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1

Pulsatory Patterns in Active Fluids  

NASA Astrophysics Data System (ADS)

We show that pulsatory patterns arise in thin active films in which two chemical species regulate active stress. The regulating species diffuse within the film and are advected by self-generated flows resulting from active stress gradients. Spontaneous pulsatory patterns emerge when the following conditions are met: (i) the fast-diffusing species up-regulates and the slow-diffusing species down-regulates active stress, or (ii) the active stress up-regulator turns over faster compared to the active stress down-regulator. Our study, motivated by pulsatory patterns in the actomyosin cortex in cells and tissues, provides a simple generic mechanism for oscillatory patterns in active fluids.

Kumar, K. Vijay; Bois, Justin S.; Jülicher, Frank; Grill, Stephan W.

2014-05-01

2

Quasi-Periodic Hopf Bifurcation.  

National Technical Information Service (NTIS)

In the paper, the authors study quasi-periodic Hopf bifurcations for the model problem of a quasi-periodically forced oscillator, where the frequencies remain fixed. For this purpose, they first consider Stoker's problem for small damping.

B. L. J. Braaksma H. W. Broer

1985-01-01

3

Talbot effect of quasi-periodic grating.  

PubMed

Theoretic and experimental studies of the Talbot effect of quasi-periodic gratings are performed in this paper. The diffractions of periodic and quasi-periodic square aperture arrays in Fresnel fields are analyzed according to the scalar diffraction theory. The expressions of the diffraction intensities of two types of quasi-periodic gratings are deduced. Talbot images of the quasi-periodic gratings are predicted to appear at multiple certain distances. The quasi-periodic square aperture arrays are produced with the aid of a liquid crystal light modulator, and the self-images of the quasi-periodic gratings are measured successfully in the experiment. This study indicates that even a structure in short-range disorder may take on the self-imaging effect in a Fresnel field. PMID:23872752

Zhang, Chong; Zhang, Wei; Li, Furui; Wang, Junhong; Teng, Shuyun

2013-07-20

4

Toward a Quasi-Periodic Bifurcation Theory,  

National Technical Information Service (NTIS)

The subject of the paper concerns families of dynamical systems having invariant tori with parallel and, more specifically, quasi-periodic motion. In particular, questions are posed of stability (persistence) and, more importantly, bifurcation. The settin...

B. L. J. Braaksma H. W. Broer G. B. Huitema

1988-01-01

5

Quasi Periodicity in Local Bifurcation Theory.  

National Technical Information Service (NTIS)

The paper presents an overview of some results obtained recently in the local theory of bifurcations of dynamical systems, which are concerned with quasi periodic flow. With this 'local theory' we here mean the qualitative (topological) behavior of parame...

H. W. Broer

1982-01-01

6

Quasi-periodic solutions of a quasi-periodically forced nonlinear beam equation  

NASA Astrophysics Data System (ADS)

In this paper, one quasi-periodically forced nonlinear beam equation utt+uxxxx+?u+?g(?t,x)u3=0,?>0,x?[0,?] with hinged boundary conditions is considered. Here ? is a small positive parameter, g( ?t, x) is real analytic in all variables and quasi-periodic in t with a frequency vector ? = ( ?1, ?2, … , ?m). It is proved that the above equation admits small-amplitude quasi-periodic solutions.

Wang, Yi

2012-06-01

7

Quasi-periodically forced nonlinear Helmholtz oscillators  

Microsoft Academic Search

In this paper we study a model that describes the dynamics of the tidal elevation within an almost-enclosed short basin that is connected to a tidal sea by a narrow strait. This model has the form of a forced nonlinear Helmholtz oscillator. The forcing is prescribed by the tide at sea and has a quasi-periodic character of a special nature,

Arjen Doelman; A. Femius Koenderink; Leo R. M. Maasc

8

Quasi-periodic quantum dot arrays produced by electrochemical synthesis.  

