K; Nania, R; Nappi, E; Nattrass, C; Navach, F; Navin, S; Nayak, T K; Nazarenko, S; Nazarov, G; Nedosekin, A; Nendaz, F; Newby, J; Nicassio, M; Nielsen, B S; Niida, T; Nikolaev, S; Nikolic, V; Nikulin, S; Nikulin, V; Nilsen, B S; Nilsson, M S; Noferini, F; Nooren, G; Novitzky, N; Nyanin, A; Nyatha, A; Nygaard, C; Nystrand, J; Obayashi, H; Ochirov, A; Oeschler, H; Oh, S K; Oleniacz, J; Oppedisano, C; Velasquez, A Ortiz; Ortona, G; Oskarsson, A; Ostrowski, P; Otterlund, I; Otwinowski, J; Oyama, K; Ozawa, K; Pachmayer, Y; Pachr, M; Padilla, F; Pagano, P; Jayarathna, S P; Paić, G; Painke, F; Pajares, C; Pal, S; Pal, S K; Palaha, A; Palmeri, A; Pappalardo, G S; Park, W J; Patalakha, D I; Paticchio, V; Pavlinov, A; Pawlak, T; Peitzmann, T; Peresunko, D; Lara, C E Pérez; Perini, D; Perrino, D; Peryt, W; Pesci, A; Peskov, V; Pestov, Y; Peters, A J; Petráček, V; Petran, M; Petris, M; Petrov, P; Petrovici, M; Petta, C; Piano, S; Piccotti, A; Pikna, M; Pillot, P; Pinazza, O; Pinsky, L; Pitz, N; Piuz, F; Piyarathna, D B; Platt, R; Płoskoń, M; Pluta, J; Pocheptsov, T; Pochybova, S; Podesta-Lerma, P L M; Poghosyan, M G; Polák, K; Polichtchouk, B; Pop, A; Porteboeuf, S; Pospíšil, V; Potukuchi, B; Prasad, S K; Preghenella, R; Prino, F; Pruneau, C A; Pshenichnov, I; Puddu, G; Pulvirenti, A; Punin, V; Putiš, M; Putschke, J; Quercigh, E; Qvigstad, H; Rachevski, A; Rademakers, A; Rademakers, O; Radomski, S; Räihä, T S; Rak, J; Rakotozafindrabe, A; Ramello, L; Reyes, A Ramírez; Rammler, M; Raniwala, R; Raniwala, S; Räsänen, S S; Read, K F; Real, J; Redlich, K; Renfordt, R; Reolon, A R; Reshetin, A; Rettig, F; Revol, J-P; Reygers, K; Ricaud, H; Riccati, L; Ricci, R A; Richter, M; Riedler, P; Riegler, W; Riggi, F; Cahuantzi, M Rodríguez; Rohr, D; Röhrich, D; Romita, R; Ronchetti, F; Rosinský, P; Rosnet, P; Rossegger, S; Rossi, A; Roukoutakis, F; Rousseau, S; Roy, C; Roy, P; Montero, A J Rubio; Rui, R; Rivetti, A; Rusanov, I; Ryabinkin, E; Rybicki, A; Sadovsky, S; Safařík, K; Sahoo, R; Sahu, P K; Saini, J; Saiz, P; Sakai, S; Sakata, D; Salgado, C A; Samanta, T; Sambyal, S; Samsonov, V; Castro, X Sanchez; Sándor, L; Sandoval, A; Sano, M; Sano, S; Santo, R; Santoro, R; Sarkamo, J; Saturnini, P; Scapparone, E; Scarlassara, F; Scharenberg, R P; Schiaua, C; Schicker, R; Schmidt, C; Schmidt, H R; Schreiner, S; Schuchmann, S; Schukraft, J; Schutz, Y; Schwarz, K; Schweda, K; Scioli, G; Scomparin, E; Scott, P A; Scott, R; Segato, G; Selyuzhenkov, I; Senyukov, S; Seo, J; Serci, S; Serradilla, E; Sevcenco, A; Sgura, I; Shabratova, G; Shahoyan, R; Sharma, N; Sharma, S; Shigaki, K; Shimomura, M; Shtejer, K; Sibiriak, Y; Siciliano, M; Sicking, E; Siemiarczuk, T; Silenzi, A; Silvermyr, D; Simonetti, G; Singaraju, R; Singh, R; Singhal, V; Sinha, B C; Sinha, T; Sitar, B; Sitta, M; Skaali, T B; Skjerdal, K; Smakal, R; Smirnov, N; Snellings, R; Søgaard, C; Soloviev, A; Soltz, R; Son, H; Song, J; Song, M; Soos, C; Soramel, F; Spyropoulou-Stassinaki, M; Srivastava, B K; Stachel, J; Stan, I; Stefanek, G; Stefanini, G; Steinbeck, T; Steinpreis, M; Stenlund, E; Steyn, G; Stocco, D; Stock, R; Stokkevag, C H; Stolpovskiy, M; Strmen, P; Suaide, A A P; Vásquez, M A Subieta; Sugitate, T; Suire, C; Sukhorukov, M; Sumbera, M; Susa, T; Swoboda, D; Symons, T J M; de Toledo, A Szanto; Szarka, I; Szostak, A; Tagridis, C; Takahashi, J; Takaki, J D Tapia; Tauro, A; Tavlet, M; Muñoz, G Tejeda; Telesca, A; Terrevoli, C; Thäder, J; Thomas, D; Thomas, J H; Tieulent, R; Timmins, A R; Tlusty, D; Toia, A; Torii, H; Toscano, L; Tosello, F; Traczyk, T; Truesdale, D; Trzaska, W H; Tsuji, T; Tumkin, A; Turrisi, R; Turvey, A J; Tveter, T S; Ulery, J; Ullaland, K; Uras, A; Urbán, J; Urciuoli, G M; Usai, G L; Vacchi, A; Vajzer, M; Vala, M; Palomo, L Valencia; Vallero, S; van der Kolk, N; van Leeuwen, M; Vande Vyvre, P; Vannucci, L; Vargas, A; Varma, R; Vasileiou, M; Vasiliev, A; Vechernin, V; Veldhoen, M; Venaruzzo, M; Vercellin, E; Vergara, S; Vernekohl, D C; Vernet, R; Verweij, M; Vickovic, L; Viesti, G; Vikhlyantsev, O; Vilakazi, Z; Baillie, O Villalobos; Vinogradov, A; Vinogradov, L; Vinogradov, Y; Virgili, T; Viyogi, Y P; Vodopyanov, A; Voloshin, K; Voloshin, S; Volpe, G; von Haller, B; Vranic, D; Øvrebekk, G; Vrláková, J; Vulpescu, B; Vyushin, A; Wagner, B; Wagner, V; Wan, R; Wang, D; Wang, Y; Wang, Y; Watanabe, K; Wessels, J P; Westerhoff, U; Wiechula, J; Wikne, J; Wilde, M; Wilk, A; Wilk, G; Williams, M C S; Windelband, B; Karampatsos, L Xaplanteris; Yang, H; Yang, S; Yasnopolskiy, S; Yi, J; Yin, Z; Yokoyama, H; Yoo, I-K; Yu, W; Yuan, X; Yushmanov, I; Zabrodin, E; Zach, C; Zampolli, C; Zaporozhets, S; Zarochentsev, A; Závada, P; Zaviyalov, N; Zbroszczyk, H; Zelnicek, P; Zenin, A; Zgura, I; Zhalov, M; Zhang, X; Zhou, D; Zichichi, A; Zinovjev, G; Zoccarato, Y; Zynovyev, M</p> <p>2010-12-17</p> <p>We report the first measurement of charged particle <span class="hlt">elliptic</span> flow in Pb-Pb collisions at sqrt[S(NN)] =2.76 TeV with the ALICE detector at the CERN Large Hadron Collider. The measurement is performed in the central pseudorapidity region (|η|<0.8) and transverse momentum range 0.2<p t<5.0 GeV/c. The <span class="hlt">elliptic</span> flow signal v₂, measured using the 4-particle <span class="hlt">correlation</span> method, averaged over transverse momentum and pseudorapidity is 0.087 ± 0.002(stat) ± 0.003(syst) in the 40%-50% centrality class. The differential <span class="hlt">elliptic</span> flow v₂ p t reaches a maximum of 0.2 near p t =3 GeV/c. Compared to RHIC Au-Au collisions at sqrt[S(NN)] 200 GeV, the <span class="hlt">elliptic</span> flow increases by about 30%. Some hydrodynamic model predictions which include viscous corrections are in agreement with the observed increase.</p> </li> </ol> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_17");'>17</a></li> <li><a href="#" onclick='return showDiv("page_18");'>18</a></li> <li class="active"><span>19</span></li> <li><a href="#" onclick='return showDiv("page_20");'>20</a></li> <li><a href="#" onclick='return showDiv("page_21");'>21</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div><!-- col-sm-12 --> </div><!-- row --> </div><!-- page_19 --> <div id="page_20" class="hiddenDiv"> <div class="row"> <div class="col-sm-12"> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_18");'>18</a></li> <li><a href="#" onclick='return showDiv("page_19");'>19</a></li> <li class="active"><span>20</span></li> <li><a href="#" onclick='return showDiv("page_21");'>21</a></li> <li><a href="#" onclick='return showDiv("page_22");'>22</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div> </div> <div class="row"> <div class="col-sm-12"> <ol class="result-class" start="381"> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=5314918','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=5314918"><span id="translatedtitle">CECAM workshop on <span class="hlt">Intrinsically</span> Disordered Proteins</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Rösner, Heike; Papaleo, Elena; Haxholm, Gitte W; Best, Robert B; Kragelund, Birthe B; Lindorff-Larsen, Kresten</p> <p>2014-01-01</p> <p>With the increasing need to integrate different areas of science in the study of <span class="hlt">intrinsically</span> disordered proteins we arranged a meeting entitled “<span class="hlt">Intrinsically</span> Disordered Proteins: Connecting Computation, Physics and Biology” in Zürich in September 2013. The aim of the meeting was to bring together scientists from a range of disciplines to provide a snapshot of the field, as well as to promote future interdisciplinary studies that link the fundamental physical and chemical properties of <span class="hlt">intrinsically</span> disordered proteins with their biological function. A range of important topics were covered at the meeting including studies linking structural studies of <span class="hlt">intrinsically</span> disordered proteins with their function, the effect of post-translational modifications, studies of folding-upon-binding, as well as presentation of a number of systems in which <span class="hlt">intrinsically</span> disordered proteins play a central role in important biological processes. A recurring theme was how computation, including various forms of molecular simulations, can be integrated with experimental and theoretical studies to help understand the complex properties of <span class="hlt">intrinsically</span> disordered proteins. With this Meeting Report we hope to give a brief overview of the inspiration obtained from presentations, discussions and conversation held at the workshop and point out possible future directions within the field of <span class="hlt">intrinsically</span> disordered proteins.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=5314871','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=5314871"><span id="translatedtitle">CECAM workshop on <span class="hlt">intrinsically</span> disordered proteins</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Rösner, Heike; Papaleo, Elena; Haxholm, Gitte W; Best, Robert B; Kragelund, Birthe B; Lindorff-Larsen, Kresten</p> <p>2014-01-01</p> <p>With the increasing need to integrate different areas of science in the study of <span class="hlt">intrinsically</span> disordered proteins we arranged a meeting entitled “<span class="hlt">Intrinsically</span> Disordered Proteins: Connecting Computation, Physics and Biology” in Zürich in September 2013. The aim of the meeting was to bring together scientists from a range of disciplines to provide a snapshot of the field, as well as to promote future interdisciplinary studies that link the fundamental physical and chemical properties of <span class="hlt">intrinsically</span> disordered proteins with their biological function. A range of important topics were covered at the meeting including studies linking structural studies of <span class="hlt">intrinsically</span> disordered proteins with their function, the effect of post-translational modifications, studies of folding-upon-binding, as well as presentation of a number of systems in which <span class="hlt">intrinsically</span> disordered proteins play a central role in important biological processes. A recurring theme was how computation, including various forms of molecular simulations, can be integrated with experimental and theoretical studies to help understand the complex properties of <span class="hlt">intrinsically</span> disordered proteins. With this Meeting Report we hope to give a brief overview of the inspiration obtained from presentations, discussions and conversations held at the workshop and point out possible future directions within the field of <span class="hlt">intrinsically</span> disordered proteins.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19790005133','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19790005133"><span id="translatedtitle">The development of a three-dimensional partially <span class="hlt">elliptic</span> flow computer program for combustor research</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Pan, Y. S.</p> <p>1978-01-01</p> <p>A three dimensional, partially <span class="hlt">elliptic</span>, computer program was developed. Without requiring three dimensional computer storage locations for all flow variables, the partially <span class="hlt">elliptic</span> program is capable of predicting three dimensional combustor flow fields with large downstream effects. The program requires only slight increase of computer storage over the parabolic flow program from which it was developed. A finite difference formulation for a three dimensional, fully <span class="hlt">elliptic</span>, turbulent, reacting, flow field was derived. Because of the negligible diffusion effects in the main flow direction in a supersonic combustor, the set of finite-difference equations can be reduced to a partially <span class="hlt">elliptic</span> form. Only the pressure field was governed by an <span class="hlt">elliptic</span> equation and requires three dimensional storage; all other dependent variables are governed by parabolic equations. A numerical procedure which combines a marching integration scheme with an iterative scheme for solving the <span class="hlt">elliptic</span> pressure was adopted.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2003JMMM..267..373G','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2003JMMM..267..373G"><span id="translatedtitle">The demagnetizing energies of a uniformly magnetized cylinder with an <span class="hlt">elliptic</span> cross-section</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Goode, D. A.; Rowlands, G.</p> <p>2003-12-01</p> <p>Analytic expressions for the demagnetizing energies are obtained in the form of partial series, for long <span class="hlt">elliptic</span> cylinders and for squat ones where the <span class="hlt">ellipticity</span> of the cross-section is unrestrained. This leaves just a small range where the demagnetizing energies are not well defined. It is found that by replacing the <span class="hlt">elliptic</span> cylinders with rectangular blocks, a good approximation to the demagnetizing energy may be made in this small range.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2008IJTPE.128.1295K','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2008IJTPE.128.1295K"><span id="translatedtitle">Current State and Future Prospect of Applications of <span class="hlt">Elliptic</span> Function to Electric Power Field</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Kinoshita, Haruka; Watanabe, Kazuo</p> <p></p> <p>The paper deals with the current state and future prospect of applications of <span class="hlt">elliptic</span> function to the electric power and energy field. In particular, practical use of conformal mapping technology by <span class="hlt">elliptic</span> function are introduced for electric power cables. Returning to Riemann's basic principle “thinking instead of calculation”, against the main current of numerical calculation, we have a new understanding of <span class="hlt">elliptic</span> function analysis for the usefulness and the beautiful with simplicity and elegance.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/24149160','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/24149160"><span id="translatedtitle">Familiarization Effects of an <span class="hlt">Elliptical</span> All-out Test and the Wingate Test Based on Mechanical Power Indices.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Ozkaya, Ozgur</p> <p>2013-01-01</p> <p>The Wingate all-out test (WAT) is commonly used to estimate anaerobic capabilities of athletes by using an upper or lower body cycle ergometer, however, a new test modality called <span class="hlt">elliptical</span> all-out test (EAT) which measures activated whole-body locomotor tasks has recently been proposed. The purpose of this study was to evaluate the familiarization effects of a 30-s EAT versus WAT. Twenty male trained athletes performed pre-familiarization (Trial- I), post-familiarization (Trial-II) and retest of Trial-II (Trial-III) sessions on both cycle ergometer and <span class="hlt">elliptical</span> trainer. Peak power (PP), average power (AP), power drop (PD) and fatigue index ratio (FI%) were analyzed using student's t-test for paired samples and <span class="hlt">correlated</span> by intra-class <span class="hlt">correlation</span> coefficients (ICC). Moreover, an error detection procedure was administered using data attained from illogical interrelations among 5-s segments of 30-s tests. The main results showed that there were significant familiarization effects in all mechanical power outputs obtained from Trial-I and Trial-II in both EAT (ICC = 0.49-0.55) and WAT (ICC = 0.50-0.57) performances (p ≤ 0.01). Significant segmental disorders were detected in power production during Trial-I of EAT, however, none existed in any of test trails in the WAT (p ≤ 0.001). After familiarization sessions, reliability coefficients between Trial-II and Trial-III showed moderate to strong-level agreements for both EAT (ICC = 0.74-0.91) and the WAT (ICC=0.76-0.93). Our results suggested that prior to the performance tests, combination of a well designed familiarization session with one full all-out test administration is necessary to estimate the least moderately reliable and accurate test indices for both WAT and EAT. Key PointsA well designed familiarization session, and then, one additional all-out test administration, several days prior to main test, is suggested to estimate more accurate and reliable retest <span class="hlt">correlations</span> for both cycling and <span class="hlt">elliptical</span></p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2004AAS...20517004D','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2004AAS...20517004D"><span id="translatedtitle"><span class="hlt">Intrinsic</span> Wavelength Shifts in Stellar Spectra</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Dravins, D.; Lindegren, L.; Ludwig, H.-G.; Madsen, S.</p> <p>2004-12-01</p> <p>Wavelengths of stellar spectral lines do not have the precise values `naively' expected from laboratory wavelengths merely Doppler-shifted by stellar radial motion. Slight displacements may originate as convective shifts (<span class="hlt">correlated</span> velocity and brightness patterns in the photosphere), as gravitational redshifts, or perhaps be induced by wave motions. <span class="hlt">Intrinsic</span> lineshifts thus reveal stellar surface structure, while possible periodic changes (during a stellar activity cycle, say) need to be segregated from variability induced by orbiting exoplanets. Absolute lineshifts can now be studied also in some stars other than the Sun, thanks to astrometric determinations of stellar radial motion. Comparisons between spectroscopic apparent radial velocities and astrometrically determined radial motions reveal greater spectral blueshifts in F-type stars than in the Sun (as theoretically expected from their more vigorous convection), further increasing in A-type stars (possibly due to atmospheric shockwaves). Solar spectral atlases, and high-resolution spectra (from UVES on ESO VLT) of a dozen solar-type stars are being surveyed for `unblended' photospheric lines of most atomic species with accurate laboratory wavelengths available. One aim is to understand the ultimate information content of stellar spectra, and in what detail it will be feasible to verify models of stellar atmospheric hydrodynamics. These may predict line asymmetries (bisectors) and shifts for widely different classes of lines, but there will not result any comparison with observations if such lines do not exist in real spectra. An expected near-future development in stellar physics is spatially resolved spectroscopy across stellar disks, enabled by optical interferometry and adaptive optics on very large telescopes. Stellar surface structure manifests itself in the center-to-limb wavelength changes along a stellar diameter, and their spatially resolved time variability, diagnostics which already now can be</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2001PhRvL..86..402A','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2001PhRvL..86..402A"><span id="translatedtitle"><span class="hlt">Elliptic</span> Flow in Au+Au Collisions at √sNN = 130 GeV</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Ackermann, K. H.; Adams, N.; Adler, C.; Ahammed, Z.; Ahmad, S.; Allgower, C.; Amsbaugh, J.; Anderson, M.; Anderssen, E.; Arnesen, H.; Arnold, L.; Averichev, G. S.; Baldwin, A.; Balewski, J.; Barannikova, O.; Barnby, L. S.; Baudot, J.; Beddo, M.; Bekele, S.; Belaga, V. V.; Bellwied, R.; Bennett, S.; Bercovitz, J.; Berger, J.; Betts, W.; Bichsel, H.; Bieser, F.; Bland, L. C.; Bloomer, M.; Blyth, C. O.; Boehm, J.; Bonner, B. E.; Bonnet, D.; Bossingham, R.; Botlo, M.; Boucham, A.; Bouillo, N.; Bouvier, S.; Bradley, K.; Brady, F. P.; Braithwaite, E. S.; Braithwaite, W.; Brandin, A.; Brown, R. L.; Brugalette, G.; Byrd, C.; Caines, H.; Calderón de La Barca Sánchez, M.; Cardenas, A.; Carr, L.; Carroll, J.; Castillo, J.; Caylor, B.; Cebra, D.; Chatopadhyay, S.; Chen, M. L.; Chen, W.; Chen, Y.; Chernenko, S. P.; Cherney, M.; Chikanian, A.; Choi, B.; Chrin, J.; Christie, W.; Coffin, J. P.; Conin, L.; Consiglio, C.; Cormier, T. M.; Cramer, J. G.; Crawford, H. J.; Danilov, V. I.; Dayton, D.; Demello, M.; Deng, W. S.; Derevschikov, A. A.; Dialinas, M.; Diaz, H.; Deyoung, P. A.; Didenko, L.; Dimassimo, D.; Dioguardi, J.; Dominik, W.; Drancourt, C.; Draper, J. E.; Dunin, V. B.; Dunlop, J. C.; Eckardt, V.; Edwards, W. R.; Efimov, L. G.; Eggert, T.; Emelianov, V.; Engelage, J.; Eppley, G.; Erazmus, B.; Etkin, A.; Fachini, P.; Feliciano, C.; Ferenc, D.; Ferguson, M. I.; Fessler, H.; Finch, E.; Fine, V.; Fisyak, Y.; Flierl, D.; Flores, I.; Foley, K. J.; Fritz, D.; Gagunashvili, N.; Gans, J.; Gazdzicki, M.; Germain, M.; Geurts, F.; Ghazikhanian, V.; Gojak, C.; Grabski, J.; Grachov, O.; Grau, M.; Greiner, D.; Greiner, L.; Grigoriev, V.; Grosnick, D.; Gross, J.; Guilloux, G.; Gushin, E.; Hall, J.; Hallman, T. J.; Hardtke, D.; Harper, G.; Harris, J. W.; He, P.; Heffner, M.; Heppelmann, S.; Herston, T.; Hill, D.; Hippolyte, B.; Hirsch, A.; Hjort, E.; Hoffmann, G. W.; Horsley, M.; Howe, M.; Huang, H. Z.; Humanic, T. J.; Hümmler, H.; Hunt, W.; Hunter, J.; Igo, G. J.; Ishihara, A.; Ivanshin, Yu. I.; Jacobs, P.; Jacobs, W. W.; Jacobson, S.; Jared, R.; Jensen, P.; Johnson, I.; Jones, P. G.; Judd, E.; Kaneta, M.; Kaplan, M.; Keane, D.; Kenney, V. P.; Khodinov, A.; Klay, J.; Klein, S. R.; Klyachko, A.; Koehler, G.; Konstantinov, A. S.; Kormilitsyne, V.; Kotchenda, L.; Kotov, I.; Kovalenko, A. D.; Kramer, M.; Kravtsov, P.; Krueger, K.; Krupien, T.; Kuczewski, P.; Kuhn, C.; Kunde, G. J.; Kunz, C. L.; Kutuev, R. Kh.; Kuznetsov, A. A.; Lakehal-Ayat, L.; Lamas-Valverde, J.; Lamont, M. A.; Landgraf, J. M.; Lange, S.; Lansdell, C. P.; Lasiuk, B.; Laue, F.; Lebedev, A.; Lecompte, T.; Leonhardt, W. J.; Leontiev, V. M.; Leszczynski, P.; Levine, M. J.; Li, Q.; Li, Q.; Li, Z.; Liaw, C.-J.; Lin, J.; Lindenbaum, S. J.; Lindenstruth, V.; Lindstrom, P. J.; Lisa, M. A.; Liu, H.; Ljubicic, T.; Llope, W. J.; Locurto, G.; Long, H.; Longacre, R. S.; Lopez-Noriega, M.; Lopiano, D.; Love, W. A.; Lutz, J. R.; Lynn, D.; Madansky, L.; Maier, R.; Majka, R.; Maliszewski, A.; Margetis, S.; Marks, K.; Marstaller, R.; Martin, L.; Marx, J.; Matis, H. S.; Matulenko, Yu. A.; Matyushevski, E. A.; McParland, C.; McShane, T. S.; Meier, J.; Melnick, Yu.; Meschanin, A.; Middlekamp, P.; Mikhalin, N.; Miller, B.; Milosevich, Z.; Minaev, N. G.; Minor, B.; Mitchell, J.; Mogavero, E.; Moiseenko, V. A.; Moltz, D.; Moore, C. F.; Morozov, V.; Morse, R.; de Moura, M. M.; Munhoz, M. G.; Mutchler, G. S.; Nelson, J. M.; Nevski, P.; Ngo, T.; Nguyen, M.; Nguyen, T.; Nikitin, V. A.; Nogach, L. V.; Noggle, T.; Norman, B.; Nurushev, S. B.; Nussbaum, T.; Nystrand, J.; Odyniec, G.; Ogawa, A.; Ogilvie, C. A.; Olchanski, K.; Oldenburg, M.; Olson, D.; Ososkov, G. A.; Ott, G.; Padrazo, D.; Paic, G.; Pandey, S. U.; Panebratsev, Y.; Panitkin, S. Y.; Pavlinov, A. I.; Pawlak, T.; Pentia, M.; Perevotchikov, V.; Peryt, W.; Petrov, V. A.; Pinganaud, W.; Pirogov, S.; Platner, E.; Pluta, J.; Polk, I.; Porile, N.; Porter, J.; Poskanzer, A. M.; Potrebenikova, E.; Prindle, D.; Pruneau, C.; Puskar-Pasewicz, J.; Rai, G.; Rasson, J.; Ravel, O.; Ray, R. L.; Razin, S. V.; Reichhold, D.; Reid, J.; Renfordt, R. E.; Retiere, F.; Ridiger, A.; Riso, J.; Ritter, H. G.; Roberts, J. B.; Roehrich, D.; Rogachevski, O. V.; Romero, J. L.; Roy, C.; Russ, D.; Rykov, V.; Sakrejda, I.; Sanchez, R.; Sandler, Z.; Sandweiss, J.; Sappenfield, P.; Saulys, A. C.; Savin, I.; Schambach, J.; Scharenberg, R. P.; Scheblien, J.; Scheetz, R.; Schlueter, R.; Schmitz, N.; Schroeder, L. S.; Schulz, M.; Schüttauf, A.; Sedlmeir, J.; Seger, J.; Seliverstov, D.; Seyboth, J.; Seyboth, P.; Seymour, R.; Shakaliev, E. I.; Shestermanov, K. E.; Shi, Y.; Shimanskii, S. S.; Shuman, D.; Shvetcov, V. S.; Skoro, G.; Smirnov, N.; Smykov, L. P.; Snellings, R.; Solberg, K.; Sowinski, J.; Spinka, H. M.; Srivastava, B.; Stephenson, E. J.; Stock, R.; Stolpovsky, A.; Stone, N.; Stone, R.; Strikhanov, M.; Stringfellow, B.; Stroebele, H.; Struck, C.; Suaide, A. A.; Sugarbaker, E.; Suire, C.; Symons, T. J.; Takahashi, J.; Tang, A. H.; Tarchini, A.; Tarzian, J.; Thomas, J. H.; Tikhomirov, V.; Szanto de Toledo, A.; Tonse, S.; Trainor, T.; Trentalange, S.; Tokarev, M.; Tonjes, M. B.; Trofimov, V.; Tsai, O.; Turner, K.; Ullrich, T.; Underwood, D. G.; Vakula, I.; van Buren, G.; Vandermolen, A. M.; Vanyashin, A.; Vasilevski, I. M.; Vasiliev, A. N.; Vigdor, S. E.; Visser, G.; Voloshin, S. A.; Vu, C.; Wang, F.; Ward, H.; Weerasundara, D.; Weidenbach, R.; Wells, R.; Wells, R.; Wenaus, T.; Westfall, G. D.; Whitfield, J. P.; Whitten, C.; Wieman, H.; Willson, R.; Wilson, K.; Wirth, J.; Wisdom, J.; Wissink, S. W.; Witt, R.; Wolf, J.; Wood, L.; Xu, N.; Xu, Z.; Yakutin, A. E.; Yamamoto, E.; Yang, J.; Yepes, P.; Yokosawa, A.; Yurevich, V. I.; Zanevski, Y. V.; Zhang, J.; Zhang, W. M.; Zhu, J.; Zimmerman, D.; Zoulkarneev, R.; Zubarev, A. N.