National Technical Information Service (NTIS)

We discuss a ''gentle'' electrochemical technique for fabricating quasi-periodic quantum dot arrays. The technique exploits a self-organizing phenomenon to produce quasi-periodic arrangement of dots and provides excellent control over dot size and interdo...

S. Bandyopadhyay A. E. Miller D. F. Yue G. Banerjee R. E. Ricker

1994-01-01

9

Quasi-periodic oscillations in superfluid magnetars  

NASA Astrophysics Data System (ADS)

We study the time evolution of axisymmetric oscillations of superfluid magnetars with a poloidal magnetic field and an elastic crust, working in Newtonian gravity. Extending earlier models, we study the effects of composition gradients and entrainment on the magneto-elastic wave spectrum and on the potential identification of the observed quasi-periodic oscillations (QPOs). We use two-fluid polytropic equations of state to construct our stellar models, which mimic realistic composition gradient configurations. The basic features of the axial axisymmetric spectrum of normal fluid stars are reproduced by our results and in addition we find several magneto-elastic waves with a mixed character. In the core, these oscillations mimic the shear mode pattern of the crust as a result of the strong dynamical coupling between these two regions. Incorporating the most recent entrainment configurations in our models, we find that they have a double effect on the spectrum: the magnetic oscillations of the core have a frequency enhancement, while the mixed magneto-elastic waves originating in the crust are moved towards the frequencies of the single-fluid case. The distribution of lower frequency magneto-elastic oscillations for our models is qualitatively similar to the observed magnetar QPOs with ? < 155 Hz. In particular, some of these QPOs could represent mixed magneto-elastic oscillations with frequencies not greatly different from the crustal modes of an unmagnetized star. We find that many QPOs could even be accounted for using a model with a relatively weak polar field of Bp ? 3 × 1014 G, because of the superfluid enhancement of magnetic oscillations. Finally, we discuss the possible identification of 625 and 1837 Hz QPOs either with non-axisymmetric modes or with high-frequency axisymmetric QPOs excited by crustal mode overtones.

Passamonti, A.; Lander, S. K.

2014-02-01

10

Embedding of Analytic Quasi-Periodic Cocycles into Analytic Quasi-Periodic Linear Systems and its Applications  

NASA Astrophysics Data System (ADS)

In this paper, we prove that any analytic quasi-periodic cocycle close to constant is the Poincaré map of an analytic quasi-periodic linear system close to constant, which bridges both methods and results in quasi-periodic linear systems and cocycles. We also show that the almost reducibility of an analytic quasi-periodic linear system is equivalent to the almost reducibility of its corresponding Poincaré cocycle. By the local embedding theorem and the equivalence, we transfer the recent local almost reducibility results of quasi-periodic linear systems (Hou and You, in Invent Math 190:209-260, 2012) to quasi-periodic cocycles, and the global reducibility results of quasi-periodic cocycles (Avila, in Almost reducibility and absolute continuity, 2010; Avila et al., in Geom Funct Anal 21:1001-1019, 2011) to quasi-periodic linear systems. Finally, we give a positive answer to a question of Avila et al. (Geom Funct Anal 21:1001-1019, 2011) and use it to study point spectrum of long-range quasi-periodic operator with Liouvillean frequency. The embedding also holds for some nonlinear systems.

You, Jiangong; Zhou, Qi

2013-11-01

11

Characteristics of quasi-periodic scintillations observed at low latitude  

NASA Astrophysics Data System (ADS)