</p> <p>2001-01-01</p> <p><span class="hlt">Elliptic</span> flow from nuclear collisions is a hadronic observable sensitive to the early stages of system evolution. We report first results on <span class="hlt">elliptic</span> flow of charged particles at midrapidity in Au+Au collisions at sNN = 130 GeV using the STAR Time Projection Chamber at the Relativistic Heavy Ion Collider. The <span class="hlt">elliptic</span> flow signal, v2, averaged over transverse momentum, reaches values of about 6% for relatively peripheral collisions and decreases for the more central collisions. This can be interpreted as the observation of a higher degree of thermalization than at lower collision energies. Pseudorapidity and transverse momentum dependence of <span class="hlt">elliptic</span> flow are also presented.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/22348550','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/22348550"><span id="translatedtitle">Excess <span class="hlt">ellipticity</span> of hot and cold spots in the WMAP data?</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Berntsen, Eirik; Hansen, Frode K. E-mail: frodekh@astro.uio.no</p> <p>2013-12-10</p> <p>We investigate claims of excess <span class="hlt">ellipticity</span> of hot and cold spots in the Wilkinson Microwave Anisotropy Probe (WMAP) data. Using the cosmic microwave background (CMB) data from 7 yr of observations by the WMAP satellite, we find, contrary to previous claims of a 10σ detection of excess <span class="hlt">ellipticity</span> in the 3 yr data, that the <span class="hlt">ellipticity</span> of hot and cold spots is perfectly consistent with simulated CMB maps based on the concordance cosmology. We further test for excess obliquity and excess skewness/kurtosis of <span class="hlt">ellipticity</span> and obliquity and find the WMAP7 data consistent with Gaussian simulated maps.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2000Icar..145..108B','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2000Icar..145..108B"><span id="translatedtitle">Interpreting the <span class="hlt">Elliptical</span> Crater Populations on Mars, Venus, and the Moon</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Bottke, William F.; Love, Stanley G.; Tytell, David; Glotch, Timothy</p> <p>2000-05-01</p> <p>Asteroids or comets striking a planetary surface at very shallow angles produce <span class="hlt">elliptical</span>-shaped craters. According to laboratory impact experiments (D. E. Gault and J. A. Wedekind 1978, Proc. Lunar Planet. Sci. Conf. 9th, 3843-3875), <span class="hlt">elliptical</span> craters result from impact angles within ˜5° of horizontal and less than 1% of projectiles with isotropic impact trajectories create <span class="hlt">elliptical</span> craters. This result disagrees with survey results which suggest that approximately 5% of all kilometer-sized craters formed on Mars, Venus, and the Moon have <span class="hlt">elliptical</span> shapes. To explain this discrepancy, we examined the threshold incidence angle necessary to produce <span class="hlt">elliptical</span> craters in laboratory impact experiments. Recent experiments show that aluminum targets produce elongated craters at much steeper impact angles than sand targets. This suggests that target properties are as important as the projectile's impact angle in determining the eventual <span class="hlt">ellipticity</span> of the crater. Creating a model which interpolates between impact data produced using sand and aluminum targets, we derive a new <span class="hlt">elliptical</span> crater threshold angle of 12° from horizontal for Mars, Venus, and the Moon. This leads to a predicted proportion of <span class="hlt">elliptical</span> craters that matches observations within uncertainty given a random projectile population. We conclude that the observed proportion of <span class="hlt">elliptical</span> craters on these bodies is a natural by-product of projectiles striking at random angles, and that no additional formation mechanisms are needed.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2008ApJ...686.1007B','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2008ApJ...686.1007B"><span id="translatedtitle">AGB Connection and Ultraviolet Luminosity Excess in <span class="hlt">Elliptical</span> Galaxies</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Buzzoni, Alberto; González-Lópezlira, Rosa A.</p> <p>2008-10-01</p> <p>Relying on infrared surface brightness fluctuactions to trace AGB properties in a sample of <span class="hlt">elliptical</span> galaxies in the Virgo and Fornax Clusters, we assess the puzzling origin of the ``UV upturn'' phenomenon, recently traced to the presence of a hot horizontal branch (HB) stellar component. The UV upturn actually signals a profound change in the galaxy stellar populations, involving both the hot stellar component and red giant evolution. In particular, the strengthening of the UV rising branch is always seen to correspond to a shortening in AGB deployment; this trend can be readily interpreted as an age effect, perhaps mildly modulated by metal abundance. Brightest stars in <span class="hlt">ellipticals</span> are all found to be genuine AGB members, all the way, and with the AGB tip exceeding the RGB tip by some 0.5-1.5 mag. The inferred core mass of these stars is found to be lesssim0.57 M⊙ among giant <span class="hlt">ellipticals</span>. This value accounts for the recognized deficiency of planetary nebulae in these galaxies, as a result of a lengthy transition time for the post-AGB stellar core to become a hard UV emitter and eventually ``fire up'' the nebula. The combined study of galaxy (1550 - V)0 color and integrated Hβ index points to a a bimodal temperature distribution for the HB with both a red clump and an extremely blue component, in a relative proportion [N(RHB) : N(BHB)] ~ [80 : 20]. For the BHB stellar population, [Fe/H] values of either simeq-0.7 or gtrsim+0.5 dex may provide the optimum ranges to feed the needed low-mass stars (M*ll 0.58 M⊙) that at some stage begin to join the standard red clump stars.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2010MNRAS.407.1148C','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2010MNRAS.407.1148C"><span id="translatedtitle">Hydrostatic equilibrium profiles for gas in <span class="hlt">elliptical</span> galaxies</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Capelo, Pedro R.; Natarajan, Priyamvada; Coppi, Paolo S.</p> <p>2010-09-01</p> <p>We present an analytic formulation for the equilibrium gas density profile of early-type galaxies that explicitly includes the contribution of stars in the gravitational potential. We build a realistic model for an isolated <span class="hlt">elliptical</span> galaxy and explore the equilibrium gas configurations as a function of multiple parameters. For an assumed central gas temperature kBT0 = 0.6 keV, we find that neglecting the gravitational effects of stars, which can contribute substantially in the innermost regions, leads to an underestimate of the enclosed baryonic gas mass by up to ~65 per cent at the effective radius and by up to ~15 per cent at the Navarro-Frenk-White (NFW) scale radius, depending on the stellar baryon fraction. This formula is therefore important for estimating the baryon fraction in an unbiased fashion. These new hydrostatic equilibrium solutions, derived for the isothermal and polytropic cases, can also be used to generate more realistic initial conditions for simulations of <span class="hlt">elliptical</span> galaxies. Moreover, the new formulation is relevant when interpreting X-ray data. We compare our composite isothermal model to the standard β-model used to fit X-ray observations of early-type galaxies, to determine the value of the NFW scale radius rs. Assuming a 10 per cent stellar baryon fraction, we find that the exclusion of stars from the gravitational potential leads to (i) an underestimate of rs by ~80 per cent and (ii) an overestimate of the enclosed dark matter at rs by a factor of ~2, compared to the equivalent β-model fit results when stars are not taken into account. For higher stellar mass fractions, a β-model is unable to accurately reproduce our solution, indicating that when the observed surface brightness profile of an isolated <span class="hlt">elliptical</span> galaxy is found to be well fitted by a β-model, the stellar mass fraction cannot be much greater than ~10 per cent.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://www.osti.gov/scitech/servlets/purl/1331207','SCIGOV-STC'); return false;" href="http://www.osti.gov/scitech/servlets/purl/1331207"><span id="translatedtitle">On the <span class="hlt">elliptic</span> genera of manifolds of Spin(7) holonomy</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Benjamin, Nathan; Harrison, Sarah M.; Kachru, Shamit; Paquette, Natalie M.; Whalen, Daniel</p> <p>2015-12-16</p> <p>Superstring compactification on a manifold of Spin(7) holonomy gives rise to a 2d worldsheet conformal field theory with an extended supersymmetry algebra. The N=1 superconformal algebra is extended by additional generators of spins 2 and 5/2, and instead of just superconformal symmetry one has a c = 12 realization of the symmetry group SW(3/2,2). In this paper, we compute the characters of this supergroup and decompose the <span class="hlt">elliptic</span> genus of a general Spin(7) compactification in terms of these characters. Here, we find suggestive relations to various sporadic groups, which are made more precise in a companion paper.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://www.osti.gov/scitech/servlets/purl/1333526','SCIGOV-STC'); return false;" href="http://www.osti.gov/scitech/servlets/purl/1333526"><span id="translatedtitle">On the <span class="hlt">Elliptic</span> Genera of Manifolds of Spin(7) Holonomy</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Benjamin, Nathan; Harrison, Sarah M.; Kachru, Shamit; Paquette, Natalie M.; Whalen, Daniel</p> <p>2015-12-16</p> <p>Superstring compactification on a manifold of Spin(7) holonomy gives rise to a 2d worldsheet conformal field theory with an extended supersymmetry algebra. The N=1N=1 superconformal algebra is extended by additional generators of spins 2 and 5/2, and instead of just superconformal symmetry one has a c = 12 realization of the symmetry group SW(3/2,2)SW(3/2,2) . In this paper, we compute the characters of this supergroup and decompose the <span class="hlt">elliptic</span> genus of a general Spin(7) compactification in terms of these characters. We find suggestive relations to various sporadic groups, which are made more precise in a companion paper.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017NIMPA.841..104C','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017NIMPA.841..104C"><span id="translatedtitle">Optimization design of a 20-in. <span class="hlt">elliptical</span> MCP-PMT</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Chen, Ping; Tian, Jinshou; Wei, Yonglin; Liu, Hulin; Sai, Xiaofeng; He, Jianping; Chen, Lin; Wang, Xing; Lu, Yu</p> <p>2017-01-01</p> <p>This paper describes the simulation work for optimizing the newly developed 20-in. <span class="hlt">elliptical</span> MCP-PMT by enlarging the outside diameters of the two focusing electrodes and the open area of the glass bulb. Effects of biasing voltages applied to the two focusing electrodes and the MCP input facet are studied. With the new design of the 20 in. MCP-PMT, the transit time spread of the prototype can be less than 3 ns and the collection efficiency is as much as the present prototype.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/27607713','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/27607713"><span id="translatedtitle">Chopper z-scan technique for <span class="hlt">elliptic</span> Gaussian beams.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Dávila-Pintle, J A; Reynoso-Lara, E; Bravo-García, Y E</p> <p>2016-09-05</p> <p>This paper reports an improvement to the chopper z-scan technique for <span class="hlt">elliptic</span> Gaussian beams. This improvement results in a higher sensitivity by measuring the ratio of eclipsing time to rotating period (duty cycle) of a chopper that eclipses the beam along the main axis. It is shown that the z-scan curve of the major axis is compressed along the z-axis. This compression factor is equal to the ratio between the minor and major axes. It was found that the normalized peak-valley difference with respect to the linear value does not depend on the axis along which eclipsing occurs.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://www.osti.gov/scitech/servlets/purl/433337','SCIGOV-STC'); return false;" href="http://www.osti.gov/scitech/servlets/purl/433337"><span id="translatedtitle">Incomplete block factorization preconditioning for indefinite <span class="hlt">elliptic</span> problems</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Guo, Chun-Hua</p> <p>1996-12-31</p> <p>The application of the finite difference method to approximate the solution of an indefinite <span class="hlt">elliptic</span> problem produces a linear system whose coefficient matrix is block tridiagonal and symmetric indefinite. Such a linear system can be solved efficiently by a conjugate residual method, particularly when combined with a good preconditioner. We show that specific incomplete block factorization exists for the indefinite matrix if the mesh size is reasonably small. And this factorization can serve as an efficient preconditioner. Some efforts are made to estimate the eigenvalues of the preconditioned matrix. Numerical results are also given.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/22036628','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/22036628"><span id="translatedtitle">Exact revision of the <span class="hlt">elliptically</span> bent mirror theory</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Mao Chengwen; Yu Xiaohan; Xiao Tiqiao; Li Aiguo; Yang Ke; Wang Hua; Yan Fen; Deng Biao</p> <p>2011-06-01</p> <p>One of the main hurdles for nanometer focusing by a bending mirror lies in the theoretical surface errors by its approximations used for the traditional theory. The impacts of approximations and analytical corrections have been discussed, and the <span class="hlt">elliptically</span> bent mirror theory has been described during exact mathematical analysis without any approximations. These approximations are harmful for the focusing system with bigger grazing angle, bigger mirror length, and bigger numerical aperture. The properties of equal-moment and single-moment bent mirrors have been described and discussed. Because of its obvious advantages, a single-moment bending mirror has high potential ability for nanometer focusing.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2010AIPC.1264....1F','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2010AIPC.1264....1F"><span id="translatedtitle">Generators for the <span class="hlt">elliptic</span> curve y2 = x3-nx</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Fujita, Yasutsugu; Terai, Nobuhiro</p> <p>2010-07-01</p> <p>Let E:y2 = x3-nx be an <span class="hlt">elliptic</span> curve over the rationals with a positive integer n. Mordell's theorem asserts that the group of rational points on E is finitely generated. Our interest is in the generators for its free part. Duquesne (2007) showed that if n = (2k2-2k+1)(18k2+30k+17) is square-free, then certain two points of infinite order can always be in a system of generators. We generalize this result and show that the same is true for "infinitely many" infinite families n = n(k,l) with two variables.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19920002474','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19920002474"><span id="translatedtitle">Some fast <span class="hlt">elliptic</span> solvers on parallel architectures and their complexities</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Gallopoulos, E.; Saad, Youcef</p> <p>1989-01-01</p> <p>The discretization of separable <span class="hlt">elliptic</span> partial differential equations leads to linear systems with special block triangular matrices. Several methods are known to solve these systems, the most general of which is the Block Cyclic Reduction (BCR) algorithm which handles equations with nonconsistant coefficients. A method was recently proposed to parallelize and vectorize BCR. Here, the mapping of BCR on distributed memory architectures is discussed, and its complexity is compared with that of other approaches, including the Alternating-Direction method. A fast parallel solver is also described, based on an explicit formula for the solution, which has parallel computational complexity lower than that of parallel BCR.</p> </li> </ol> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_18");'>18</a></li> <li><a href="#" onclick='return showDiv("page_19");'>19</a></li> <li class="active"><span>20</span></li> <li><a href="#" onclick='return showDiv("page_21");'>21</a></li> <li><a href="#" onclick='return showDiv("page_22");'>22</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div><!-- col-sm-12 --> </div><!-- row --> </div><!-- page_20 --> <div id="page_21" class="hiddenDiv"> <div class="row"> <div class="col-sm-12"> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_19");'>19</a></li> <li><a href="#" onclick='return showDiv("page_20");'>20</a></li> <li class="active"><span>21</span></li> <li><a href="#" onclick='return showDiv("page_22");'>22</a></li> <li><a href="#" onclick='return showDiv("page_23");'>23</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div> </div> <div class="row"> <div class="col-sm-12"> <ol class="result-class" start="401"> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19900031624&hterms=Computational+Complexity&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D40%26Ntt%3DComputational%2BComplexity','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19900031624&hterms=Computational+Complexity&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D40%26Ntt%3DComputational%2BComplexity"><span id="translatedtitle">Some fast <span class="hlt">elliptic</span> solvers on parallel architectures and their complexities</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Gallopoulos, E.; Saad, Y.</p> <p>1989-01-01</p> <p>The discretization of separable <span class="hlt">elliptic</span> partial differential equations leads to linear systems with special block tridiagonal matrices. Several methods are known to solve these systems, the most general of which is the Block Cyclic Reduction (BCR) algorithm which handles equations with nonconstant coefficients. A method was recently proposed to parallelize and vectorize BCR. In this paper, the mapping of BCR on distributed memory architectures is discussed, and its complexity is compared with that of other approaches including the Alternating-Direction method. A fast parallel solver is also described, based on an explicit formula for the solution, which has parallel computational compelxity lower than that of parallel BCR.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2015JGP....91..141B','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2015JGP....91..141B"><span id="translatedtitle">Irreducible vector bundles on some <span class="hlt">elliptic</span> non-Kahler threefolds</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Brînzănescu, Vasile; Vuletescu, Victor</p> <p>2015-05-01</p> <p>We study rank-2 vector bundles on non-Kähler threefolds π : X → B, which are <span class="hlt">elliptic</span> principal bundles with at least one non-zero Chern class over a complex surface B with no curves. In this case, we prove that every rank-2 irreducible vector bundle on X is a pull-back from B up to a twist by a line bundle. These 2-vector bundles are, via the Kobayashi-Hitchin correspondence, solutions of the Yang-Mills equations on the threefold X.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017JMP....58c1503F','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017JMP....58c1503F"><span id="translatedtitle">Existence of solution for a generalized quasilinear <span class="hlt">elliptic</span> problem</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Furtado, Marcelo F.; Silva, Edcarlos D.; Silva, Maxwell L.</p> <p>2017-03-01</p> <p>It establishes existence and multiplicity of solutions to the <span class="hlt">elliptic</span> quasilinear Schrödinger equation -div(g2(u ) ∇u ) +g (u ) g'(u ) |∇u| 2 +V (x ) u =h (x ,u ) ,x ∈ℝN ,where g, h, V are suitable smooth functions. The function g is asymptotically linear at infinity and, for each fixed x ∈ℝN , the function h(x, s) behaves like s at the origin and s3 at infinity. In the proofs, we apply variational methods.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2015AmJPh..83..205Z','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2015AmJPh..83..205Z"><span id="translatedtitle">Wave functions of <span class="hlt">elliptical</span> quantum dots in a magnetic field</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Zhou, Daming; Lorke, Axel</p> <p>2015-03-01</p> <p>We use the variational principle to obtain the wave functions of <span class="hlt">elliptical</span> quantum dots under the influence of an external magnetic field. For the first excited states, whose wave functions have recently been mapped experimentally, we find a simple expression, based on a linear combination of the wave functions in the absence of a magnetic field. The results illustrate how a magnetic field breaks the x-y symmetry and mixes the corresponding eigenstates. The obtained eigenenergies agree well with those obtained by more involved analytical and numerical methods.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/6314229','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/6314229"><span id="translatedtitle">Construction of preconditioners for <span class="hlt">elliptic</span> problems by substructuring. II</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Bramble, J.H.; Pasciak, J.E.; Schatz, A.H.</p> <p>1987-07-01</p> <p>We give a method for constructing preconditioners for the discrete systems arising in the approximation of solutions of <span class="hlt">elliptic</span> boundary value problems. These preconditioners are based on domain decomposition techniques and lead to algorithms which are well suited for parallel computing environments. The method presented in this paper leads to a preconditioned system with condition number proportional to d/h where d is the subdomain size and h is the mesh size. These techniques are applied to singularly perturbed problems and problems in the three dimensions. The results of numerical experiments illustrating the performance of the method on problems in two and three dimensions are given.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/5516008','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/5516008"><span id="translatedtitle">The construction of preconditioners for <span class="hlt">elliptic</span> problems by substructuring, IV</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Bramble, J.H.; Pasciak, J.E.; Schatz, A.H.</p> <p>1989-07-01</p> <p>We consider the problem of solving the algebraic system of equations which result from the discretization of <span class="hlt">elliptic</span> boundary value problems defined on three-dimensional Euclidean space. We develop preconditioners for such systems based on substructuring (also known as domain decomposition). The resulting algorithms are well suited to emerging parallel computing architectures. We describe two techniques for developing these preconditioners. A theory for the analysis of the condition number for the resulting preconditioned system is given and the results of supporting numerical experiments are presented.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/6647075','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/6647075"><span id="translatedtitle">Iterative schemes for nonsymmetric and indefinite <span class="hlt">elliptic</span> boundary value problems</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Bramble, J.H.; Leyk, Z.; Pasciak, J.E.</p> <p>1993-01-01</p> <p>The purpose of this paper is twofold. The first is to describe some simple and robust iterative schemes for nonsymmetric and indefinite <span class="hlt">elliptic</span> boundary value problems. The schemes are based in the Sobolev space H ([Omega]) and require minimal hypotheses. The second is to develop algorithms utilizing a coarse-grid approximation. This leads to iteration matrices whose eigenvalues lie in the right half of the complex plane. In fact, for symmetric indefinite problems, the iteration is reduced to a well-conditioned symmetric positive definite system which can be solved by conjugate gradient interation. Applications of the general theory as well as numerical examples are given. 