Quasi-periodic scintillations are characterized as primary deep fadeout in field strength, associated with regular ringing patterns before and after it. In this paper, observations of quasi-periodic scintillations using geostationary satellite (FLEETSAT) transmissions operating at frequency 250 MHz at low-latitude ground station, Varanasi (geomagnetic latitude 14°55'N, longitude 153°59'E), are reported. The results indicate that the quasi-periodic scintillations are most likely produced by plasma blobs/bubbles present in the E and F regions of the ionosphere which are helpful in identifying the generation mechanism of the associated irregularities. The various characteristic features of the different types of quasi-periodic scintillations observed at low latitude are discussed for the first time in detail based on a highly comprehensive analysis of longer data sets using autocorrelation, power spectrum, and scintillation index analysis. The computed horizontal scale size of the quasi-periodic scintillations producing irregularity varies from 100 to 1300 m which shows that the irregularities are of intermediate-scale sizes. The spectral index obtained from the slopes of power spectrum varies from -2 to -8. All of these observed results are important for identifying the generation mechanism of ionospheric irregularities associated with quasi-periodic scintillations. The observed fading patterns, especially the modulation of the diffraction patterns (fading envelopes), can be explained by considering an obstacle called radio lens in the ionosphere elongated in one direction. For the first time, we have successfully simulated the amplitude versus time plots of almost all types of quasi-periodic scintillation patches and found that our modeled and observed characteristics of quasi-periodic scintillation patches compare well with each other.

Patel, Kalpana; Singh, Ashutosh K.; Singh, A. K.; Singh, R. P.

2009-12-01

12

Quasi-periodic solutions of forced isochronous oscillators at resonance  

NASA Astrophysics Data System (ADS)

We deal with the existence of quasi-periodic solutions of forced isochronous oscillators with a repulsive singularity, the nonlinearity is a bounded perturbation. Using a variant of Moser's twist theorem of invariant curves, due to Ortega [R. Ortega, Boundedness in a piecewise linear oscillator and a variant of the small twist theorem, Proc. London Math. Soc. 79 (1999) 381-413], we show that there are many quasi-periodic solutions and the boundedness of all solutions.

Liu, Bin

13

The Ten-Rotation Quasi-periodicity in Sunspot Areas  

NASA Astrophysics Data System (ADS)

Sunspot-area fluctuations over an epoch of 12 solar cycles (12 - 23) are investigated in detail using wavelets. Getko ( Universal Heliophysical Processes, IAU Symp. 257, 169, 2009) found three significant quasi-periodicities at 10, 17, and 23 solar rotations, but two longer periods could be treated as subharmonics of the ten-rotation quasi-periodicity. Therefore we focused the analysis on the occurrence of this quasi-periodicity during the low- and high-activity periods of each solar cycle. Because of the N - S asymmetry, each solar hemisphere was considered separately. The skewness of each fluctuation-probability distribution suggests that the positive and negative fluctuations could be examined separately. To avoid the problem that occurs when a few strong fluctuations create a wavelet peak, we applied fluctuation transformations for which the amplitudes at the high- and the low-activity periods are almost the same. The wavelet analyses show that the ten-rotation quasi-periodicity is mainly detected during the high-activity periods, but it also exists during a few low-activity periods. The division of each solar hemisphere into 30?-wide longitude bins and the wavelet calculations for the areas of sunspot clusters belonging to these 30? bins enable one to detect longitude zones in which the ten-rotation quasi-periodicity exists. These zones are present during the whole high-activity periods and dominate the integrated spectra.

Getko, R.

2014-06-01

14

Pressure-driven reconnection and quasi periodical oscillations in plasmas  

NASA Astrophysics Data System (ADS)

This paper presents a model for an ohmically heated plasma in which a feedback exists between thermal conduction and transport, on one side, and the magneto-hydro-dynamical stability of the system, on the other side. In presence of a reconnection threshold for the magnetic field, a variety of periodical or quasi periodical oscillations for the physical quantities describing the system are evidenced. The model is employed to interpret the observed quasi periodical oscillations of electron temperature and perturbed magnetic field around the so called "Single Helical" state in the reversed field pinch, but its relevance for other periodical phenomena observed in magnetic confinement systems, especially in tokamaks, is suggested.

Paccagnella, R.

2014-03-01

15

A result on quasi-periodic solutions of a nonlinear beam equation with a quasi-periodic forcing term  

NASA Astrophysics Data System (ADS)

In this paper, a quasi-periodically forced nonlinear beam equation {u_{tt}+u_{xxxx}+? u+\\varepsilon?(t)h(u)=0} with hinged boundary conditions is considered, where ? > 0, {\\varepsilon} is a small positive parameter, {?} is a real analytic quasi-periodic function in t with a frequency vector ? = ( ? 1, ? 2 . . . , ? m ), and the nonlinearity h is a real analytic odd function of the form {h(u)=?_1u+?_{2bar{r}+1}u^{2bar{r}+1}+sum_{k? bar{r}+1}?_{2k+1}u^{2k+1},?_1,?_{2bar{r}+1} neq0, bar{r} in {mathbb {N}}.} The above equation admits a quasi-periodic solution.

Wang, Yi; Si, Jianguo

2012-02-01

16

Scattering Theory for Jacobi Operators with Quasi-Periodic Background  

NASA Astrophysics Data System (ADS)

We develop direct and inverse scattering theory for Jacobi operators which are short range perturbations of quasi-periodic finite-gap operators. We show existence of transformation operators, investigate their properties, derive the corresponding Gel'fand-Levitan-Marchenko equation, and find minimal scattering data which determine the perturbed operator uniquely.

Egorova, Iryna; Michor, Johanna; Teschl, Gerald

2006-06-01

17

Construction of Quasi-Periodic Breathersvia KAM Technique  

NASA Astrophysics Data System (ADS)

By developing a KAM theorem which involves an infinitely multiple normal frequency, it is shown that there are plenty of breathers, quasi-periodic in time and super-exponentially localized in space, for the networks of weakly coupled oscillators. This answers an open problem by Aubry [A2] in case the linearized system has no continuous spectrum.

Yuan, Xiaoping

18

TT Ari and its Quasi-Periodic Oscillations  

NASA Astrophysics Data System (ADS)

Quasi-periodic oscillation (QPO) of TT Ari are transient, short-lived phenomena. They appear and disappear and their periods and amplitudes vary on a time scale as short as 1 hour. Consequently the periodograms covering longer intervals of time are generally meaningless.

Smak, J.

2014-06-01

19

Normal linear stability of quasi-periodic tori  

NASA Astrophysics Data System (ADS)

We consider families of dynamical systems having invariant tori that carry quasi-periodic motions. Our interest is the persistence of such tori under small, nearly-integrable perturbations. This persistence problem is studied in the dissipative, the Hamiltonian and the reversible setting, as part of a more general KAM theory for classes of structure preserving dynamical systems. This concerns the parametrized KAM theory as initiated by Moser [J.K. Moser, On the theory of quasiperiodic motions, SIAM Rev. 8 (2) (1966)145-172; J.K. Moser, Convergent series expansions for quasi-periodic motions, Math. Ann. 169 (1967) 136-176] and further developed in [G.B. Huitema, Unfoldings of quasi-periodic tori, PhD thesis, University of Groningen, 1988; H.W. Broer, G.B. Huitema, F. Takens, Unfoldings of quasi-periodic tori, Mem. Amer. Math. Soc. 83 (421) (1990) 1-82; H.W. Broer, G.B. Huitema, Unfoldings of quasi-periodic tori in reversible systems, J. Dynam. Differential Equations 7 (1) (1995) 191-212]. The corresponding nondegeneracy condition involves certain (trans-)versality conditions on the normal linear, leading, part at the invariant tori. We show that as a consequence, a Cantor family of Diophantine tori with positive Hausdorff measure is persistent under nearly-integrable perturbations. This result extends the above references since presently the case of multiple Floquet exponents is included. Our leading example is the normal 1 :-1 resonance, which occurs a lot in applications, both Hamiltonian and reversible. As an illustration of this we briefly describe the Lagrange top coupled to an oscillator.

Broer, H. W.; Hoo, J.; Naudot, V.