20 refs., 8 tabs.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/5263436','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/5263436"><span id="translatedtitle">The construction of preconditioners for <span class="hlt">elliptic</span> problems by substructuring, IV</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Bramble, J.H.; Pasciak, J.E.; Schatz, A.H.</p> <p>1987-06-01</p> <p>We consider the problem of solving the algebraic system of equations which result from the discretization of <span class="hlt">elliptic</span> boundary value problems defined on three dimensional Euclidean space. We develop preconditioners for such systems based on substructuring (also known as domain decomposition). The resulting algorithms are well suited to emerging parallel computing architectures. We describe two techniques for developing these precondictioners. A theory for the analysis of the condition number for the resulting preconditioned system is given and the results of supporting numerical experiments are presented. 16 refs., 2 tabs.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/6649004','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/6649004"><span id="translatedtitle">Iterative method for <span class="hlt">elliptic</span> problems on regions partitioned into substructures</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Bramble, J.H.; Pasciak, J.E.; Schatz, A.H.</p> <p>1986-04-01</p> <p>Some new preconditioners for discretizations of <span class="hlt">elliptic</span> boundary problems are studied. With these preconditioners, the domain under consideration is broken into subdomains and preconditioners are defined which only require the solution of matrix problems on the subdomains. Analytic estimates are given which guarantee that under appropriate hypotheses, the preconditioned iterative procedure converges to the solution of the discrete equations with a rate per iteration that is independent of the number of unknowns. Numerical examples are presented which illustrate the theoretically predicted iterative convergence rates.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/21067566','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/21067566"><span id="translatedtitle">Optimal Control of the Obstacle for an <span class="hlt">Elliptic</span> Variational Inequality</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Adams, D. R.; Lenhart, S. M.; Yong, J.</p> <p>1998-09-15</p> <p>An optimal control problem for an <span class="hlt">elliptic</span> obstacle variational inequality is considered. The obstacle is taken to be the control and the solution to the obstacle problem is taken to be the state. The goal is to find the optimal obstacle from H{sup 1}{sub 0} ({omega}) so that the state is close to the desired profile while the H{sup 1}({omega}) norm of the obstacle is not too large. Existence, uniqueness, and regularity as well as some characterizations of the optimal pairs are established.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19730038110&hterms=satellite+orientation&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3Dsatellite%2Borientation','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19730038110&hterms=satellite+orientation&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3Dsatellite%2Borientation"><span id="translatedtitle">Orientation and resonance locks for satellites in the <span class="hlt">elliptic</span> orbit.</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Liu, H.-S.</p> <p>1972-01-01</p> <p>In order to achieve the maximum strength of higher resonance locks for satellites in the <span class="hlt">elliptic</span> orbit, the condition of satellite orientation during the process of deployment is established. It is shown that for maximum strength locks the axis of the minimum moment of inertia of satellites should point toward the attracting body at plus or minus (5/8) pi and 0 values of the true anomaly f. This condition of deployment is applicable to all cases of resonance rotation regardless of the value of lock number k and orbit eccentricity e.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4197466','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4197466"><span id="translatedtitle">Some new addition formulae for Weierstrass <span class="hlt">elliptic</span> functions</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Eilbeck, J. Chris; England, Matthew; Ônishi, Yoshihiro</p> <p>2014-01-01</p> <p>We present new addition formulae for the Weierstrass functions associated with a general <span class="hlt">elliptic</span> curve. We prove the structure of the formulae in n-variables and give the explicit addition formulae for the 2- and 3-variable cases. These new results were inspired by new addition formulae found in the case of an equianharmonic curve, which we can now observe as a specialization of the results here. The new formulae, and the techniques used to find them, also follow the recent work for the generalization of Weierstrass functions to curves of higher genus. PMID:25383018</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2006JDE...226...99B','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2006JDE...226...99B"><span id="translatedtitle">Characterization of the shape stability for nonlinear <span class="hlt">elliptic</span> problems</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Bucur, Dorin</p> <p></p> <p>We characterize all geometric perturbations of an open set, for which the solution of a nonlinear <span class="hlt">elliptic</span> PDE of p-Laplacian type with Dirichlet boundary condition is stable in the L-norm. The necessary and sufficient conditions are jointly expressed by a geometric property associated to the γ-convergence. If the dimension N of the space satisfies N-1<p⩽N and if the number of the connected components of the complements of the moving domains are uniformly bounded, a simple characterization of the uniform convergence can be derived in a purely geometric frame, in terms of the Hausdorff complementary convergence. Several examples are presented.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2012ArRMA.205..345A','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2012ArRMA.205..345A"><span id="translatedtitle">Singular Solutions of Fully Nonlinear <span class="hlt">Elliptic</span> Equations and Applications</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Armstrong, Scott N.; Sirakov, Boyan; Smart, Charles K.</p> <p>2012-08-01</p> <p>We study the properties of solutions of fully nonlinear, positively homogeneous <span class="hlt">elliptic</span> equations near boundary points of Lipschitz domains at which the solution may be singular. We show that these equations have two positive solutions in each cone of {R^n} , and the solutions are unique in an appropriate sense. We introduce a new method for analyzing the behavior of solutions near certain Lipschitz boundary points, which permits us to classify isolated boundary singularities of solutions which are bounded from either above or below. We also obtain a sharp Phragmén-Lindelöf result as well as a principle of positive singularities in certain Lipschitz domains.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/1331260','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/1331260"><span id="translatedtitle">Conforming and nonconforming virtual element methods for <span class="hlt">elliptic</span> problems</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Cangiani, Andrea; Manzini, Gianmarco; Sutton, Oliver J.</p> <p>2016-08-03</p> <p>Here we present, in a unified framework, new conforming and nonconforming virtual element methods for general second-order <span class="hlt">elliptic</span> problems in two and three dimensions. The differential operator is split into its symmetric and nonsymmetric parts and conditions for stability and accuracy on their discrete counterparts are established. These conditions are shown to lead to optimal H<sup>1</sup>- and L<sup>2</sup>-error estimates, confirmed by numerical experiments on a set of polygonal meshes. The accuracy of the numerical approximation provided by the two methods is shown to be comparable.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/pages/biblio/1331260-conforming-nonconforming-virtual-element-methods-elliptic-problems','SCIGOV-DOEP'); return false;" href="https://www.osti.gov/pages/biblio/1331260-conforming-nonconforming-virtual-element-methods-elliptic-problems"><span id="translatedtitle">Conforming and nonconforming virtual element methods for <span class="hlt">elliptic</span> problems</span></a></p> <p><a target="_blank" href="http://www.osti.gov/pages">DOE PAGES</a></p> <p>Cangiani, Andrea; Manzini, Gianmarco; Sutton, Oliver J.</p> <p>2016-08-03</p> <p>Here we present, in a unified framework, new conforming and nonconforming virtual element methods for general second-order <span class="hlt">elliptic</span> problems in two and three dimensions. The differential operator is split into its symmetric and nonsymmetric parts and conditions for stability and accuracy on their discrete counterparts are established. These conditions are shown to lead to optimal H1- and L2-error estimates, confirmed by numerical experiments on a set of polygonal meshes. The accuracy of the numerical approximation provided by the two methods is shown to be comparable.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=20040082326&hterms=crossover+design&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3Dcrossover%2Bdesign','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=20040082326&hterms=crossover+design&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3Dcrossover%2Bdesign"><span id="translatedtitle">Design Space Issues for <span class="hlt">Intrinsic</span> Evolvable Hardware</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Hereford, James; Gwaltney, David</p> <p>2004-01-01</p> <p>This paper discuss the problem of increased programming time for <span class="hlt">intrinsic</span> evolvable hardware (EHW) as the complexity of the circuit grows. We develop equations for the size of the population, n, and the number of generations required for the population to converge, ngen, based on L, the length of the programming string. We show that the processing time of the computer becomes negligible for <span class="hlt">intrinsic</span> EHW since the selection/crossover/mutation steps are only done once per generation, suggesting there is room for use of more complex evolutionary algorithms m <span class="hlt">intrinsic</span> EHW. F i y , we review the state of the practice and discuss the notion of a system design approach for <span class="hlt">intrinsic</span> EHW.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/23400402','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/23400402"><span id="translatedtitle">Recovering <span class="hlt">intrinsic</span> fluorescence by Monte Carlo modeling.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Müller, Manfred; Hendriks, Benno H W</p> <p>2013-02-01</p> <p>We present a novel way to recover <span class="hlt">intrinsic</span> fluorescence in turbid media based on Monte Carlo generated look-up tables and making use of a diffuse reflectance measurement taken at the same location. The method has been validated on various phantoms with known <span class="hlt">intrinsic</span> fluorescence and is benchmarked against photon-migration methods. This new method combines more flexibility in the probe design with fast reconstruction and showed similar reconstruction accuracy as found in other reconstruction methods.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/19745710','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/19745710"><span id="translatedtitle">Refining the <span class="hlt">intrinsic</span> chimera flap: a review.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Agarwal, Jayant P; Agarwal, Shailesh; Adler, Neta; Gottlieb, Lawrence J</p> <p>2009-10-01</p> <p>Reconstruction of complex tissue deficiencies in which each missing component is in a different spatial relationship to each other can be particularly challenging, especially in patients with limited recipient vessels. The chimera flap design is uniquely suited to reconstruct these deformities. Chimera flaps have been previously defined in many ways with 2 main categories: prefabricated or <span class="hlt">intrinsic</span>. Herein we attempt to clarify the definition of a true <span class="hlt">intrinsic</span> chimeric flap and provide examples of how these constructs provide a method for reconstruction of complex defects. The versatility of the <span class="hlt">intrinsic</span> chimera flap and its procurement from 7 different vascular systems is described. A clarification of the definition of a true <span class="hlt">intrinsic</span> chimera flap is described. In addition, construction of flaps from the lateral femoral circumflex, deep circumflex iliac, inferior gluteal, peroneal, subscapular, thoracodorsal, and radial arterial systems is described to showcase the versatility of these chimera flaps. A true <span class="hlt">intrinsic</span> chimera flap must consist of more than a single tissue type. Each of the tissue components receives its blood flow from separate vascular branches or perforators that are connected to a single vascular source. These vascular branches must be of appropriate length to allow for insetting with 3-dimensional spatial freedom. There are a multitude of sites from which true <span class="hlt">intrinsic</span> chimera flaps may be harvested.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/26360839','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/26360839"><span id="translatedtitle">Miniaturized <span class="hlt">INtrinsic</span> DISsolution Screening (MINDISS) assay for preformulation.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Alsenz, Jochem; Haenel, Elisabeth; Anedda, Aline; Du Castel, Pauline; Cirelli, Giorgio</p> <p>2016-05-25</p> <p>This study describes a novel Miniaturized <span class="hlt">INtrinsic</span> DISsolution Screening (MINDISS) assay for measuring disk <span class="hlt">intrinsic</span> dissolution rates (DIDR). In MINDISS, compacted mini disks of drugs (2-5mg/disk) are prepared in custom made holders with a surface area of 3mm(2). Disks are immersed, pellet side down, into 0.35ml of appropriate dissolution media per well in 96-well microtiter plates, media are stirred and disk-holders are transferred to new wells after defined periods of time. After filtration, drug concentration in dissolution media is quantified by Ultra Performance Liquid Chromatography (UPLC) and solid state property of the disk is characterized by Raman spectroscopy. MINDISS was identified as an easy-to-use tool for rapid, parallel determination of DIDR of compounds that requires only small amounts of compound and of dissolution medium. Results obtained with marketed drugs in MINDISS <span class="hlt">correlate</span> well with large scale DIDR methods and indicate that MINDISS can be used for (1) rank-ordering of compounds by <span class="hlt">intrinsic</span> dissolution in late phase discovery and early development, (2) comparison of polymorphic forms and salts, (3) screening and selection of appropriate dissolution media, and (4) characterization of the intestinal release behavior of compounds along the gastro intestinal tract by changing biorelevant media during experiments.</p> </li> </ol> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_19");'>19</a></li> <li><a href="#" onclick='return showDiv("page_20");'>20</a></li> <li class="active"><span>21</span></li> <li><a href="#" onclick='return showDiv("page_22");'>22</a></li> <li><a href="#" onclick='return showDiv("page_23");'>23</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div><!-- col-sm-12 --> </div><!-- row --> </div><!-- page_21 --> <div id="page_22" class="hiddenDiv"> <div class="row"> <div class="col-sm-12"> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_20");'>20</a></li> <li><a href="#" onclick='return showDiv("page_21");'>21</a></li> <li class="active"><span>22</span></li> <li><a href="#" onclick='return showDiv("page_23");'>23</a></li> <li><a href="#" onclick='return showDiv("page_24");'>24</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div> </div> <div class="row"> <div class="col-sm-12"> <ol class="result-class" start="421"> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/6622182','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/6622182"><span id="translatedtitle"><span class="hlt">Intrinsic</span> vs extrinsic motivation in learning disabled children.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Reeve, P T; Loper, A B</p> <p>1983-08-01</p> <p>44 children identified as learning disabled were administered Harter's Scale of <span class="hlt">Intrinsic</span> Versus Extrinsic Orientation in the Classroom. Scores were <span class="hlt">correlated</span> with several indices of school behavior, standardized achievement test scores, report-card letter grades, and teachers' behavioral ratings. No consistent pattern of relationship was evidenced between the scale and academic achievement as assessed by standardized tests and report-card letter grades. However, a weak but statistically significant pattern of relationship (rs .24 to .33) was noted between two subscales of the Harter scale and teachers' behavioral ratings. Internality on these subscales tended to be associated with higher teachers' ratings.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2009LNCS.5844...86H','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2009LNCS.5844...86H"><span id="translatedtitle"><span class="hlt">Intrinsic</span> Monitoring Using Behaviour Models in IPv6 Networks</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Höfig, Edzard; Coşkun, Hakan</p> <p></p> <p>In conventional networks, <span class="hlt">correlating</span> path information to resource utilisation on the granularity of packets is a hard problem when using policy-based traffic handling schemes. We introduce a new approach termed ‘<span class="hlt">intrinsic</span> monitoring’ which relies on the use of IPv6 extension headers in combination with formal behaviour models to gather resource information along a path. This allows a network monitoring system to delegate monitoring functionality to the network devices themselves, with the result of a drastic reduction in management traffic due to the increased autonomy of the monitoring system. As monitoring information travels in-band with the network traffic, path information remains perfectly accurate.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3926902','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3926902"><span id="translatedtitle">Feasibility of using a compact <span class="hlt">elliptical</span> device to increase energy expenditure during sedentary activities</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>Rovniak, Liza S.; Denlinger, LeAnn; Duveneck, Ellen; Sciamanna, Christopher N.; Kong, Lan; Freivalds, Andris; Ray, Chester A.</p> <p>2013-01-01</p> <p>Objectives This study aimed to evaluate the feasibility of using a compact <span class="hlt">elliptical</span> device to increase energy expenditure during sedentary activities. A secondary aim was to evaluate if two accelerometers attached to the <span class="hlt">elliptical</span> device could provide reliable and valid assessments of participants’ frequency and duration of <span class="hlt">elliptical</span> device use. Design Physically inactive adults (n = 32, age range = 25–65) were recruited through local advertisements and selected using stratified random sampling based on sex, body mass index (BMI), and age. Methods Indirect calorimetry was used to assess participants’ energy expenditure while seated and while using the <span class="hlt">elliptical</span> device at a self-selected intensity level. Participants also self-reported their interest in using the <span class="hlt">elliptical</span> device during sedentary activities. Two Actigraph GT3X accelerometers were attached to the <span class="hlt">elliptical</span> device to record time-use patterns. Results Participants expended a median of 179.1 kilocalories per hour while using the <span class="hlt">elliptical</span> device (range = 108.2–269.0), or a median of 87.9 more kilocalories (range = 19.7–178.6) than they would expend per hour of sedentary sitting. Participants reported high interest in using the <span class="hlt">elliptical</span> device during TV watching and computer work, but relatively low interest in using the device during office meetings. Women reported greater interest in using the <span class="hlt">elliptical</span> device than men. The two accelerometers recorded identical time-use patterns on the <span class="hlt">elliptical</span> device and demonstrated concurrent validity with time-stamped computer records. Conclusions Compact <span class="hlt">elliptical</span> devices could increase energy expenditure during sedentary activities, and may provide proximal environmental cues for increasing energy expenditure across multiple life domains. PMID:24035273</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/27824362','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/27824362"><span id="translatedtitle">Electronegativity and <span class="hlt">intrinsic</span> disorder of preeclampsia-related proteins.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Polanco, Carlos; Castañón-González, Jorge Alberto; Uversky, Vladimir N; Buhse, Thomas; Samaniego Mendoza, José Lino; Calva, Juan J</p> <p>2017-01-01</p> <p>Preeclampsia, hemorrhage, and infection are the leading causes of maternal death in underdeveloped countries. Since several proteins associated with preeclampsia are known, we conducted a computational study which evaluated the commonness and potential functionality of <span class="hlt">intrinsic</span> disorder of these proteins and also made an attempt to characterize their origin. The origin of the preeclampsia-related proteins was assessed with a supervised technique, a Polarity Index Method (PIM), which evaluates the electronegativity of proteins based solely on their sequence. The commonness of <span class="hlt">intrinsic</span> disorder was evaluated using several disorder predictors from the PONDR family, the charge-hydropathy plot (CH-plot) and cumulative distribution function (CDF) analyses, and using the MobiDB web-based tool, whereas potential functionality of <span class="hlt">intrinsic</span> disorder was studied with the D2P2 resource and ANCHOR predictor of disorder-based binding sites, and the STRING tool was used to build the interactivity networks of the preeclampsia-related proteins. Peculiarities of the PIM-derived polar profile of the group of preeclampsia-related proteins were then compared with profiles of a group of lipoproteins, antimicrobial peptides, angiogenesis-related proteins, and the <span class="hlt">intrinsically</span> disordered proteins. Our results showed a high graphical <span class="hlt">correlation</span> between preeclampsia proteins, lipoproteins, and the angiogenesis proteins. We also showed that many preeclampsia-related proteins contain numerous functional disordered regions. Therefore, these bioinformatics results led us to assume that the preeclampsia proteins are highly associated with the lipoproteins group, and that some preeclampsia-related proteins contain significant amounts of functional disorders.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/25769218','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/25769218"><span id="translatedtitle">Development of an innovative device for ultrasonic <span class="hlt">elliptical</span> vibration cutting.