20

Quasi-periodic quantum dot arrays produced by electrochemical synthesis  

SciTech Connect

We discuss a ``gentle`` electrochemical technique for fabricating quasi-periodic quantum dot arrays. The technique exploits a self-organizing phenomenon to produce quasi-periodic arrangement of dots and provides excellent control over dot size and interdot spacing. Unlike conventional nanolithography, it does not cause radiation damage to the structures during exposure to pattern delineating beams (e-beam, ion-beam or x-ray). Moreover, it does not require harsh processing steps like reactive ion etching, offers a minimum feature size of {approximately}40 {angstrom}, allows the fabrication of structures on nonplanar surfaces (e.g. spherical or cylindrical substrates), is amenable to mass production (millions of wafers can be processed simultaneously) and is potentially orders of magnitude cheaper than conventional nanofabrication. In this paper, we describe our initial results and show the promise of this technique for low-cost and high-yield nanosynthesis.

Bandyopadhyay, S.; Miller, A.E.; Yue, D.F.; Banerjee, G. [Univ. of Notre Dame, Notre Dame, IN (United States). Dept. of Electrical Engineering; Ricker, R.E.; Jones, S. [National Inst. of Standards and Technology, Gaithersburg, MD (United States). Materials Science and Engineering Laboratory; Eastman, J.A. [Argonne National Lab., IL (United States); Baugher, E.; Chandrasekhar, M. [Univ. of Missouri-Columbia, Columbia, MS (United States). Dept. of Physics and Astronomy

1994-06-01

21

Anderson Localization for Time Quasi Periodic Random Sch\\\\\\  

Microsoft Academic Search

We prove that at large disorder, with large probability and for a set of\\u000aDiophantine frequencies of large measure, Anderson localization in $\\\\Bbb Z^d$\\u000ais {\\\\it stable} under localized time-quasi-periodic perturbations by proving\\u000athat the associated quasi-energy operator has pure point spectrum. The main\\u000atools are the Fr\\\\\\

Jean Bourgain; Wei-Min Wang

2002-01-01

22

Quasi-periodic orbits about the translunar libration point  

Microsoft Academic Search

Analytical solutions for quasi-periodic orbits about the translunar libration point are obtained by using the method of Lindstedt-Poincaré and computerized algebraic manipulations. The solutions include the effects of nonlinearities, lunar orbital eccentricity, and the Sun's gravitational field. For a small-amplitude orbit, the orbital path as viewed from the Earth traces out a Lissajous figure. This is due to a small

Robert W. Farquhar; Ahmed A. Kamel

1973-01-01

23

Quasi-periodic vertical structures of dusty plasma crystals  

Microsoft Academic Search

A semi-analytical model is proposed for understanding the quasi-periodic vertical structures in a plasma crystal, which are shown to be sustained by the combined effects of an ion flow, gravity and horizontal bonds of the dust particles. These structures are the manifestations of large-amplitude standing wake fields that lead to strong vertical bonds for the formation of an oriented hexagonal

Tzihong Chiueh; D. Ming-Ting Kuo

1999-01-01

24

Quasi-periodic modulations of the Jovian magnetotail  

Microsoft Academic Search

Measurements with the Energetic Particles Detector (EPD) on Galileo orbit C9 in the Jovian magnetotail revealed the existence of distinct quasi-periodic variations of energetic ion intensities which are superimposed on the well-known 10-hour modulations due to the planetary rotation. The intensity variations are associated with changes of the particle energy spectra and the plasma flow pattern. They are clearly of

J. Woch; N. Krupp; A. Lagg; B. Wilken; S. Livi; D. J. Williams

1998-01-01

25

Explicit quasi-periodic solutions of the Vakhnenko equation  

NASA Astrophysics Data System (ADS)

The trigonal curve associated with the Vakhnenko equation is introduced by using the Lax matrix for the nth stationary positive flow. Based on the theory of the trigonal curve and the properties of the three kinds of Abel differentials, the Riemann theta function representation for the Baker-Akhiezer function is derived, from which the straightening out of flows in the Jacobian variety is exactly given through the Abel maps. We finally arrive at quasi-periodic solutions of the Vakhnenko equation.

Zhai, Yunyun; Geng, Xianguo; He, Guoliang

2014-05-01

26

QUASI-PERIODIC OSCILLATIONS IN LASCO CORONAL MASS EJECTION SPEEDS  

SciTech Connect

Quasi-periodic oscillations in the speed profile of coronal mass ejections (CMEs) in the radial distance range 2-30 solar radii are studied. We considered the height-time data of the 307 CMEs recorded by the Large Angle and Spectrometric Coronagraph (LASCO) during 2005 January-March. In order to study the speed-distance profile of the CMEs, we have used only 116 events for which there are at least 10 height-time measurements made in the LASCO field of view. The instantaneous CME speed is estimated using a pair of height-time data points, providing the speed-distance profile. We found quasi-periodic patterns in at least 15 speed-distance profiles, where the speed amplitudes are larger than the speed errors. For these events we have determined the speed amplitude and period of oscillations. The periods of quasi-periodic oscillations are found in the range 48-240 minutes, tending to increase with height. The oscillations have similar properties as those reported by Krall et al., who interpreted them in terms of the flux-rope model. The nature of forces responsible for the motion of CMEs and their oscillations are discussed.

Shanmugaraju, A. [Department of Physics, Arul Anandar College, Karumathur-625 514 (India); Moon, Y.-J. [School of Space Research, Kyung Hee University, Yongin 446-701 (Korea, Republic of); Cho, K.-S.; Bong, S. C. [Korea Astronomy and Space Science Institute (KASI), Whaamdong, Yuseong-gu, Daejeon, 305-348 (Korea, Republic of); Gopalswamy, N.; Akiyama, S.; Yashiro, S. [NASA Goddard Space Flight Center, Greenbelt, MD (United States); Umapathy, S. [School of Physics, Madurai Kamaraj University, Madurai (India); Vrsnak, B., E-mail: shanmugaraju_a@yahoo.co, E-mail: moonyj@khu.ac.k [Hvar Observatory, Faculty of Geodesy, Zagreb (Croatia)

2010-01-01

27

Overall ultimate yield strength of a quasi-periodic masonry  

NASA Astrophysics Data System (ADS)

The purpose of this Note is the determination of the in-plane homogenized strength domain of a "quasi-periodic" masonry under the assumption of infinitely resistant blocks connected by cohesionless Mohr-Coulomb interfaces. This masonry is obtained by introducing a random perturbation on the horizontal width of the blocks of a periodic running bond masonry. It is found that in some non-trivial cases the strength domain coincides exactly with that of the initial periodic masonry. To cite this article: K. Sab, C. R. Mecanique 337 (2009).

Sab, Karam

2009-08-01

28

The quasi-periodicity of the minority game revisited  

NASA Astrophysics Data System (ADS)

We analyze two well-known related aspects regarding the sequence of minority sides from the Minority Game (MG) in its symmetric phase: period-two dynamics and quasi-periodic behavior. We also study the sequence of minority sides in a general way within a graph-theoretical framework. In order to analyze the outcome dynamics of the MG, it is useful to define the MG, namely an MG with a new choosing rule of the strategy to play, which takes into account both prior preferences and game information. In this way, each time an agent is undecided because two of her best strategies predict different choices while being equally successful so far, she selects her a priori favorite strategy to play, instead of performing a random tie-break as in the MG. This new choosing rule leaves the generic behavior of the model unaffected and simplifies the game analysis. Furthermore, interesting properties arise which are only partially present in the MG, like the quasi-periodic behavior of the sequence of minority sides, which turns out to be periodic for the MG.

Acosta, Gabriel; Caridi, Inés; Guala, Sebastián; Marenco, Javier

2013-10-01

29

Quasi-periodic Solutions of the Kaup-Kupershmidt Hierarchy  

NASA Astrophysics Data System (ADS)

Based on solving the Lenard recursion equations and the zero-curvature equation, we derive the Kaup-Kupershmidt hierarchy associated with a 3×3 matrix spectral problem. Resorting to the characteristic polynomial of the Lax matrix for the Kaup-Kupershmidt hierarchy, we introduce a trigonal curve {K}_{m-1} and present the corresponding Baker-Akhiezer function and meromorphic function on it. The Abel map is introduced to straighten out the Kaup-Kupershmidt flows. With the aid of the properties of the Baker-Akhiezer function and the meromorphic function and their asymptotic expansions, we arrive at their explicit Riemann theta function representations. The Riemann-Jacobi inversion problem is achieved by comparing the asymptotic expansion of the Baker-Akhiezer function and its Riemann theta function representation, from which quasi-periodic solutions of the entire Kaup-Kupershmidt hierarchy are obtained in terms of the Riemann theta functions.