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Zhou, Ming; Hu, Linhua</p> <p>2015-07-01</p> <p>An innovative ultrasonic <span class="hlt">elliptical</span> vibration cutting (UEVC) device with 1st resonant mode of longitudinal vibration and 3rd resonant mode of bending vibration was proposed in this paper, which can deliver higher output power compared to previous UEVC devices. Using finite element method (FEM), resonance frequencies of the longitudinal and bending vibrations were tuned to be as close as possible in order to excite these two vibrations using two-phase driving voltages at a single frequency, while wave nodes of the longitudinal and bending vibrations were also adjusted to be as coincident as possible for mounting the device at a single fixed point. Based on the simulation analysis results a prototype device was fabricated, then its vibration characteristics were evaluated by an impedance analyzer and a laser displacement sensor. With two-phase sinusoidal driving voltages both of 480 V(p-p) at an ultrasonic frequency of 20.1 kHz, the developed prototype device achieved an <span class="hlt">elliptical</span> vibration with a longitudinal amplitude of 8.9 μm and a bending amplitude of 11.3 μm. The performance of the developed UEVC device is assessed by the cutting tests of hardened steel using single crystal diamond tools. Experimental results indicate that compared to ordinary cutting process, the tool wear is reduced significantly by using the proposed device.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19890065685&hterms=dumb&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D10%26Ntt%3Ddumb','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19890065685&hterms=dumb&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D10%26Ntt%3Ddumb"><span id="translatedtitle">Two high-velocity encounters of <span class="hlt">elliptical</span> galaxies</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Balcells, Marc; Borne, Kirk D.; Hoessel, John G.</p> <p>1989-01-01</p> <p>This paper describes results obtained on a simulation of two high-velocity encounters of NGC 4782/4783 and NGC 2672/2673 binary <span class="hlt">elliptical</span> galaxies which differ substantially in mass ratio (about 1 for the first pair, and about 10 for the second). CCD images and velocities obtained from digital spectra were used to constrain simulations of the galaxy collisions. The binary orbital elements, the orientation of the orbit in the sky, the time since pericenter, and the dynamical mass of the pair were derived. Results suggested that the dumb-bell galaxy NGC 4782/4783 is not a supermassive galaxy, as was claimed earlier on the basis of the high relative velocity and high central dispersion, but has a moderate mass to luminosity ratio M/L(B) of about 10. It was concluded that its trajectory changed from hyperbolic to <span class="hlt">elliptical</span> as a result of energy lost during the collision. It was found that the NGC 2672/2673 also has a moderate M/L(B) of about 7.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2003ASAJ..114.2419B','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2003ASAJ..114.2419B"><span id="translatedtitle">Vibration of in-vacuo <span class="hlt">elliptic</span> cylindrical shells</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Boisvert, Jeffrey E.; Hayek, Sabih I.</p> <p>2003-10-01</p> <p>The equations of motion for the vibration of <span class="hlt">elliptic</span> cylindrical shells of constant thickness were derived using a Galerkin approach. The elastic strain energy density used in this derivation has seven independent kinematic variables: three displacements, two thickness-shear, and two thickness-stretch. The resulting seven coupled algebraic equations are symmetric and positive definite. The shell has a constant thickness, h, finite length, L, and is simply supported at its ends, (z=0,L), where z is the axial coordinate. The <span class="hlt">elliptic</span> cross-section is defined by the shape parameter, a, and the half-length of the major axis, l. The modal solutions are expanded in a doubly infinite series of comparison functions in terms of circular functions in the angular and axial coordinates. The natural frequencies and the mode shapes were obtained by the Galerkin method. Numerical results were obtained for several h/l and L/l ratios, and various shape parameters, including the limiting case of a simply supported cylindrical shell (a=100). [Work supported by ONR and the Navy/ASEE Summer Faculty Program.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2015PhDT........81C','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2015PhDT........81C"><span id="translatedtitle">Analysis and Numerical Treatment of <span class="hlt">Elliptic</span> Equations with Stochastic Data</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Cheng, Shi</p> <p></p> <p>Many science and engineering applications are impacted by a significant amount of uncertainty in the model. Examples include groundwater flow, microscopic biological system, material science and chemical engineering systems. Common mathematical problems in these applications are <span class="hlt">elliptic</span> equations with stochastic data. In this dissertation, we examine two types of stochastic <span class="hlt">elliptic</span> partial differential equations(SPDEs), namely nonlinear stochastic diffusion reaction equations and general linearized elastostatic problems in random media. We begin with the construction of an analysis framework for this class of SPDEs, extending prior work of Babuska in 2010. We then use the framework both for establishing well-posedness of the continuous problems and for posing Galerkintype numerical methods. In order to solve these two types of problems, single integral weak formulations and stochastic collocation methods are applied. Moreover, a priori error estimates for stochastic collocation methods are derived, which imply that the rate of convergence is exponential, along with the order of polynomial increasing in the space of random variables. As expected, numerical experiments show the exponential rate of convergence, verified by a posterior error analysis. Finally, an adaptive strategy driven by a posterior error indicators is designed.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2012Nonli..25.1135T','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2012Nonli..25.1135T"><span id="translatedtitle">The geometry of finite difference discretizations of semilinear <span class="hlt">elliptic</span> operators</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Teles, Eduardo; Tomei, Carlos</p> <p>2012-04-01</p> <p>Discretizations by finite differences of some semilinear <span class="hlt">elliptic</span> equations lead to maps F(u) = Au - f(u), u \\in {{R}}^n , given by nonlinear convex diagonal perturbations of symmetric matrices A. For natural nonlinearity classes, we consider the equation F(u) = y - tp, where t is a large positive number and p is a vector with negative coordinates. As the range of the derivative f'i of the coordinates of f encloses more eigenvalues of A, the number of solutions increases geometrically, eventually reaching 2n. This phenomenon, somewhat in contrast with behaviour associated with the Lazer-McKenna conjecture, has a very simple geometric explanation: a perturbation of a multiple fold gives rise to a function which sends connected components of its critical set to hypersurfaces with large rotation numbers with respect to vectors with very negative coordinates. Strictly speaking, the results have nothing to do with <span class="hlt">elliptic</span> equations: they are properties of the interaction of a (self-adjoint) linear map with increasingly stronger nonlinear convex diagonal interactions.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2014cosp...40E1017G','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2014cosp...40E1017G"><span id="translatedtitle">The distribution of Infrared point sources in nearby <span class="hlt">elliptical</span> galaxies</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Gogoi, Rupjyoti; Misra, Ranjeev; Puthiyaveettil, Shalima</p> <p></p> <p>Infra-red point sources in nearby early-type galaxies are often counterparts of sources in other wavebands such as optical and X-rays. In particular, the IR counterpart of X-ray sources may be due to a globular cluster hosting the X-ray source or could be associated directly with the binary, providing crucial information regarding their environment. In general, the IR sources would be from globular clusters and their IR colors would provide insight into their stellar composition. However, many of the IR sources maybe background objects and it is important to identify them or at least quantify the level of background contamination. Archival Spitzer IRAC images provide a unique opportunity to study these sources in nearby <span class="hlt">Ellipticals</span> and in particular to estimate the distributions of their IR luminosity, color and distance from the center. We will present the results of such an analysis for three nearby galaxies. We have also estimated the background contamination using several blank fields. Our preliminary results suggest that IR colors can be effectively used to differentiate between the background and sources in the galaxy, and that the distribution of sources are markedly different for different <span class="hlt">Elliptical</span> galaxies.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/22257008','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/22257008"><span id="translatedtitle">Experimental study of <span class="hlt">elliptical</span> jet from sub to supercritical conditions</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Muthukumaran, C. K.; Vaidyanathan, Aravind</p> <p>2014-04-15</p> <p>The jet mixing at supercritical conditions involves fluid dynamics as well as thermodynamic phenomena. All the jet mixing studies at critical conditions to the present date have focused only on axisymmetric jets. When the liquid jet is injected into supercritical environment, the thermodynamic transition could be well understood by considering one of the important fluid properties such as surface tension since it decides the existence of distinct boundary between the liquid and gaseous phase. It is well known that an <span class="hlt">elliptical</span> liquid jet undergoes axis-switching phenomena under atmospheric conditions due to the presence of surface tension. The experimental investigations were carried out with low speed <span class="hlt">elliptical</span> jet under supercritical condition. Investigation of the binary component system with fluoroketone jet and N{sub 2} gas as environment shows that the surface tension force dominates for a large downstream distance, indicating delayed thermodynamic transition. The increase in pressure to critical state at supercritical temperature is found to expedite the thermodynamic transition. The ligament like structures has been observed rather than droplets for supercritical pressures. However, for the single component system with fluoroketone jet and fluoroketone environment shows that the jet disintegrates into droplets as it is subjected to the chamber conditions even for the subcritical pressures and no axis switching phenomenon is observed. For a single component system, as the pressure is increased to critical state, the liquid jet exhibits gas-gas like mixing behavior and that too without exhibiting axis-switching behavior.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2015AcAau.111...37H','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2015AcAau.111...37H"><span id="translatedtitle">Optimal Lorentz-augmented spacecraft formation flying in <span class="hlt">elliptic</span> orbits</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Huang, Xu; Yan, Ye; Zhou, Yang</p> <p>2015-06-01</p> <p>An electrostatically charged spacecraft accelerates as it moves through the Earth's magnetic field due to the induced Lorentz force, providing a new means of propellantless electromagnetic propulsion for orbital maneuvers. The feasibility of Lorentz-augmented spacecraft formation flying in <span class="hlt">elliptic</span> orbits is investigated in this paper. Assuming the Earth's magnetic field as a tilted dipole corotating with Earth, a nonlinear dynamical model that characterizes the orbital motion of Lorentz spacecraft in the vicinity of arbitrary <span class="hlt">elliptic</span> orbits is developed. To establish a predetermined formation configuration at given terminal time, pseudospectral method is used to solve the optimal open-loop trajectories of hybrid control inputs consisted of Lorentz acceleration and thruster-generated control acceleration. A nontilted dipole model is also introduced to analyze the effect of dipole tilt angle via comparisons with the tilted one. Meanwhile, to guarantee finite-time convergence and system robustness against external perturbations, a continuous fast nonsingular terminal sliding mode controller is designed and the closed-loop system stability is proved by Lyapunov theory. Numerical simulations substantiate the validity of proposed open-loop and closed-loop control schemes, and the results indicate that an almost propellantless formation establishment can be achieved by choosing appropriate objective function in the pseudospectral method. Furthermore, compared to the nonsingular terminal sliding mode controller, the closed-loop controller presents superior convergence rate with only a bit more control effort. And the proposed controller can be applied in other Lorentz-augmented relative orbital control problems.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/22382174','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/22382174"><span id="translatedtitle">A heterogeneous stochastic FEM framework for <span class="hlt">elliptic</span> PDEs</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Hou, Thomas Y. Liu, Pengfei</p> <p>2015-01-15</p> <p>We introduce a new concept of sparsity for the stochastic <span class="hlt">elliptic</span> operator −div(a(x,ω)∇(⋅)), which reflects the compactness of its inverse operator in the stochastic direction and allows for spatially heterogeneous stochastic structure. This new concept of sparsity motivates a heterogeneous stochastic finite element method (HSFEM) framework for linear <span class="hlt">elliptic</span> equations, which discretizes the equations using the heterogeneous coupling of spatial basis with local stochastic basis to exploit the local stochastic structure of the solution space. We also provide a sampling method to construct the local stochastic basis for this framework using the randomized range finding techniques. The resulting HSFEM involves two stages and suits the multi-query setting: in the offline stage, the local stochastic structure of the solution space is identified; in the online stage, the equation can be efficiently solved for multiple forcing functions. An online error estimation and correction procedure through Monte Carlo sampling is given. Numerical results for several problems with high dimensional stochastic input are presented to demonstrate the efficiency of the HSFEM in the online stage.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/20350851','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/20350851"><span id="translatedtitle">Fast space-variant <span class="hlt">elliptical</span> filtering using box splines.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Chaudhury, Kunal Narayan; Munoz-Barrutia, Arrate; Unser, Michael</p> <p>2010-09-01</p> <p>The efficient realization of linear space-variant (non-convolution) filters is a challenging computational problem in image processing. In this paper, we demonstrate that it is possible to filter an image with a Gaussian-like <span class="hlt">elliptic</span> window of varying size, elongation and orientation using a fixed number of computations per pixel. The associated algorithm, which is based upon a family of smooth compactly supported piecewise polynomials, the radially-uniform box splines, is realized using preintegration and local finite-differences. The radially-uniform box splines are constructed through the repeated convolution of a fixed number of box distributions, which have been suitably scaled and distributed radially in an uniform fashion. The attractive features of these box splines are their asymptotic behavior, their simple covariance structure, and their quasi-separability. They converge to Gaussians with the increase of their order, and are used to approximate anisotropic Gaussians of varying covariance simply by controlling the scales of the constituent box distributions. Based upon the second feature, we develop a technique for continuously controlling the size, elongation and orientation of these Gaussian-like functions. Finally, the quasi-separable structure, along with a certain scaling property of box distributions, is used to efficiently realize the associated space-variant <span class="hlt">elliptical</span> filtering, which requires O(1) computations per pixel irrespective of the shape and size of the filter.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016EPJA...52..247B','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016EPJA...52..247B"><span id="translatedtitle"><span class="hlt">Elliptic</span> flow in heavy-ion collisions at NICA energies</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>B. Ivanov, Yu.; Soldatov, A. A.</p> <p>2016-08-01</p> <p>The transverse-momentum-integrated <span class="hlt">elliptic</span> flow of charged particles at midrapidity, v2 (charged), and that of identified hadrons from Au+Au collisions are analyzed in the range of incident energies relevant to the Nuclotron-based Ion Collider Facility (NICA). Simulations are performed within a three-fluid model employing three different equations of state (EoSs): a purely hadronic EoS and two versions of the EoS involving the deconfinement transition-a first-order phase transition and a smooth crossover one. The present simulations demonstrate low sensitivity of v2 (charged) to the EoS. All considered scenarios equally well reproduce recent STAR data on v2 (charged) for mid-central Au+Au collisions and properly describe its change of sign at the incident energy decrease below √{s_{NN}} ≈ 3.5 GeV. The predicted integrated <span class="hlt">elliptic</span> flow of various species exhibits a stronger dependence on the EoS. A noticeable sensitivity to the EoS is found for anti-protons and, to a lesser extent, for K- mesons. Presently there are no experimental data that could verify these predictions. Future experiments at NICA could corroborate these findings.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2014JHEP...10..062B','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2014JHEP...10..062B"><span id="translatedtitle">The superconformal index and an <span class="hlt">elliptic</span> algebra of surface defects</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Bullimore, Mathew; Fluder, Martin; Hollands, Lotte; Richmond, Paul</p> <p>2014-10-01</p> <p>In this paper we continue the study of the superconformal index of four-dimensional =2 theories of class in the presence of surface defects. Our main result is the construction of an algebra of difference operators, whose elements are labeled by irreducible representations of A N -1. For the fully antisymmetric tensor representations these difference operators are the Hamiltonians of the <span class="hlt">elliptic</span> Ruijsenaars-Schneider system. The structure constants of the algebra are <span class="hlt">elliptic</span> generalizations of the Littlewood-Richardson coefficients. In the Macdonald limit, we identify the difference operators with local operators in the two-dimensional TQFT interpretation of the superconformal index. We also study the dimensional reduction to difference operators acting on the three-sphere partition function, where they characterize supersymmetric defects supported on a circle, and show that they are transformed to supersymmetric Wilson loops under mirror symmetry. Finally, we compare to the difference operators that create 't Hooft loops in the four-dimensional =2* theory on a four-sphere by embedding the three-dimensional theory as an S-duality domain wall.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/15783761','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/15783761"><span id="translatedtitle"><span class="hlt">Intrinsic</span> spin and orbital angular momentum Hall effect.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Zhang, S; Yang, Z</p> <p>2005-02-18</p> <p>A generalized definition of <span class="hlt">intrinsic</span> and extrinsic transport coefficients is introduced. We show that transport coefficients from the <span class="hlt">intrinsic</span> origin are solely determined by local electronic structure, and thus the <span class="hlt">intrinsic</span> spin Hall effect is not a transport phenomenon. The <span class="hlt">intrinsic</span> spin Hall current is always accompanied by an equal but opposite <span class="hlt">intrinsic</span> orbital angular momentum Hall current. We prove that the <span class="hlt">intrinsic</span> spin Hall effect does not induce a spin accumulation at the edge of the sample or near the interface.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2015ApJ...806..225P','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2015ApJ...806..225P"><span id="translatedtitle">On the <span class="hlt">Intrinsic</span> Diversity of Type II-Plateau Supernovae</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Pejcha, Ondřej; Prieto, Jose L.</p> <p>2015-06-01</p> <p>Hydrogen-rich Type II-Plateau supernovae (SNe) exhibit <span class="hlt">correlations</span> between the plateau luminosity {L}{pl}, the nickel mass {M}{Ni}, the explosion energy {E}{exp}, and the ejecta mass {M}{ej}. Using our global, self-consistent, multi-band model of nearby well-observed SNe, we find that the covariances of these quantities are strong and that the confidence ellipsoids are oriented in the direction of the <span class="hlt">correlations</span>, which reduces their significance. By proper treatment of the covariance matrix of the model, we discover a significant <span class="hlt">intrinsic</span> width to the <span class="hlt">correlations</span> between {L}{pl}, {E}{exp} and {M}{Ni}, where the uncertainties due to the distance and the extinction dominate. For fixed {E}{exp}, the spread in {M}{Ni} is about 0.25 dex, which we attribute to the differences in the progenitor internal structure. We argue that the effects of incomplete γ-ray trapping are not important in our sample. Similarly, the physics of the Type II-Plateau SN light curves leads to inherently degenerate estimates of {E}{exp} and {M}{ej}, which makes their observed <span class="hlt">correlation</span> weak. Ignoring the covariances of SN parameters or the <span class="hlt">intrinsic</span> width of the <span class="hlt">correlations</span> causes significant biases in the slopes of the fitted relations. Our results imply that Type II-Plateau SN explosions are not described by a single physical parameter or a simple one-dimensional trajectory through the parameter space, but instead reflect the diversity of the core and surface properties of their progenitors. We discuss the implications for the physics of the explosion mechanism and possible future observational constraints.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://www.osti.gov/scitech/servlets/purl/877207','SCIGOV-STC'); return false;" href="http://www.osti.gov/scitech/servlets/purl/877207"><span id="translatedtitle">The Relation Between Accretion Rate And Jet Power in X-Ray Luminous <span class="hlt">Elliptical</span> Galaxies</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Allen, Steven W.; Dunn, R.J.H.; Fabian, A.C.; Taylor, G.B.; Reynolds, C.S.; /Maryland U.</p> <p>2006-03-10</p> <p>Using Chandra X-ray observations of nine nearby, X-ray luminous <span class="hlt">elliptical</span> galaxies with good optical velocity dispersion measurements, we show that a tight <span class="hlt">correlation</span> exists between the Bondi accretion rates calculated from the observed gas temperature and density profiles and estimated black hole masses, and the power emerging from these systems in relativistic jets. The jet powers, which are inferred from the energies and timescales required to inflate cavities observed in the surrounding X-ray emitting gas, can be related to the accretion rates using a power law model of the form log (P{sub Bondi}/10{sup 43} erg s{sup -1}) = A + B log (P{sub jet}/10{sup 43} erg s{sup -1}), with A = 0.62 {+-} 0.15 and B = 0.77 {+-} 0.18. Our results show that a significant fraction of the energy associated with the rest mass of material entering the Bondi accretion radius (2.4{sub -0.7}{sup +1.0} per cent, for P{sub jet} = 10{sup 43} erg s{sup -1}) eventually emerges in the relativistic jets. Our results have significant implications for studies of accretion, jet formation and galaxy formation. The observed tight <span class="hlt">correlation</span> suggests that the Bondi formulae provide a reasonable description of the accretion process in these systems, despite the likely presence of magnetic pressure and angular momentum in the accreting gas. The similarity of the P{sub Bondi} and P{sub jet} values argues that a significant fraction of the matter entering the accretion radius flows down to regions close to the black holes, where the jets are presumably formed. The tight <span class="hlt">correlation</span> between P{sub Bondi} and P{sub jet} also suggests that the accretion flows are approximately stable over timescales of a few million years. Our results show that the black hole ''engines'' at the hearts of large <span class="hlt">elliptical</span> galaxies and groups feed back sufficient energy to stem cooling and star formation, leading naturally to the observed exponential cut off at the bright end of the galaxy luminosity function.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/26403968','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/26403968"><span id="translatedtitle"><span class="hlt">Intrinsic</span> and extrinsic mechanical properties related to the differentiation of mesenchymal stem cells.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Lee, Jin-Ho; Park, Hun-Kuk; Kim, Kyung Sook</p> <p>2016-05-06</p> <p>Diverse <span class="hlt">intrinsic</span> and extrinsic mechanical factors have a strong influence on the regulation of stem cell fate. In this work, we examined recent literature on the effects of mechanical environments on stem cells, especially on differentiation of mesenchymal stem cells (MSCs). We provide a brief review of <span class="hlt">intrinsic</span> mechanical properties of single MSC and examined the <span class="hlt">correlation</span> between the <span class="hlt">intrinsic</span> mechanical property of MSC and the differentiation ability. The effects of extrinsic mechanical factors relevant to the differentiation of MSCs were considered separately. The effect of nanostructure and elasticity of the matrix on the differentiation of MSCs were summarized. Finally, we consider how the extrinsic mechanical properties transfer to MSCs and then how the effects on the <span class="hlt">intrinsic</span> mechanical properties affect stem cell differentiation.</p> </li> </ol> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_20");'>20</a></li> <li><a href="#" onclick='return showDiv("page_21");'>21</a></li> <li class="active"><span>22</span></li> <li><a href="#" onclick='return showDiv("page_23");'>23</a></li> <li><a href="#" onclick='return showDiv("page_24");'>24</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div><!-- col-sm-12 --> </div><!-- row --> </div><!-- page_22 --> <div id="page_23" class="hiddenDiv"> <div class="row"> <div class="col-sm-12"> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_21");'>21</a></li> <li><a href="#" onclick='return showDiv("page_22");'>22</a></li> <li class="active"><span>23</span></li> <li><a href="#" onclick='return showDiv("page_24");'>24</a></li> <li><a href="#" onclick='return showDiv("page_25");'>25</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div> </div> <div class="row"> <div class="col-sm-12"> <ol class="result-class" start="441"> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/18826542','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/18826542"><span id="translatedtitle">Longitudinal analysis of <span class="hlt">intrinsic</span> motivation and competence beliefs: is there a relation over time?</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Spinath, Birgit; Steinmayr, Ricarda</p> <p>2008-01-01</p> <p>The present study explored whether competence beliefs and <span class="hlt">intrinsic</span> motivation for different school domains show reciprocal effects over time. A sample of 670 German elementary school pupils (M= 8.8 years, SD= 0.51) was followed over 1 year. At 4 measurement occasions, children completed self-reports on their <span class="hlt">intrinsic</span> motivation and competence beliefs for math, German, and school in general. Latent growth models revealed that <span class="hlt">intrinsic</span> motivation and competence beliefs decreased over time. Comparing <span class="hlt">correlational</span> and cross-lagged structural equation models yielded only weak evidence for cross-lagged influences between the 2 constructs. Results suggest that the developmental curves of competence beliefs and <span class="hlt">intrinsic</span> motivation might be less inextricably interwoven than frequently assumed.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/22068802','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/22068802"><span id="translatedtitle">Time growth rate and field profiles of hybrid modes excited by a relativistic <span class="hlt">elliptical</span> electron beam in an <span class="hlt">elliptical</span> metallic waveguide with dielectric rod</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Jazi, B.; Rahmani, Z.; Abdoli-Arani, A.; Heidari-Semiromi, E.</p> <p>2012-10-15</p> <p>The dispersion relation of guided electromagnetic waves propagating in an <span class="hlt">elliptical</span> metallic waveguide with a dielectric rod driven by relativistic <span class="hlt">elliptical</span> electron beam (REEB) is investigated. The electric field profiles and the growth rates of the waves are numerically calculated by using Mathieu functions. The effects of relative permittivity constant of dielectric rod, accelerating voltage, and current density of REEB on the growth rate are presented.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/20020074874','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/20020074874"><span id="translatedtitle">Lateral Migration and Rotational Motion of <span class="hlt">Elliptic</span> Particles in Planar Poiseuille Flow</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Qi, Dewei; Luo, Li-Shi; Aravamuthan, Raja; Strieder, William; Bushnell, Dennis M. (Technical Monitor)</p> <p>2002-01-01</p> <p>Simulations of <span class="hlt">elliptic</span> particulate suspensions in the planar Poiseuille flow are performed by using the lattice Boltzmann equation. Effects of the multi-particle on the lateral migration and rotational motion of both neutrally and non-neutrally buoyant <span class="hlt">elliptic</span> particles are investigated. Low and intermediate total particle volume fraction f(sub a) = 13%, 15%, and 40% are considered in this work.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/20010062806','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/20010062806"><span id="translatedtitle">Some Improvements on Signed Window Algorithms for Scalar Multiplications in <span class="hlt">Elliptic</span> Curve Cryptosystems</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Vo, San C.; Biegel, Bryan (Technical Monitor)</p> <p>2001-01-01</p> <p>Scalar multiplication is an essential operation in <span class="hlt">elliptic</span> curve cryptosystems because its implementation determines the speed and the memory storage requirements. This paper discusses some improvements on two popular signed window algorithms for implementing scalar multiplications of an <span class="hlt">elliptic</span> curve point - Morain-Olivos's algorithm and Koyarna-Tsuruoka's algorithm.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017JMP....58c3504S','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017JMP....58c3504S"><span id="translatedtitle">The Sylvester equation and the <span class="hlt">elliptic</span> Korteweg-de Vries system</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Sun, Ying-ying; Zhang, Da-jun; Nijhoff, Frank W.</p> <p>2017-03-01</p> <p>The <span class="hlt">elliptic</span> potential Korteweg-de Vries lattice system is a multi-component extension of the lattice potential Korteweg-de Vries equation, whose soliton solutions are associated with an <span class="hlt">elliptic</span> Cauchy kernel (i.e., a Cauchy kernel on the torus). In this paper we generalize the class of solutions by allowing the spectral parameter to be a full matrix obeying a matrix version of the equation of the <span class="hlt">elliptic</span> curve, and for the Cauchy matrix to be a solution of a Sylvester type matrix equation subject to this matrix <span class="hlt">elliptic</span> curve equation. The construction involves solving the matrix <span class="hlt">elliptic</span> curve equation by using Toeplitz matrix techniques, and analysing the solution of the Sylvester equation in terms of Jordan normal forms. Furthermore, we consider the continuum limit system associated with the <span class="hlt">elliptic</span> potential Korteweg-de Vries system, and analyse the dynamics of the soliton solutions, which reveals some new features of the <span class="hlt">elliptic</span> system in comparison to the non-<span class="hlt">elliptic</span> case.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016ApJ...820...69S','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016ApJ...820...69S"><span id="translatedtitle">The Next Generation Virgo Cluster Survey. VII. The <span class="hlt">Intrinsic</span> Shapes of Low-luminosity Galaxies in the Core of the Virgo Cluster, and a Comparison with the Local Group</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Sánchez-Janssen, Rubén; Ferrarese, Laura; MacArthur, Lauren A.; Côté, Patrick; Blakeslee, John P.; Cuillandre, Jean-Charles; Duc, Pierre-Alain; Durrell, Patrick; Gwyn, Stephen; McConnacchie, Alan W.; Boselli, Alessandro; Courteau, Stéphane; Emsellem, Eric; Mei, Simona; Peng, Eric; Puzia, Thomas H.; Roediger, Joel; Simard, Luc; Boyer, Fred; Santos, Matthew</p> <p>2016-03-01</p> <p>We investigate the <span class="hlt">intrinsic</span> shapes of low-luminosity galaxies in the central 300 kpc of the Virgo Cluster using deep imaging obtained as part of the Next Generation Virgo Cluster Survey (NGVS). We build a sample of nearly 300 red-sequence cluster members in the yet-unexplored -14 < Mg < -8 mag range, and we measure their apparent axis ratios, q, through Sérsic fits to their two-dimensional light distribution, which is well described by a constant <span class="hlt">ellipticity</span> parameter. The resulting distribution of apparent axis ratios is then fit by families of triaxial models with normally distributed <span class="hlt">intrinsic</span> <span class="hlt">ellipticities</span>, E = 1 - C/A, and triaxialities, T = (A2 - B2)/(A2 - C2). We develop a Bayesian framework to explore the posterior distribution of the model parameters, which allows us to work directly on discrete data, and to account for individual, surface-brightness-dependent axis ratio uncertainties. For this population we infer a mean <span class="hlt">intrinsic</span> <span class="hlt">ellipticity</span> \\bar{E} = {0.43}-0.02+0.02 and a mean triaxiality \\bar{T} = {0.16}-0.06+0.07. This implies that faint Virgo galaxies are best described as a family of thick, nearly oblate spheroids with mean <span class="hlt">intrinsic</span> axis ratios 1:0.94:0.57. The core of Virgo lacks highly elongated low-luminosity galaxies, with 95% of the population having q > 0.45. We additionally attempt a study of the <span class="hlt">intrinsic</span> shapes of Local Group (LG) satellites of similar luminosities. For the LG population we infer a slightly larger mean <span class="hlt">intrinsic</span> <span class="hlt">ellipticity</span> \\bar{E} = {0.51}-0.06+0.07, and the paucity of objects with round apparent shapes translates into more triaxial mean shapes, 1:0.76:0.49. Numerical studies that follow the tidal evolution of satellites within LG-sized halos are in good agreement with the inferred shape distributions, but the mismatch for faint galaxies in Virgo highlights the need for more adequate simulations of this population in the cluster environment. We finally compare the <span class="hlt">intrinsic</span> shapes of NGVS low-mass galaxies with</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2015CeMDA.123..279P','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2015CeMDA.123..279P"><span id="translatedtitle">Stability of two groups of multi-revolution <span class="hlt">elliptic</span> halo orbits in the <span class="hlt">elliptic</span> restricted three-body problem</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Peng, Hao; Xu, Shijie</p> <p>2015-11-01</p> <p>The multi-revolution <span class="hlt">elliptic</span> halo (ME-Halo) orbit is a kind of strictly periodic orbit existing in the <span class="hlt">elliptic</span> restricted three-body problem (ERTBP) model. Its remarkable features include that it survives the eccentricity perturbation of the primaries, it has a long period commeasurable with the primary period and that its stability property varies greatly as the eccentricity. The authors utilized continuation methods together with the multi-segment optimization method to generate two groups of ME-Halo orbits, and then systematically investigated their stability evolution with respect to the eccentricity and the mass ratio of the primaries. These parameters show complicate impacts on the stability. Some ME-Halo orbits can possess more than one pairs of real eigenvalue, some have negative real eigenvalues or complex eigenvalues out of the unit circle. For certain parameters, continuation failures are observed to be accompanied by a series of eigenvalue collision and bifurcations. The results in this paper can help to understand the nonautonomous dynamic of the ERTBP and can further aid in understanding the dynamical environment for real-world applications and, thus, contribute to the trajectory development process.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016MNRAS.461.2115D','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016MNRAS.461.2115D"><span id="translatedtitle">Is the cluster environment quenching the Seyfert activity in <span class="hlt">elliptical</span> and spiral galaxies?</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>de Souza, R. S.; Dantas, M. L. L.; Krone-Martins, A.; Cameron, E.; Coelho, P.; Hattab, M. W.; de Val-Borro, M.; Hilbe, J. M.; Elliott, J.; Hagen, A.; COIN Collaboration</p> <p>2016-09-01</p> <p>We developed a hierarchical Bayesian model (HBM) to investigate how the presence of Seyfert activity relates to their environment, herein represented by the galaxy cluster mass, M200, and the normalized cluster centric distance, r/r200. We achieved this by constructing an unbiased sample of galaxies from the Sloan Digital Sky Survey, with morphological classifications provided by the Galaxy Zoo Project. A propensity score matching approach is introduced to control the effects of confounding variables: stellar mass, galaxy colour, and star formation rate. The connection between Seyfert-activity and environmental properties in the de-biased sample is modelled within an HBM framework using the so-called logistic regression technique, suitable for the analysis of binary data (e.g. whether or not a galaxy hosts an AGN). Unlike standard ordinary least square fitting methods, our methodology naturally allows modelling the probability of Seyfert-AGN activity in galaxies on their natural scale, i.e. as a binary variable. Furthermore, we demonstrate how an HBM can incorporate information of each particular galaxy morphological type in an unified framework. In <span class="hlt">elliptical</span> galaxies our analysis indicates a strong <span class="hlt">correlation</span> of Seyfert-AGN activity with r/r200, and a weaker <span class="hlt">correlation</span> with the mass of the host cluster. In spiral galaxies these trends do not appear, suggesting that the link between Seyfert activity and the properties of spiral galaxies are independent of the environment.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/22308562','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/22308562"><span id="translatedtitle"><span class="hlt">Intrinsic</span> delay of permeable base transistor</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Chen, Wenchao; Guo, Jing; So, Franky</p> <p>2014-07-28</p> <p>Permeable base transistors (PBTs) fabricated by vacuum deposition or solution process have the advantages of easy fabrication and low power operation and are a promising device structure for flexible electronics. <span class="hlt">Intrinsic</span> delay of PBT, which characterizes the speed of the transistor, is investigated by solving the three-dimensional Poisson equation and drift-diffusion equation self-consistently using finite element method. Decreasing the emitter thickness lowers the <span class="hlt">intrinsic</span> delay by improving on-current, and a thinner base is also preferred for low <span class="hlt">intrinsic</span> delay because of fewer carriers in the base region at off-state. The <span class="hlt">intrinsic</span> delay exponentially decreases as the emitter contact Schottky barrier height decreases, and it linearly depends on the carrier mobility. With an optimized emitter contact barrier height and device geometry, a sub-nano-second <span class="hlt">intrinsic</span> delay can be achieved with a carrier mobility of ∼10 cm{sup 2}/V/s obtainable in solution processed indium gallium zinc oxide, which indicates the potential of solution processed PBTs for GHz operations.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/12434838','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/12434838"><span id="translatedtitle"><span class="hlt">Intrinsic</span>-extrinsic factors in sport motivation.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Pedersen, Darhl M</p> <p>2002-10-01</p> <p>Participants were 83 students (36 men and 47 women). 10 <span class="hlt">intrinsic</span>-extrinsic factors involved in sport motivation were obtained. The factors were generated from items obtained from the participants rather than items from the experimenter. This was done to avoid the possible influence of preconceptions on the part of the experimenter regarding what the final dimensions may be. Obtained motivational factors were Social Reinforcement, Fringe Benefits, Fame and Fortune, External Forces, Proving Oneself, Social Benefits, Mental Enrichment, Expression of Self, Sense of Accomplishment, and Self-enhancement. Each factor was referred to an <span class="hlt">intrinsic</span>-extrinsic dimension to describe its relative position on that dimension. The order of the factors as listed indicates increasing <span class="hlt">intrinsic</span> motivation. i.e., the first four factors were rated in the extrinsic range, whereas the remaining six were rated to be in the <span class="hlt">intrinsic</span> range. Next, the participants rated the extent to which each of the various factors was involved in their decision to participate in sport activities. The pattern of use of the motivational factors was the same for both sexes except that men indicated greater use of the Fringe Benefits factor. Overall, the more <span class="hlt">intrinsic</span> a sport motivation factor was rated, the more likely it was to be rated as a factor in actual sport participation.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/22356506','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/22356506"><span id="translatedtitle">The Carnegie Supernova Project: <span class="hlt">Intrinsic</span> colors of type Ia supernovae</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Burns, Christopher R.; Persson, S. E.; Freedman, Wendy L.; Madore, Barry F.; Stritzinger, Maximilian; Contreras, Carlos; Phillips, M. M.; Hsiao, E. Y.; Boldt, Luis; Campillay, Abdo; Castellón, Sergio; Morrell, Nidia; Salgado, Francisco; Folatelli, Gaston; Suntzeff, Nicholas B.</p> <p>2014-07-01</p> <p>We present an updated analysis of the <span class="hlt">intrinsic</span> colors of Type Ia supernova (SNe Ia) using the latest data release of the Carnegie Supernova Project. We introduce a new light-curve parameter very similar to stretch that is better suited for fast-declining events, and find that these peculiar types can be seen as extensions to the population of 'normal' SNe Ia. With a larger number of objects, an updated fit to the Lira relation is presented along with evidence for a dependence on the late-time slope of the B – V light-curves with stretch and color. Using the full wavelength range from u to H band, we place constraints on the reddening law for the sample as a whole and also for individual events/hosts based solely on the observed colors. The photometric data continue to favor low values of R{sub V} , though with large variations from event to event, indicating an <span class="hlt">intrinsic</span> distribution. We confirm the findings of other groups that there appears to be a <span class="hlt">correlation</span> between the derived reddening law, R{sub V} , and the color excess, E(B – V), such that larger E(B – V) tends to favor lower R{sub V} . The <span class="hlt">intrinsic</span> u-band colors show a relatively large scatter that cannot be explained by variations in R{sub V} or by the Goobar power-law for circumstellar dust, but rather is <span class="hlt">correlated</span> with spectroscopic features of the supernova and is therefore likely due to metallicity effects.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19950045440&hterms=globular&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D60%26Ntt%3Dglobular','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19950045440&hterms=globular&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D60%26Ntt%3Dglobular"><span id="translatedtitle">The richness of the globular cluster system of NGC 3923: Clues to <span class="hlt">elliptical</span> galaxy formation</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Zepf, Stephen E.; Geisler, Doug; Ashman, Keith M.</p> <p>1994-01-01</p> <p>We present new data on the globular cluster system of the <span class="hlt">elliptical</span> galaxy NGC 3923 which show that it has the most globular clusters per unit luminosity of any noncluster <span class="hlt">elliptical</span> yet observed, with S(sub N) = 6.4 +/- 1.4. NGC 3923 is also among the brightest <span class="hlt">ellipticals</span> outside of a galaxy cluster for which the number of globular clusters has been determined. Our observation of a large number of clusters per unit luminosity (high S(sub N)-value) for a bright <span class="hlt">elliptical</span> in a sparse environment is consistent with the suggestion of Djorgovski and Santiago that the number of globular clusters is a power-law function of the luminosity with an exponent greater than 1. We relate this higher specific frequency of globular clusters in more luminous galaxies to other observations which indicate that the physical conditions within <span class="hlt">elliptical</span> galaxies at the time of their formation were dependent on galaxy mass.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017PhRvA..95c1404S','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017PhRvA..95c1404S"><span id="translatedtitle">Fully differential study on dissociative ionization dynamics of deuteron molecules in strong <span class="hlt">elliptical</span> laser fields</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Shao, Yun; He, Peilun; Liu, Ming-Ming; Sun, Xufei; Li, Min; Deng, Yongkai; Wu, Chengyin; He, Feng; Gong, Qihuang; Liu, Yunquan</p> <p>2017-03-01</p> <p>Deuteron momentum distributions from the dissociative ionization of D2 in intense <span class="hlt">elliptically</span> polarized laser fields have been explored in a joint experimental and numerical study. The asymmetrical charge localization in the dissociative D2 + offers a large torque, and thus an <span class="hlt">elliptically</span> polarized laser field efficiently rotates the molecular ion during its dissociation, resulting in the emission of deuterons finally deviating from the bond direction at the instant of tunneling ionization of D2. The rotating torque of the molecular ions increases with the field <span class="hlt">ellipticity</span>, leading to an <span class="hlt">ellipticity</span>-dependent tilt angle for the deuteron momentum distribution. Due to the notable rotation of D2 + during its dissociation, the photoelectron angular distributions in the laboratory frame and the molecular frame are distinct, which illustrates that the axial recoil approximation is broken for discussing the photoelectron angular distributions of molecules in <span class="hlt">elliptically</span> polarized laser fields.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/23871744','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/23871744"><span id="translatedtitle">Learning to learn - <span class="hlt">intrinsic</span> plasticity as a metaplasticity mechanism for memory formation.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Sehgal, Megha; Song, Chenghui; Ehlers, Vanessa L; Moyer, James R</p> <p>2013-10-01</p> <p>"Use it or lose it" is a popular adage often associated with use-dependent enhancement of cognitive abilities. Much research has focused on understanding exactly how the brain changes as a function of experience. Such experience-dependent plasticity involves both structural and functional alterations that contribute to adaptive behaviors, such as learning and memory, as well as maladaptive behaviors, including anxiety disorders, phobias, and posttraumatic stress disorder. With the advancing age of our population, understanding how use-dependent plasticity changes across the lifespan may also help to promote healthy brain aging. A common misconception is that such experience-dependent plasticity (e.g., associative learning) is synonymous with synaptic plasticity. Other forms of plasticity also play a critical role in shaping adaptive changes within the nervous system, including <span class="hlt">intrinsic</span> plasticity - a change in the <span class="hlt">intrinsic</span> excitability of a neuron. <span class="hlt">Intrinsic</span> plasticity can result from a change in the number, distribution or activity of various ion channels located throughout the neuron. Here, we review evidence that <span class="hlt">intrinsic</span> plasticity is an important and evolutionarily conserved neural <span class="hlt">correlate</span> of learning. <span class="hlt">Intrinsic</span> plasticity acts as a metaplasticity mechanism by lowering the threshold for synaptic changes. Thus, learning-related <span class="hlt">intrinsic</span> changes can facilitate future synaptic plasticity and learning. Such <span class="hlt">intrinsic</span> changes can impact the allocation of a memory trace within a brain structure, and when compromised, can contribute to cognitive decline during the aging process. This unique role of <span class="hlt">intrinsic</span> excitability can provide insight into how memories are formed and, more interestingly, how neurons that participate in a memory trace are selected. Most importantly, modulation of <span class="hlt">intrinsic</span> excitability can allow for regulation of learning ability - this can prevent or provide treatment for cognitive decline not only in patients with clinical disorders but</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/18004752','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/18004752"><span id="translatedtitle"><span class="hlt">Intrinsically</span> disordered protein from a pathogenic mesophile Mycobacterium tuberculosis adopts structured conformation at high temperature.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Kumar, Niti; Shukla, Swati; Kumar, Sanjiv; Suryawanshi, Anju; Chaudhry, Uma; Ramachandran, Srinivasan; Maiti, Souvik</p> <p>2008-05-15</p> <p>Compared to eukaryotes, the occurrence of "<span class="hlt">intrinsically</span> disordered" or "natively unfolded" proteins in prokaryotes has not been explored extensively. Here, we report the occurrence of an <span class="hlt">intrinsically</span> disordered protein from the mesophilic human pathogen Mycobacterium tuberculosis. The Histidine-tagged recombinant Rv3221c biotin-binding protein is <span class="hlt">intrinsically</span> disordered at ambient and physiological growth temperatures as revealed by circular dichroism and Fourier transform infrared (FTIR) spectroscopic studies. However, an increase in temperature induces a transition from disordered to structured state with a folding temperature of approximately 53 degrees C. Addition of a structure inducing solvent trifluoroethanol (TFE) causes the protein to fold at lower temperatures suggesting that TFE fosters hydrophobic interactions, which drives protein folding. Differential Scanning Calorimetry studies revealed that folding is endothermic and the transition from a disordered to structured state is continuous (higher-order), implying existence of intermediates during folding process. Secondary structure analysis revealed that the protein has propensity to form beta-sheets. This is in conformity with FTIR spectrum that showed an absorption peak at wave number of 1636 cm(-1), indicative of disordered beta-sheet conformation in the native state. These data suggest that although Rv3221c may be disordered under ambient or optimal growth temperature conditions, it has the potential to fold into ordered structure at high temperature driven by increased hydrophobic interactions. In contrast to the generally known behavior of other <span class="hlt">intrinsically</span> disordered proteins folding at high temperature, Rv3221c does not appear to oligomerize or aggregate as revealed through numerous experiments including Congo red binding, Thioflavin T-binding, turbidity measurements, and examining molar <span class="hlt">ellipticity</span> as a function of protein concentration. The amino acid composition of Rv3221c reveals that</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2015A%26A...574A..93L','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2015A%26A...574A..93L"><span id="translatedtitle">Dark matter deprivation in the field <span class="hlt">elliptical</span> galaxy NGC 7507</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Lane, Richard R.; Salinas, Ricardo; Richtler, Tom</p> <p>2015-02-01</p> <p>Context. Previous studies have shown that the kinematics of the field <span class="hlt">elliptical</span> galaxy NGC 7507 do not necessarily require dark matter. This is troubling because, in the context of ΛCDM cosmologies, all galaxies should have a large dark matter component. Aims: Our aims are to determine the rotation and velocity dispersion profile out to larger radii than do previous studies, and, therefore, more accurately estimate of the dark matter content of the galaxy. Methods: We use penalised pixel-fitting software to extract velocities and velocity dispersions from GMOS slit mask spectra. Using Jeans and MONDian modelling, we then produce models with the goal of fitting the velocity dispersion data. Results: NGC 7507 has a two-component stellar halo, with the outer halo counter rotating with respect to the inner halo, with a kinematic boundary at a radius of ~110'' (~12.4 kpc). The velocity dispersion profile exhibits an increase at ~70'' (~7.9 kpc), reminiscent of several other <span class="hlt">elliptical</span> galaxies. Our best fit models are those under mild anisotropy, which include ~100 times less dark matter than predicted by ΛCDM, although mildly anisotropic models that are completely dark matter free fit the measured dynamics almost equally well. Our MONDian models, both isotropic and anisotropic, systematically fail to reproduce the measured velocity dispersions at almost all radii. Conclusions: The counter-rotating outer halo implies a merger remnant, as does the increase in velocity dispersion at ~70''. From simulations it seems plausible that the merger that caused the increase in velocity dispersion was a spiral-spiral merger. Our Jeans models are completely consistent with a no dark matter scenario, however, some dark matter can be accommodated, although at much lower concentrations than predicted by ΛCDM simulations. This indicates that NGC 7507 may be a dark matter free <span class="hlt">elliptical</span> galaxy. Regardless of whether NGC 7507 is completely dark matter free or very dark matter poor</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/1990RMxAA..21...89A','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/1990RMxAA..21...89A"><span id="translatedtitle">Violent Relaxation, Dynamical Instabilities and the Formation of <span class="hlt">Elliptical</span> Galaxies</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Aguilar, L. A.</p> <p>1990-11-01</p> <p>RESUMEN: El problema de la formaci6n de galaxias elfpticas por medjo de colapso gravitacional sin disipaci6n de energfa es estudiado usando un gran numero de simulaciones numericas. Se muestra que este tipo de colapsos, partiendo de condiciones iniciales frfas donde la energfa cinetica inicial representa s6lo un 5%, 0 , de a potencial inicial, produce sistemas relajados de forma triaxial muy similares a las galaxias elfpticas reales en sus formas y perfiles de densidad en proyecci6i . La forina triaxial resulta de la acci6n de una inestabilidad dinamica que aparece en sistemas 'inicos dominados por movimientos radiales, mientras que el perfil de densidad final Cs debido al llamado relajamiento violento que tiende a producir una distribuci6n en espacio fase unica. Estos dos fen6menos tienden a borrar los detalles particulares sobre las condiciones iniciales y dan lugar a una evoluci6n convergente hacia sistemas realistas, esto innecesario el uso de condiciones iniciales especiales (excepto por Ia condici6i de que estas deben ser frfas). Las condiciones iniciales frfas producen los movimientos radiales y fluctuaciones de la energfa potencial requeridos por ambos fen6menos. ABSTRACT: The problem of formation of <span class="hlt">elliptical</span> galaxies via dissipationless collapse is studied using a large set of numerical simulations. It is shown that dissipationless collapses from cold initial conditions, where the total initial kinetic energy is less than 5% ofthe initial potential energy, lead to relaxed triaxial systems ery similar to real <span class="hlt">elliptical</span> galaxies ii projected shape and density profiles. The triaxial shape is due to the of a dynamical instability that appears on systems dominated by radial orbits, while final density profile is due to violent relaxation that tends to produce a unique distribution iii space. These two phenomena erase memory of the initial prodtice a convergent evolution toward realistic systems, thus making unnecessary use o[special initial conditions (other</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/35461','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/35461"><span id="translatedtitle"><span class="hlt">Intrinsic</span> errors in several ab initio methods. The dissociation energy of N{sub 2}</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Peterson, K.A. |; Dunning, T.H. Jr.</p> <p>1995-03-23</p> <p>Using sequences of <span class="hlt">correlation</span> consistent basis sets, complete basis set (CBS) limits for the dissociation energy D{sub c} of N{sub 2} have been estimated for a variety of commonly used electron <span class="hlt">correlation</span> methods. After extrapolation to the CBS limit, the difference between theory and experiment corresponds to the error <span class="hlt">intrinsic</span> to the chosen theoretical method. <span class="hlt">Correlated</span> wave functions (valence electrons <span class="hlt">correlated</span> only) for which <span class="hlt">intrinsic</span> errors have been estimated include internally contracted multireference configuration interaction (CMRCI), singles and doubles coupled cluster theory with and without perturbative triple excitations [CCSD, CCSD(T)], and second-, third-, and fourth-order Moller-Plesset perturbation theory (MP2, MP3, MP4). For CMRCI and CCSD(T), D{sub c} converges smoothly from below the experimental value and yields the smallest <span class="hlt">intrinsic</span> errors, -0.8 and -1.6 kcal/mol, respectively. In contrast, for MP2 and MP4, D{sub c} exhibits fortuitously good agreement with experiment for small basis sets but leads to CBS limits that are 11.6 and 3.4 kcal/mol larger than experiment, respectively. <span class="hlt">Correlation</span> of the 1s core electrons is predicted to yield <span class="hlt">intrinsic</span> errors of less than 1 kcal/mol for CMRCI and CCSD(T), while those for MP2 and MP4 increase still further. 38 refs., 1 fig., 1 tab.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://eric.ed.gov/?q=Amino+AND+acids&pg=3&id=ED537535','ERIC'); return false;" href="http://eric.ed.gov/?q=Amino+AND+acids&pg=3&id=ED537535"><span id="translatedtitle">Genome-Wide Prediction of <span class="hlt">Intrinsic</span> Disorder; Sequence Alignment of <span class="hlt">Intrinsically</span> Disordered Proteins</span></a></p> <p><a target="_blank" href="http://www.eric.ed.gov/ERICWebPortal/search/extended.jsp?_pageLabel=advanced">ERIC Educational Resources Information Center</a></p> <p>Midic, Uros</p> <p>2012-01-01</p> <p><span class="hlt">Intrinsic</span> disorder (ID) is defined as a lack of stable tertiary and/or secondary structure under physiological conditions in vitro. <span class="hlt">Intrinsically</span> disordered proteins (IDPs) are highly abundant in nature. IDPs possess a number of crucial biological functions, being involved in regulation, recognition, signaling and control, e.g. their functional…</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/23375259','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/23375259"><span id="translatedtitle">Structure and <span class="hlt">intrinsic</span> disorder in protein autoinhibition.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Trudeau, Travis; Nassar, Roy; Cumberworth, Alexander; Wong, Eric T C; Woollard, Geoffrey; Gsponer, Jörg</p> <p>2013-03-05</p> <p>Autoinhibition plays a significant role in the regulation of many proteins. By analyzing autoinhibited proteins, we demonstrate that these proteins are enriched in <span class="hlt">intrinsic</span> disorder because of the properties of their inhibitory modules (IMs). A comparison of autoinhibited proteins with structured and <span class="hlt">intrinsically</span> disordered IMs revealed that in the latter group (1) multiple phosphorylation sites are highly abundant; (2) splice variants occur in greater number than in their structured cousins; and (3) activation is often associated with changes in secondary structure in the IM. Analyses of families of autoinhibited proteins revealed that the levels of disorder in IMs can vary significantly throughout homologous proteins, whereas residues located at the interfaces between the IMs and inhibited domains are conserved. Our findings suggest that <span class="hlt">intrinsically</span> disordered IMs provide advantages over structured ones that are likely to be exploited in the fine-tuning of the equilibrium between active and inactive states of autoinhibited proteins.</p> </li> </ol> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_21");'>21</a></li> <li><a href="#" onclick='return showDiv("page_22");'>22</a></li> <li class="active"><span>23</span></li> <li><a href="#" onclick='return showDiv("page_24");'>24</a></li> <li><a href="#" onclick='return showDiv("page_25");'>25</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div><!-- col-sm-12 --> </div><!-- row --> </div><!-- page_23 --> <div id="page_24" class="hiddenDiv"> <div class="row"> <div class="col-sm-12"> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_21");'>21</a></li> <li><a href="#" onclick='return showDiv("page_22");'>22</a></li> <li><a href="#" onclick='return showDiv("page_23");'>23</a></li> <li class="active"><span>24</span></li> <li><a href="#" onclick='return showDiv("page_25");'>25</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div> </div> <div class="row"> <div class="col-sm-12"> <ol class="result-class" start="461"> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2002MNRAS.335..517V','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2002MNRAS.335..517V"><span id="translatedtitle">A SAURON study of M32: measuring the <span class="hlt">intrinsic</span> flattening and the central black hole mass</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Verolme, E. K.; Cappellari, M.; Copin, Y.; van der Marel, R. P.; Bacon, R.; Bureau, M.; Davies, R. L.; Miller, B. M.; de Zeeuw, P. T.</p> <p>2002-09-01</p> <p>We present dynamical models of the nearby compact <span class="hlt">elliptical</span> galaxy M32, using high-quality kinematic measurements, obtained with the integral-field spectrograph SAURON mounted on the William Herschel Telescope on La Palma. We also include STIS data obtained previously by Joseph et al. We find a best-fitting black hole mass of M•= (2.5 +/- 0.5) × 106 Msolar and a stellar I-band mass-to-light ratio of (1.85 +/- 0.15) Msolar/Lsolar. For the first time, we are also able to constrain the inclination along which M32 is observed to 70°+/- 5°. Assuming that M32 is indeed axisymmetric, the averaged observed flattening of 0.73 then corresponds to an <span class="hlt">intrinsic</span> flattening of 0.68 +/- 0.03. These tight constraints are mainly caused by the use of integral-field data. We show this quantitatively by comparing with models that are constrained by multiple slits only. We show the phase-space distribution and <span class="hlt">intrinsic</span> velocity structure of the best-fitting model and investigate the effect of regularization on the orbit distribution.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016ApJ...824...40O','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016ApJ...824...40O"><span id="translatedtitle">The <span class="hlt">Intrinsic</span> Shape of Sagittarius A* at 3.5 mm Wavelength</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Ortiz-León, Gisela N.; Johnson, Michael D.; Doeleman, Sheperd S.; Blackburn, Lindy; Fish, Vincent L.; Loinard, Laurent; Reid, Mark J.; Castillo, Edgar; Chael, Andrew A.; Hernández-Gómez, Antonio; Hughes, David H.; León-Tavares, Jonathan; Lu, Ru-Sen; Montaña, Alfredo; Narayanan, Gopal; Rosenfeld, Katherine; Sánchez, David; Schloerb, F. Peter; Shen, Zhi-qiang; Shiokawa, Hotaka; SooHoo, Jason; Vertatschitsch, Laura</p> <p>2016-06-01</p> <p>The radio emission from Sgr A{}\\ast is thought to be powered by accretion onto a supermassive black hole of ˜ 4× {10}6 {M}⊙ at the Galactic Center. At millimeter wavelengths, Very Long Baseline Interferometry (VLBI) observations can directly resolve the bright innermost accretion region of Sgr A{}\\ast . Motivated by the addition of many sensitive long baselines in the north-south direction, we developed a full VLBI capability at the Large Millimeter Telescope Alfonso Serrano (LMT). We successfully detected Sgr A{}\\ast at 3.5 mm with an array consisting of six Very Long Baseline Array telescopes and the LMT. We model the source as an <span class="hlt">elliptical</span> Gaussian brightness distribution and estimate the scattered size and orientation of the source from closure amplitude and self-calibration analysis, obtaining consistent results between methods and epochs. We then use the known scattering kernel to determine the <span class="hlt">intrinsic</span> two-dimensional source size at 3.5 mm: (147+/- 7 μ {{as}})× (120+/- 12 μ {{as}}), at position angle 88^\\circ +/- 7^\\circ east of north. Finally, we detect non-zero closure phases on some baseline triangles, but we show that these are consistent with being introduced by refractive scattering in the interstellar medium and do not require <span class="hlt">intrinsic</span> source asymmetry to explain.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19950038708&hterms=globular&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D60%26Ntt%3Dglobular','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19950038708&hterms=globular&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D60%26Ntt%3Dglobular"><span id="translatedtitle">The fundamental plane <span class="hlt">correlations</span> for globular clusters</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Djorgovski, S.</p> <p>1995-01-01</p> <p>In the parameter space whose axes include a radius (core, or half-light), a surface brightness (central, or average within the half-light radius), and the central projected velocity dispersion, globular clusters lie on a two-dimensional surface (a plane, if the logarithmic quantities are used). This is analogous to the 'fundamental plane' of <span class="hlt">elliptical</span> galaxies. The implied bivariate <span class="hlt">correlations</span> are the best now known for globular clusters. The derived scaling laws for the core properties imply that cluster cores are fully virialized, homologous systems, with a constant (M/L) ratio. The corresponding scaling laws on the half-light scale are differrent, but are nearly identical to those derived from the 'fundamental plane' of <span class="hlt">ellipticals</span>. This may be due to the range of cluster concentrations, which are <span class="hlt">correlated</span> with other parameters. A similar explanation for <span class="hlt">elliptical</span> galaxies may be viable. These <span class="hlt">correlations</span> provide new empirical constraints for models of globular cluster formation and evolution, and may also be usable as rough distance-indicator relations for globular clusters.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/1991JPSJ...60.3983H','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/1991JPSJ...60.3983H"><span id="translatedtitle"><span class="hlt">Intrinsic</span> Probability of a Multifractal Set</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Hosokawa, Iwao</p> <p>1991-12-01</p> <p>It is shown that a self-similar measure isotropically distributed in a d-dimensional set should have its own intermittency exponents equivalent to its own generalized dimensions (in the sense of Hentschel and Procaccia), and that the intermittency exponents are completely designated by an <span class="hlt">intrinsic</span> probability which governs the spatial distribution of the measure. Based on this, it is proven that the <span class="hlt">intrinsic</span> probability uniquely determines the spatial distribution of the scaling index α of the measure as well as the so-called f-α spectrum of the multifractal set.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/6288095','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/6288095"><span id="translatedtitle">Bootstrapped models for <span class="hlt">intrinsic</span> random functions</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Campbell, K.</p> <p>1988-08-01</p> <p>Use of <span class="hlt">intrinsic</span> random function stochastic models as a basis for estimation in geostatistical work requires the identification of the generalized covariance function of the underlying process. The fact that this function has to be estimated from data introduces an additional source of error into predictions based on the model. This paper develops the sample reuse procedure called the bootstrap in the context of <span class="hlt">intrinsic</span> random functions to obtain realistic estimates of these errors. Simulation results support the conclusion that bootstrap distributions of functionals of the process, as well as their kriging variance, provide a reasonable picture of variability introduced by imperfect estimation of the generalized covariance function.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://www.osti.gov/scitech/servlets/purl/6340930','SCIGOV-STC'); return false;" href="http://www.osti.gov/scitech/servlets/purl/6340930"><span id="translatedtitle">Bootstrapped models for <span class="hlt">intrinsic</span> random functions</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Campbell, K.</p> <p>1987-01-01</p> <p>The use of <span class="hlt">intrinsic</span> random function stochastic models as a basis for estimation in geostatistical work requires the identification of the generalized covariance function of the underlying process, and the fact that this function has to be estimated from the data introduces an additional source of error into predictions based on the model. This paper develops the sample reuse procedure called the ''bootstrap'' in the context of <span class="hlt">intrinsic</span> random functions to obtain realistic estimates of these errors. Simulation results support the conclusion that bootstrap distributions of functionals of the process, as well as of their ''kriging variance,'' provide a reasonable picture of the variability introduced by imperfect estimation of the generalized covariance function.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19910007606','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19910007606"><span id="translatedtitle">Dust and ionized gas in active radio <span class="hlt">elliptical</span> galaxies</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Forbes, D. A.; Sparks, W. B.; Macchetto, F. D.</p> <p>1990-01-01</p> <p>The authors present broad and narrow bandwidth imaging of three southern <span class="hlt">elliptical</span> galaxies which have flat-spectrum active radio cores (NGC 1052, IC 1459 and NGC 6958). All three contain dust and extended low excitation optical line emission, particularly extensive in the case of NGC 1052 which has a large H alpha + (NII) luminosity. Both NGC 1052 and IC 1459 have a spiral morphology in emission-line images. All three display independent strong evidence that a merger or infall event has recently occurred, i.e., extensive and infalling HI gas in NGC 1052, a counter-rotating core in IC 1459 and Malin-Carter shells in NGC 6958. This infall event is the most likely origin for the emission-line gas and dust, and the authors are currently investigating possible excitation mechanisms (Sparks et al. 1990).</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/pages/biblio/1235326-miniaturized-ltcc-elliptic-function-lowpass-filters-side-stopbands','SCIGOV-DOEP'); return false;" href="https://www.osti.gov/pages/biblio/1235326-miniaturized-ltcc-elliptic-function-lowpass-filters-side-stopbands"><span id="translatedtitle">Miniaturized LTCC <span class="hlt">elliptic</span>-function lowpass filters with side stopbands</span></a></p> <p><a target="_blank" href="http://www.osti.gov/pages">DOE PAGES</a></p> <p>Hsieh, Lung -Hwa; Dai, Steve Xunhu</p> <p>2015-05-28</p> <p>A compact, high-selectivity, and wide stopband lowpass filter is highly demanded in wireless communication systems to suppress adjacent harmonics and unwanted signals. In this letter, a new miniaturized lowpass filter with <span class="hlt">elliptic</span>-function frequency response is introduced. The filter is fabricated in multilayer low temperature cofired ceramics. The size of the miniaturized filter is 5.5 × 3.9 × 1.72 mm3. As a result, the measured insertion loss of the filter is better than 0.37 dB from DC to 1.28 GHz and the measured stopband of the filter is great than 22 dB from 2.3 to 7.5 GHz.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/22494656','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/22494656"><span id="translatedtitle">Magnetic flux studies in horizontally cooled <span class="hlt">elliptical</span> superconducting cavities</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Martinello, M. Checchin, M.; Grassellino, A. Crawford, A. C.; Melnychuk, O.; Romanenko, A.; Sergatskov, D. A.</p> <p>2015-07-28</p> <p>Previous studies on magnetic flux expulsion as a function of cooldown procedures for <span class="hlt">elliptical</span> superconducting radio frequency (SRF) niobium cavities showed that when the cavity beam axis is placed parallel to the helium cooling flow and sufficiently large thermal gradients are achieved, all magnetic flux could be expelled and very low residual resistance could be achieved. In this paper, we investigate flux trapping for the case of resonators positioned perpendicularly to the helium cooling flow, which is more representative of how SRF cavities are cooled in accelerators and for different directions of the applied magnetic field surrounding the resonator. We show that different field components have a different impact on the surface resistance, and several parameters have to be considered to fully understand the flux dynamics. A newly discovered phenomenon of concentration of flux lines at the cavity top leading to temperature rise at the cavity equator is presented.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19940026931','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19940026931"><span id="translatedtitle">Multisatellite constellation configuration selection for multiregional highly <span class="hlt">elliptical</span> orbit constellations</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Matossian, Mark G.</p> <p>1994-01-01</p> <p>The Archimedes Project is a joint effort of the European Space Agency (ESA) and the National Space Development Agency of Japan (NASDA). The primary goal of the Archimedes project is to perform a technical feasibility analysis and preliminary design of a highly inclined multisatellite constellation for direct broadcast and mobile communications services for Europe, Japan and much of North America. This report addresses one aspect of this project, specifically an analysis of continuous satellite coverage using multiregional highly <span class="hlt">elliptical</span> orbits (M-HEO's). The analysis methodology and ensuing software tool, named SPIFF, were developed specifically for this project by the author during the summer of 1992 under the STA/NSF Summer Institute in Japan Program at Tsukuba Space Center.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/437563','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/437563"><span id="translatedtitle">Asymptotics of solutions of some nonlinear <span class="hlt">elliptic</span> systems</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Bidaut-Veron, M.F.; Raoux, T.</p> <p>1996-12-31</p> <p>This paper deals with the local and global behaviour of the positive solutions of the semilinear <span class="hlt">elliptic</span> system in R{sup N} (N{ge}3) {Delta}u+{vert_bar}x{vert_bar}{sup {sigma}}u{sup q}v{sup p+1} =0, {Delta}v+{vert_bar}x{vert_bar}{sup {sigma}}u{sup q+1}v{sup p}=0, where {sigma},p,q{epsilon}R, and p,q>0. Our main results in the fact that the solutions satisfy Harnack inequality when Q = p+q+1<(N+2)/(N-2), which gives local estimates. Without this assumption on Q, we give the precise behaviour of the solutions, provided that these estimates are true. When Q < (N+2)/(N-2), the solutions can also present an anisotropic behaviour. 34 refs.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19780047977&hterms=braking&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D30%26Ntt%3Dbraking','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19780047977&hterms=braking&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D30%26Ntt%3Dbraking"><span id="translatedtitle">Atmospheric braking to circularize an <span class="hlt">elliptical</span> Venus orbit</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Mcronald, A. D.; Nock, K. T.</p> <p>1977-01-01</p> <p>The use of atmospheric drag to circularize an <span class="hlt">elliptical</span> spacecraft orbit at Venus is analyzed parametrically for the Venus Orbital Imaging Radar Mission (VOIR) in 1983. Navigation, maneuver, and guidance requirements are discussed for the decay of a 24-hr orbit to a close circular orbit in about 30-60 days. A prototype 'Aerobrake' is described which is approximately 5 m in diameter and 25 kg in mass and which replaces a chemical retroengine of about 1300 kg in mass (delta V = 2.5 km/s) by a 700 kg in-orbit mass. The aerobrake, a light deployable Inconel sheet, shields the spacecraft from the flow and radiates the aerodynamic heating.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/1995CeMDA..62..305D','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/1995CeMDA..62..305D"><span id="translatedtitle">Some Expansions of the <span class="hlt">Elliptic</span> Motion to High Eccentricities</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>da Silva Fernandes, Sandro</p> <p>1995-12-01</p> <p>Some classic expansions of the <span class="hlt">elliptic</span> motion — cosmE and sinmE — in powers of the eccentricity are extended to highly eccentric orbits, 0.6627...<e<1. The new expansions are developed in powers of (e-e*), wheree* is a fixed value of the eccentricity. The coefficients are given in terms of the derivatives of Bessel functions with respect to the eccentricity. The expansions have the same radius of convergence ρ(e*) of the extended solution of Kepler's equation, previously derived by the author. Some other simple expansions — (a/r), (r/a), (r/a) sinv, ..., — derived straightforward from the expansions ofE, cosE and sinE are also presented.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19840060628&hterms=ascent+guidance&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D60%26Ntt%3Dascent%2Bguidance','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19840060628&hterms=ascent+guidance&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D60%26Ntt%3Dascent%2Bguidance"><span id="translatedtitle">Explicit guidance of drag modulated aeroassisted transfer between <span class="hlt">elliptical</span> orbits</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Vinh, N. X.; Mease, K. D.; Hanson, J. M.; Johannesen, J. R.</p> <p>1984-01-01</p> <p>This paper presents the complete analysis of the problem of minimum-fuel aeroassisted transfer between coplanar <span class="hlt">elliptical</span> orbits in the case where the orientation of the final orbit is free for selection in the optimization process. The comparison between the optimal pure propulsive transfer and the idealized aeroassisted transfer, by several passages through the atmosphere, is made. In the case where aeroassisted transfer provides fuel saving, a practical scheme for its realization by one passage is proposed. The maneuver consists of three phases: a deorbit phase for nonzero entry angle, followed by an atmospheric fly-through with variable drag control and completed by a postatmospheric phase. An explicit guidance formula for drag control is derived and it is shown that the required exit speed for ascent to the final orbit can be obtained with a very high degree of accuracy.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2001JASS...18..175C','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2001JASS...18..175C"><span id="translatedtitle">Stellar Population Synthesis of the <span class="hlt">Elliptical</span> Galaxy NGC 4649</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Chun, Mun-Suk; Gim, Moon-Whan; Sohn, Young-Jong</p> <p>2001-12-01</p> <p>We investigated population of the <span class="hlt">elliptical</span> galaxy NGC 4649 using the spectral synthesis technique based on the linear program in the spectral regions between 3160Å to 10800Å. We used the spectral data of stars obtained by Gunn & Stryker (1983), and the integrated spectrum of NGC 4649 observed by Bertola et al. (1982). Among four models with different main sequence turn-off points, G8-K0V main sequence turn-off model is best fitted to the integrated spectrum of NGC 4649. We also found that super metal rich K giants are needed to describe the absorption lines in the long wavelength regions of integrated spectrum of NGC 4649. The mass to absolute light ratio obtained from the spectral synthesis is ~20 similar to those calculated dynamically.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://ntrs.nasa.gov/search.jsp?R=19920028108&hterms=emissions+paris+agreement&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D50%26Ntt%3Demissions%2Bparis%2Bagreement','NASA-TRS'); return false;" href="https://ntrs.nasa.gov/search.jsp?R=19920028108&hterms=emissions+paris+agreement&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D50%26Ntt%3Demissions%2Bparis%2Bagreement"><span id="translatedtitle">On the <span class="hlt">elliptical</span> polarization of Jupiter's decametric radio emission</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Melrose, D. B.; Dulk, G. A.</p> <p>1991-01-01</p> <p>The origin of the 100 percent <span class="hlt">elliptical</span> polarization of Jupiter's decametric radio emission is investigated. The transfer of polarized radiation when coupling of the Stokes parameters is important is studied, and it is found, in agreement with earlier authors, that the density in and near the source region must be so low that the polarization remains fixed along the ray path. The polarization of the cyclotron maser radiation in these circumstances is determined, and it is found that the dispersion relation of the rarefied plasma composed of energetic, anisotropic electrons is like that in the vacuum. It is also found that the growth rate is sufficient to saturate the maser and account for the observed brightness temperature. Possible sources of plasma in and near the source region in Jupiter's inner, polar magnetosphere are considered.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://www.osti.gov/scitech/servlets/purl/5306227','SCIGOV-STC'); return false;" href="http://www.osti.gov/scitech/servlets/purl/5306227"><span id="translatedtitle">A domain decomposition algorithm for solving large <span class="hlt">elliptic</span> problems</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Nolan, M.P.</p> <p>1991-01-01</p> <p>AN algorithm which efficiently solves large systems of equations arising from the discretization of a single second-order <span class="hlt">elliptic</span> partial differential equation is discussed. The global domain is partitioned into not necessarily disjoint subdomains which are traversed using the Schwarz Alternating Procedure. On each subdomain the multigrid method is used to advance the solution. The algorithm has the potential to decrease solution time when data is stored across multiple levels of a memory hierarchy. Results are presented for a virtual memory, vector multiprocessor architecture. A study of choice of inner iteration procedure and subdomain overlap is presented for a model problem, solved with two and four subdomains, sequentially and in parallel. Microtasking multiprocessing results are reported for multigrid on the Alliant FX-8 vector-multiprocessor. A convergence proof for a class of matrix splittings for the two-dimensional Helmholtz equation is given. 70 refs., 3 figs., 20 tabs.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/6536676','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/6536676"><span id="translatedtitle">Dynamical modeling of <span class="hlt">elliptical</span> galaxies. II. numerical prolate models</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Lake, G.</p> <p>1981-01-01</p> <p>The analytical solutions of Paper I are generalized using the self-consistent field method. These prolate models are constructed using only two integrals of motion, the energy (E) and the angular momentum about the axis of symmetry, (L/sub z/). They are the first models with flattening greater than E4 which possess <span class="hlt">elliptical</span> isophotes and realistic density profiles. The singularity in the surface brightness which characterized the models of Paper I has been removed by smoothing the extreme suppression of L/sub z/. The new models (like those of Paper I) still show a sharp rise in the velocity dispersion at the center. This feature is due to the strongly anisotropic velocity dispersions, rather than the existence of a supermassive object.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2017PApGe.174.1153C','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2017PApGe.174.1153C"><span id="translatedtitle">Grid Setting in Seismic Tomography for <span class="hlt">Elliptical</span> Anisotropic Media</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Cardarelli, E.; Cerreto, A.</p> <p>2017-03-01</p> <p>In this study, we discuss the adjustment of grid definition in relation to seismic tomography in the case of <span class="hlt">elliptical</span> anisotropic media. To optimize cell numbers and dimensions, the results of a staggered grid method are used to define an adjusted grid as a starting model for inversion. This procedure can be iterated, although improvements are not assured. First, two synthetic models with growing level of complexity are performed. Next, data from a previously conducted field survey are analyzed by introducing staggered grids. Finally, the results are compared with the previous results. The adjusted grid represents a technique that can be used to obtain an effective way of discretizing the model domain for further inversion, which often improves results for the velocity model. These conclusions can also be applied to isotropic media, as described in this study.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2013SPIE.8760E..1QS','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2013SPIE.8760E..1QS"><span id="translatedtitle">Truncated stacked <span class="hlt">elliptical</span> patch antenna for broadband performance</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Sharma, Vijay; Sharma, Brajraj; Sharma, K. B.; Bhatnagar, D.</p> <p>2013-01-01</p> <p>A new design of a single-feed truncated <span class="hlt">elliptical</span> patch antenna with and without slots for broadband performance with stacked arrangement is proposed in this paper and its performance is tested in free space. This multilayered rectangular microstrip antenna is designed and analyzed by using the ie3d simulation software. In between conducting and ground plane, designed antenna has two glass epoxy fr-4 substrates separated by an air substrate to attain broadband performance. The impedance bandwidth of designed antenna is better than 2.11GHz or 60% with respect to the central frequency. The simulated e plane co and cross radiation patterns are identical in shape for most of the part of bandwidth however at higher frequency side due to the presence of higher modes and cross polarization the radiation pattern are no more directive normal to patch geometry.</p> </li> </ol> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_21");'>21</a></li> <li><a href="#" onclick='return showDiv("page_22");'>22</a></li> <li><a href="#" onclick='return showDiv("page_23");'>23</a></li> <li class="active"><span>24</span></li> <li><a href="#" onclick='return showDiv("page_25");'>25</a></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div><!-- col-sm-12 --> </div><!-- row --> </div><!-- page_24 --> <div id="page_25" class="hiddenDiv"> <div class="row"> <div class="col-sm-12"> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_21");'>21</a></li> <li><a href="#" onclick='return showDiv("page_22");'>22</a></li> <li><a href="#" onclick='return showDiv("page_23");'>23</a></li> <li><a href="#" onclick='return showDiv("page_24");'>24</a></li> <li class="active"><span>25</span></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div> </div> <div class="row"> <div class="col-sm-12"> <ol class="result-class" start="481"> <li> <p><a target="_blank" onclick="trackOutboundLink('http://www.osti.gov/scitech/servlets/purl/510563','SCIGOV-STC'); return false;" href="http://www.osti.gov/scitech/servlets/purl/510563"><span id="translatedtitle">Heterogeneous domain decomposition for singularly perturbed <span class="hlt">elliptic</span> boundary value problems</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Garbey, M.; Kaper, H.G.</p> <p>1995-04-14</p> <p>A heterogeneous domain-decomposition method is presented for the numerical solution of singularly perturbed <span class="hlt">elliptic</span> boundary value problem. The method, which is parallelizable at various levels, uses several ideas of asymptotic analysis. The sub-domains match the domains of validity of the local ({open_quotes}inner{close_quotes} and {open_quotes}outer{close_quotes}) asymptotic expansions, and cut-off functions are used to match solutions in neighboring subdomains. The positions of the interfaces, as well as the mesh widths, depend on the small parameter, {epsilon}. On the subdomains, iterative solution techniques are used, which may vary from one subdomain to another. The global convergence rate depends on {epsilon}; it generally increases like some power of (log({epsilon}{sup -1})){sup -1} as {epsilon} {down_arrow} 0. The method is illustrated on several two-dimensional singular perturbation problems.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/17280320','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/17280320"><span id="translatedtitle">Vortex chirality in exchange-biased <span class="hlt">elliptical</span> magnetic rings.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Jung, W; Castaño, F J; Ross, C A</p> <p>2006-12-15</p> <p>The flux-closed or "vortex" state in thin-film magnetic rings has been proposed as a data storage token, but it has proven difficult to control the vortex chirality in a simple manner. Here, a model is described that predicts the vortex chirality of an <span class="hlt">elliptical</span> magnetic ring as a function of the direction of the applied field and of the exchange bias, based on the change in energy of the system as the domain walls move. Experimental measurements of chirality in Co and Co/IrMn magnetic rings with 3.2 microm major axis are in excellent agreement with the model. The vortex circulation direction can therefore be tailored with an appropriate combination of applied field direction and exchange bias direction with respect to the major axis.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19830021785','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19830021785"><span id="translatedtitle">Algorithms and data structures for adaptive multigrid <span class="hlt">elliptic</span> solvers</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Vanrosendale, J.</p> <p>1983-01-01</p> <p>Adaptive refinement and the complicated data structures required to support it are discussed. These data structures must be carefully tuned, especially in three dimensions where the time and storage requirements of algorithms are crucial. Another major issue is grid generation. The options available seem to be curvilinear fitted grids, constructed on iterative graphics systems, and unfitted Cartesian grids, which can be constructed automatically. On several grounds, including storage requirements, the second option seems preferrable for the well behaved scalar <span class="hlt">elliptic</span> problems considered here. A variety of techniques for treatment of boundary conditions on such grids are reviewed. A new approach, which may overcome some of the difficulties encountered with previous approaches, is also presented.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2009SIGMA...5..065L','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2009SIGMA...5..065L"><span id="translatedtitle">Monopoles and Modifications of Bundles over <span class="hlt">Elliptic</span> Curves</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Levin, Andrey M.; Olshanetsky, Mikhail A.; Zotov, Andrei V.</p> <p>2009-06-01</p> <p>Modifications of bundles over complex curves is an operation that allows one to construct a new bundle from a given one. Modifications can change a topological type of bundle. We describe the topological type in terms of the characteristic classes of the bundle. Being applied to the Higgs bundles modifications establish an equivalence between different classical integrable systems. Following Kapustin and Witten we define the modifications in terms of monopole solutions of the Bogomolny equation. We find the Dirac monopole solution in the case R × (<span class="hlt">elliptic</span> curve). This solution is a three-dimensional generalization of the Kronecker series. We give two representations for this solution and derive a functional equation for it generalizing the Kronecker results. We use it to define Abelian modifications for bundles of arbitrary rank. We also describe non-Abelian modifications in terms of theta-functions with characteristic.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/6931777','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/6931777"><span id="translatedtitle">Construction of preconditioners for <span class="hlt">elliptic</span> problems by substructuring, III</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Bramble, J.H.; Pasciak, J.E.; Schatz, A.H.</p> <p>1988-10-01</p> <p>In earlier parts of this series of papers, we constructed preconditioners for the discrete systems of equations arising from the numerical approximation of <span class="hlt">elliptic</span> boundary value problems. The resulting algorithms are well suited for implementation on computers with parallel architecture. In this paper, we will develop a technique which utilizes these earlier methods to derive even more efficient preconditioners. The iterative algorithms using these new preconditioners converge to the solution of the discrete equations with a rate that is independent of the number of unknowns. These preconditioners involve an incomplete Chebyshev iteration for boundary interface conditions which results in a negligible increase in the amount of computational work. Theoretical estimates and the results of numerical experiments are given which demonstrate the effectiveness of the methods.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/6485968','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/6485968"><span id="translatedtitle">Construction of preconditioners for <span class="hlt">elliptic</span> problems by substructuring. I</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Bramble, J.H.; Pasciak, J.E.; Schatz, A.H.</p> <p>1986-07-01</p> <p>We consider the problem of solving the algebraic system of equations which arise from the discretization of symmetric <span class="hlt">elliptic</span> boundary value problems via finite element methods. A new class of preconditioners for the discrete system is developed based on substructuring (also known as domain decomposition). The resulting preconditioned algorithms are well suited to emerging parallel computing architectures. The proposed methods are applicable to problems on general domains involving differential operators with rather general coefficients. A basic theory for the analysis of the condition number of the preconditioned system (which determines the iterative convergence rate of the algorithm) is given. Techniques for applying the theory and algorithms to problems with irregular geometry are discussed and the results of extensive numerical experiments are reported.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2004cbhg.sympE..21G','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2004cbhg.sympE..21G"><span id="translatedtitle">Inner and Outer Photometric Structure of <span class="hlt">Elliptical</span> Galaxies</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Graham, Alister W.; Erwin, P.; Trujillo, I.; Asensio Ramos, A.</p> <p></p> <p>The Nuker model, when applied to the inner regions of ``core'' galaxies, is shown to produce systematic biases in the determination of the core ``break-radii''. These radii can easily be (and often have been, see Trujillo et al. 2003) over-estimated by more than 100%. Moreover, due to curvature in the outer profiles of early-type galaxies (i.e., beyond the break-radius), none of the Nuker model parameters are found to be robust quantities. A new empirical model that simultaneously describes both the inner and outer light-profiles of <span class="hlt">elliptical</span> galaxies (and bulges in general) is presented. It consists of a Sérsic function with an inner power-law and a variable transition region.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/19920006444','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/19920006444"><span id="translatedtitle">Optimal least-squares finite element method for <span class="hlt">elliptic</span> problems</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Jiang, Bo-Nan; Povinelli, Louis A.</p> <p>1991-01-01</p> <p>An optimal least squares finite element method is proposed for two dimensional and three dimensional <span class="hlt">elliptic</span> problems and its advantages are discussed over the mixed Galerkin method and the usual least squares finite element method. In the usual least squares finite element method, the second order equation (-Delta x (Delta u) + u = f) is recast as a first order system (-Delta x p + u = f, Delta u - p = 0). The error analysis and numerical experiment show that, in this usual least squares finite element method, the rate of convergence for flux p is one order lower than optimal. In order to get an optimal least squares method, the irrotationality Delta x p = 0 should be included in the first order system.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/18970616','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/18970616"><span id="translatedtitle">Determination of <span class="hlt">intrinsic</span> viscosity of poly(ethylene terephthalate) using infrared spectroscopy and multivariate calibration method.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Silva Spinacé, M A; Lucato, M U; Ferrão, M F; Davanzo, C U; De Paoli, M-A</p> <p>2006-05-15</p> <p>A methodology was developed to determine the <span class="hlt">intrinsic</span> viscosity of poly(ethylene terephthalate) (PET) using diffuse reflectance infrared Fourier transform spectroscopy (DRIFTS) and multivariate calibration (MVC) methods. Multivariate partial least squares calibration was applied to the spectra using mean centering and cross validation. The results were <span class="hlt">correlated</span> to the <span class="hlt">intrinsic</span> viscosities determined by the standard chemical method (ASTM D 4603-01) and a very good <span class="hlt">correlation</span> for values in the range from 0.346 to 0.780dLg(-1) (relative viscosity values ca. 1.185-1.449) was observed. The spectrophotometer detector sensitivity and the humidity of the samples did not influence the results. The methodology developed is interesting because it does not produce hazardous wastes, avoids the use of time-consuming chemical methods and can rapidly predict the <span class="hlt">intrinsic</span> viscosity of PET samples over a large range of values, which includes those of recycled materials.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3780435','PMC'); return false;" href="https://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3780435"><span id="translatedtitle">WEAK GALERKIN METHODS FOR SECOND ORDER <span class="hlt">ELLIPTIC</span> INTERFACE PROBLEMS</span></a></p> <p><a target="_blank" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p>MU, LIN; WANG, JUNPING; WEI, GUOWEI; YE, XIU; ZHAO, SHAN</p> <p>2013-01-01</p> <p>Weak Galerkin methods refer to general finite element methods for partial differential equations (PDEs) in which differential operators are approximated by their weak forms as distributions. Such weak forms give rise to desirable flexibilities in enforcing boundary and interface conditions. A weak Galerkin finite element method (WG-FEM) is developed in this paper for solving <span class="hlt">elliptic</span> PDEs with discontinuous coefficients and interfaces. Theoretically, it is proved that high order numerical schemes can be designed by using the WG-FEM with polynomials of high order on each element. Extensive numerical experiments have been carried to validate the WG-FEM for solving second order <span class="hlt">elliptic</span> interface problems. High order of convergence is numerically confirmed in both L2 and L∞ norms for the piecewise linear WG-FEM. Special attention is paid to solve many interface problems, in which the solution possesses a certain singularity due to the nonsmoothness of the interface. A challenge in research is to design nearly second order numerical methods that work well for problems with low regularity in the solution. The best known numerical scheme in the literature is of order O(h) to O(h1.5) for the solution itself in L∞ norm. It is demonstrated that the WG-FEM of the lowest order, i.e., the piecewise constant WG-FEM, is capable of delivering numerical approximations that are of order O(h1.75) to O(h2) in the L∞ norm for C1 or Lipschitz continuous interfaces associated with a C1 or H2 continuous solution. PMID:24072935</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://hdl.handle.net/2060/20040074328','NASA-TRS'); return false;" href="http://hdl.handle.net/2060/20040074328"><span id="translatedtitle">Underexpanded Screeching Jets From Circular, Rectangular, and <span class="hlt">Elliptic</span> Nozzles</span></a></p> <p><a target="_blank" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p>Panda, J.; Raman, G.; Zaman, K. B. M. Q.</p> <p>2004-01-01</p> <p>The screech frequency and amplitude, the shock spacing, the hydrodynamic-acoustic standing wave spacing, and the convective velocity of large organized structures are measured in the nominal Mach number range of 1.1 less than or = Mj less that or = l0.9 for supersonic, underexpanded jets exhausting from a circular, a rectangular and an <span class="hlt">elliptic</span> nozzle. This provides a carefully measured data set useful in comparing the importance of various physical parameters in the screech generation process. The hydrodynamic-acoustic standing wave is formed between the potential pressure field of large turbulent structures and the acoustic pressure field of the screech sound. It has been demonstrated earlier that in the currently available screech frequency prediction models replacement of the shock spacing by the standing wave spacing provides an exact expression. In view of this newly found evidence, a comparison is made between the average standing wavelength and the average shock spacing. It is found that there exists a small, yet important, difference, which is dependent on the azimuthal screech mode. For example, in the flapping modes of circular, rectangular, and <span class="hlt">elliptic</span> jets, the standing wavelength is slightly longer than the shock spacing, while for the helical screech mode in a circular jet the opposite is true. This difference accounts for the departure of the existing models from predicting the exact screech frequency. Another important parameter, necessary in screech prediction, is the convective velocity of the large organized structures. It is demonstrated that the presence of the hydrodynamic-acoustic standing wave, even inside the jet shear layer, becomes a significant source of error in the convective velocity data obtained using the conventional methods. However, a new relationship, using the standing wavelength and screech frequency is shown to provide more accurate results.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2004AJ....127.3213M','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2004AJ....127.3213M"><span id="translatedtitle">Early-Type Galaxies in Extremely Isolated Environments: Typical <span class="hlt">Ellipticals</span>?</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Marcum, Pamela M.; Aars, Christian E.; Fanelli, Michael N.</p> <p>2004-06-01</p> <p>We have conducted a BVR imaging survey of nine early-type galaxies previously verified to exist in extremely isolated environments. Our goals are to establish a baseline of morphological and photometric properties for spheroidal systems evolving in extremely low-density environments and to compare these properties with signatures predicted for merged galaxy groups. We find that these isolated systems are underluminous by at least a magnitude compared with objects identified as merged group remnants in other studies. Image processing techniques sensitive to shell features produced no detections, a result in strong contrast to the high frequency of such structures found in other isolated <span class="hlt">elliptical</span> galaxies. Two objects, KIG 164 and KIG 870, appear to be merger remnants, as indicated by their disturbed morphology, apparent tidal features, and blue colors. KIG 164 exhibits an asymmetric nuclear morphology and a low surface brightness ``bridge'' between it and a possible dwarf satellite. KIG 870 shows both fan-shaped emission at large radii and a possible double nucleus. Two other galaxies, KIG 412 and KIG 792, are also blue, but without any morphological peculiarities, suggesting that these systems are advanced mergers, older than KIG 164 and KIG 870. Two systems appear to be isolated lenticular galaxies with no evidence of a merger history. Based on their red colors, good fit to a R1/4-law light distribution, and the lack of morphological peculiarities, two other galaxies, KIG 557 and KIG 824, are found to be excellent candidates for passively evolving primordial <span class="hlt">elliptical</span> galaxies formed early in cosmic time. Optical data were obtained with the 2.1 m Otto Struve telescope at McDonald Observatory, which is operated by the University of Texas at Austin.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/24072935','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/24072935"><span id="translatedtitle">WEAK GALERKIN METHODS FOR SECOND ORDER <span class="hlt">ELLIPTIC</span> INTERFACE PROBLEMS.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Mu, Lin; Wang, Junping; Wei, Guowei; Ye, Xiu; Zhao, Shan</p> <p>2013-10-01</p> <p>Weak Galerkin methods refer to general finite element methods for partial differential equations (PDEs) in which differential operators are approximated by their weak forms as distributions. Such weak forms give rise to desirable flexibilities in enforcing boundary and interface conditions. A weak Galerkin finite element method (WG-FEM) is developed in this paper for solving <span class="hlt">elliptic</span> PDEs with discontinuous coefficients and interfaces. Theoretically, it is proved that high order numerical schemes can be designed by using the WG-FEM with polynomials of high order on each element. Extensive numerical experiments have been carried to validate the WG-FEM for solving second order <span class="hlt">elliptic</span> interface problems. High order of convergence is numerically confirmed in both L2 and L∞ norms for the piecewise linear WG-FEM. Special attention is paid to solve many interface problems, in which the solution possesses a certain singularity due to the nonsmoothness of the interface. A challenge in research is to design nearly second order numerical methods that work well for problems with low regularity in the solution. The best known numerical scheme in the literature is of order [Formula: see text] to [Formula: see text] for the solution itself in L∞ norm. It is demonstrated that the WG-FEM of the lowest order, i.e., the piecewise constant WG-FEM, is capable of delivering numerical approximations that are of order [Formula: see text] to [Formula: see text] in the L∞ norm for C(1) or Lipschitz continuous interfaces associated with a C(1) or H(2) continuous solution.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2015SPIE.9573E..0BC','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2015SPIE.9573E..0BC"><span id="translatedtitle"><span class="hlt">Elliptically</span> framed tip-tilt mirror optimized for stellar tracking</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Clark, James H.; Penado, F. E.; Petak, Jeremy</p> <p>2015-09-01</p> <p>We compare a design innovation of an <span class="hlt">elliptically</span> framed tip-tilt optical tracker with an existing circularly framed tracker for the Navy Precision Optical Interferometer. The tracker stabilizes a 12.5 cm stellar beam on a target hundreds of meters away and requires an increase in operational frequency. We reduced mass and size by integrating an <span class="hlt">elliptical</span> mirror as one of the rotating components, which eliminated a rotating frame. We used the same materials as the existing tracker; however, light-weighted both the aluminum frame and Zerodur® mirror. We generated a computer-aided design model, converted it into a finite element model and performed modal analysis on two load cases. In load case 1, we tied down three points on the bottom surface of the tracker corresponding to the tie-down points of the comparison tracker. This reveals a first mode (lowest) frequency of 140 Hz, a factor of two over the baseline tracker's first mode frequency of 67 Hz. In load case 2, we constrained four additional points inboard of the corners of the tracker base, for a total of seven tie-downs, simulating a firmly bolted and secured mount. The first mode of vibration for this case is 211 Hz, an increase over load case 1 by a factor of 1.5 and more than three times the fundamental frequency of the existing tracker. We conclude that these geometrical changes with the additional tie-down bolts are a viable solution path forward to improve steering speed and recommend a continuation with this effort.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://adsabs.harvard.edu/abs/2016PhFl...28c6101Z','NASAADS'); return false;" href="http://adsabs.harvard.edu/abs/2016PhFl...28c6101Z"><span id="translatedtitle">Aspect ratio effect on shock-accelerated <span class="hlt">elliptic</span> gas cylinders</span></a></p> <p><a target="_blank" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p>Zou, Liyong; Liao, Shenfei; Liu, Cangli; Wang, Yanping; Zhai, Zhigang</p> <p>2016-03-01</p> <p>The evolution of an <span class="hlt">elliptic</span> heavy-gas (SF6) cylinder accelerated by a planar weak shock wave is investigated experimentally using particle image velocimetry (PIV) diagnostics, and the emphasis is on the aspect ratio effect on shock-<span class="hlt">elliptic</span> cylinder interaction. Experiments are conducted at five different aspect ratios (the ratio of length in streamwise and spanwise directions) varied from 0.25 to 4.0. PIV raw images and quantitative flow field data are obtained at t = 0.6 ms after the shock impact. As the aspect ratio increases, the interface morphology develops faster owing to more vorticity produced along the interface and smaller vortex spacing between the two vortex cores. For each case in this study, the maximal fluctuating velocity locates at the middle point of the two counter-vortices. The histograms of fluctuating velocity reveal that a distinct double-peak structure appears in the largest aspect ratio case in comparison with a single-peak structure in the smallest aspect ratio case. The vortex velocities predicted by the theoretical model [G. Rudinger and L. M. Somers, "Behaviour of small regions of different gases carried in accelerated gas flows," J. Fluid Mech. 7, 161-176 (1960)] agree well with the experimental ones. With the increase of aspect ratio, the maximal value of vorticity increases as well as the circulation, and more low-magnitude quantities are generated, which indicates the formation of multi-scale flow structure in the late mixing process. It is found that the experimental circulation of the vortex motion is reasonably estimated by the ideal point vortex-pair model.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.ncbi.nlm.nih.gov/pubmed/27810692','PUBMED'); return false;" href="https://www.ncbi.nlm.nih.gov/pubmed/27810692"><span id="translatedtitle">Kinematic and muscle demand similarities between motor-assisted <span class="hlt">elliptical</span> training and walking: Implications for pediatric gait rehabilitation.</span></a></p> <p><a target="_blank" href="https://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p>Burnfield, Judith M; Cesar, Guilherme M; Buster, Thad W; Irons, Sonya L; Nelson, Carl A</p> <p>2017-01-01</p> <p>Many children with physical disabilities and special health care needs experience barriers to accessing effective therapeutic technologies to improve walking and fitness in healthcare and community environments. The expense of many robotic and exoskeleton technologies hinders widespread use in most clinics, school settings, and fitness facilities. A motor-assisted <span class="hlt">elliptical</span> trainer that is being used to address walking and fitness deficits in adults was modified to enable children as young as three years of age to access the technology (Pedi-ICARE). We compared children's kinematic and muscle activation patterns during walking and training on the Pedi-ICARE. Eighteen children walked (self-selected comfortable speed), Pedi-ICARE trained with motor-assistance at self-selected comfortable speed (AAC), and trained while over-riding motor-assistance (AAC+). Coefficient of multiple <span class="hlt">correlations</span> (CMCs) compared lower extremity kinematic profiles during AAC and AAC+ to gait. Repeated measures ANOVAs identified muscle demand differences across conditions. CMCs revealed strong similarities at the hip and knee between each motor-assisted <span class="hlt">elliptical</span> condition and gait. Ankle CMCs were only moderate. Muscle demands were generally lowest during AAC. Over-riding the motor increased hip and knee muscle demands. The similarity of motion patterns between Pedi-ICARE conditions and walking suggest the device could be used to promote task-specific training to improve walking. The capacity to manipulate muscle demands using different motor-assistance conditions highlights Pedi-ICARE's versatility in addressing a wide range of children's abilities.</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://eric.ed.gov/?q=motivation+AND+employees&pg=3&id=EJ680938','ERIC'); return false;" href="http://eric.ed.gov/?q=motivation+AND+employees&pg=3&id=EJ680938"><span id="translatedtitle">Organisational Learning and Employees' <span class="hlt">Intrinsic</span> Motivation</span></a></p> <p><a target="_blank" href="http://www.eric.ed.gov/ERICWebPortal/search/extended.jsp?_pageLabel=advanced">ERIC Educational Resources Information Center</a></p> <p>Remedios, Richard; Boreham, Nick</p> <p>2004-01-01</p> <p>This study examined the effects of organisational learning initiatives on employee motivation. Four initiatives consistent with theories of organisational learning were a priori ranked in terms of concepts that underpin <span class="hlt">intrinsic</span>-motivation theory. Eighteen employees in a UK petrochemical company were interviewed to ascertain their experiences of…</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://eric.ed.gov/?q=overseas+AND+student&pg=2&id=EJ790164','ERIC'); return false;" href="http://eric.ed.gov/?q=overseas+AND+student&pg=2&id=EJ790164"><span id="translatedtitle"><span class="hlt">Intrinsic</span> Factors Affecting Overseas Student Teaching</span></a></p> <p><a target="_blank" href="http://www.eric.ed.gov/ERICWebPortal/search/extended.jsp?_pageLabel=advanced">ERIC Educational Resources Information Center</a></p> <p>Firmin, Michael W.; MacKay, Brenda B.; Firmin, Ruth L.</p> <p>2007-01-01</p> <p>We conducted a qualitative research study involving 13 undergraduate students who completed their student-teaching in overseas contexts. Participants completed two waves of interviews immediately after returning to campus from their multicultural experiences. Three <span class="hlt">intrinsic</span> factors were found to have the greatest impact on students' overseas…</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('http://eric.ed.gov/?q=extrinsic+AND+intrinsic+AND+motivation&pg=4&id=EJ898306','ERIC'); return false;" href="http://eric.ed.gov/?q=extrinsic+AND+intrinsic+AND+motivation&pg=4&id=EJ898306"><span id="translatedtitle"><span class="hlt">Intrinsic</span> and Extrinsic Motivation among Collegiate Instrumentalists</span></a></p> <p><a target="_blank" href="http://www.eric.ed.gov/ERICWebPortal/search/extended.jsp?_pageLabel=advanced">ERIC Educational Resources Information Center</a></p> <p>Diaz, Frank M.</p> <p>2010-01-01</p> <p>The purpose of this study was to gather and compare information on measures of <span class="hlt">intrinsic</span> and extrinsic motivation among instrumentalists enrolled in collegiate ensembles. A survey instrument was developed to gather information concerning demographic data and responses to questions on motivational preference. Participants were undergraduate and…</p> </li> <li> <p><a target="_blank" onclick="trackOutboundLink('https://www.osti.gov/scitech/biblio/5832812','SCIGOV-STC'); return false;" href="https://www.osti.gov/scitech/biblio/5832812"><span id="translatedtitle">Electroneutral <span class="hlt">intrinsic</span> point defects in cadmium chalcogenides</span></a></p> <p><a target="_blank" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p>Kharif, Ya.L.; Kudryashov, N.I.; Strunilina, T.A.</p> <p>1987-12-01</p> <p>Low-mobility electrically neutral <span class="hlt">intrinsic</span> point defects were observed in cadmium chalcogenides. It was shown that the concentration of these defects is proportional to the cadmium vapor pressure to the 1/3 power at a constant temperature, and a mechanism for the formation of these defects were proposed.</p> </li> </ol> <div class="pull-right"> <ul class="pagination"> <li><a href="#" onclick='return showDiv("page_1");'>«</a></li> <li><a href="#" onclick='return showDiv("page_21");'>21</a></li> <li><a href="#" onclick='return showDiv("page_22");'>22</a></li> <li><a href="#" onclick='return showDiv("page_23");'>23</a></li> <li><a href="#" onclick='return showDiv("page_24");'>24</a></li> <li class="active"><span>25</span></li> <li><a href="#" onclick='return showDiv("page_25");'>»</a></li> </ul> </div> </div><!-- col-sm-12 --> </div><!-- row --> </div><!-- page_25 --> <center> <div class="footer-extlink text-muted"><small>Some links on this page may take you to non-federal websites. Their policies may differ from this site.</small> </div> </center> <div id="footer-wrapper"> <div class="footer-content"> <div id="footerOSTI" class=""> <div class="row"> <div class="col-md-4 text-center col-md-push-4 footer-content-center"><small><a href="http://www.science.gov/disclaimer.html">Privacy and Security</a></small> <div class="visible-sm visible-xs push_footer"></div> </div> <div class="col-md-4 text-center col-md-pull-4 footer-content-left"> <img src="https://www.osti.gov/images/DOE_SC31.png" alt="U.S. Department of Energy" usemap="#doe" height="31" width="177"><map style="display:none;" name="doe" id="doe"><area shape="rect" coords="1,3,107,30" href="http://www.energy.gov" alt="U.S. Deparment of Energy"><area shape="rect" coords="114,3,165,30" href="http://www.science.energy.gov" alt="Office of Science"></map> <a ref="http://www.osti.gov" style="margin-left: 15px;"><img src="https://www.osti.gov/images/footerimages/ostigov53.png" alt="Office of Scientific and Technical Information" height="31" width="53"></a> <div class="visible-sm visible-xs push_footer"></div> </div> <div class="col-md-4 text-center footer-content-right"> <a href="http://www.osti.gov/nle"><img src="https://www.osti.gov/images/footerimages/NLElogo31.png" alt="National Library of Energy" height="31" width="79"></a> <a href="http://www.science.gov"><img src="https://www.osti.gov/images/footerimages/scigov77.png" alt="science.gov" height="31" width="98"></a> <a href="http://worldwidescience.org"><img src="https://www.osti.gov/images/footerimages/wws82.png" alt="WorldWideScience.org" height="31" width="90"></a> </div> </div> </div> </div> </div> <p><br></p> </div><!-- container --> </body> </html>