Geng, Xianguo; Wu, Lihua; He, Guoliang

2013-08-01

30

Quasi-periodic orbits about the translunar libration point.  

NASA Technical Reports Server (NTRS)

Analytical solutions for quasi-periodic orbits about the translunar libration point are obtained by using the method of Lindstedt-Poincare and computerized algebraic manipulations. The solutions include the effects of nonlinearities, lunar orbital eccentricity, and the sun's gravitational field. For a small-amplitude orbit, the orbital path as viewed from the earth traces out a Lissajous figure. This is due to a small difference in the fundamental frequencies of the in-plane and out-of-plane oscillations. However, when the amplitude of the in-plane oscillation is greater than 32,379 km, there is a corresponding value of the out-of-plane amplitude that will produce a path where the fundamental frequencies are equal. This synchronized trajectory describes a 'halo orbit' of the moon.

Farquhar, R. W.; Kamel, A. A.

1972-01-01

31

Quasi-periodic orbits about the translunar libration point.  

NASA Technical Reports Server (NTRS)

Analytical solutions for quasi-periodic orbits about the translunar libration point are obtained by using the method of Lindstedt-Poincare and computerized algebraic manipulations. The solutions include the effects of nonlinearities, lunar orbital eccentricity, and the sun's gravitational field. For a small-amplitude orbit, the orbital path as viewed from the earth traces out a Lissajous figure. This is due to a small difference in the fundamental frequencies of the in-plane and out-of-plane oscillations. However, when the amplitude of the in-plane oscillation is greater than 32,379 km, there is a corresponding value of the out-of-plane amplitude that will produce a path where the fundamental frequencies are equal. This synchronized trajectory describes a 'halo orbit' of the moon.

Farquhar, R. W.; Kamel, A. A.

1973-01-01

32

Search for Quasi-Periodic Oscillations in Quasars and AGNS  

NASA Astrophysics Data System (ADS)

Quasars and Active galaxies such OJ287 RX J0437.4-4711 exhibit variabilities in a wide range of time-scales and in almost all the wavelengths. We show that some of these variabilities are periodic and have similarities with the Quasi-periodic oscillations of their micro-quasar counterparts such as GRS1915+105 Cyg. X1 GRO J1655-40 etc. Only difference is that the periodicity scales with the mass of the central engine. We explain these QPOs in terms of the oscillation of standing shocks around the central black holes. Our work conclusively proves that the physical phenomena around stellar mass and supermassive black holes are similar.

Nandi, Anuj; Chakrabarti, Sandip K.

33

Quasi-periodic oscillations in GX 17 + 2  

NASA Technical Reports Server (NTRS)

X-ray observations of GX 17 + 2 were made in March and April, 1988 with the Large Area Counter of the Ginga satellite. The source was observed in the flaring, normal, and horizontal branches. Quasi-periodic oscillations (QPOs) were oberved in all three of these branches. The relationship between QPO behavior and the X-ray spectral properties of GX 17 + 2 is examined. Continuous variation of QPO behavior is observed as GX 17 + 2 moves from the normal to flaring branch, indicating that the normal-branch QPO and the flaring-branch QPO are probably one physical phenomenon. This QPO behavior is similar to that observed in Sco X-1. Also, it is found that GX 17 + 2 is an example of the Z-type sources defined by Hasinger et al. (1989).

Penninx, W.; Lewin, W. H. G.; Mitsuda, K.; Van Der Klis, M.; Van Paradijs, J.

1990-01-01

34

Aperiodic and Quasi-Periodic Variability in Scorpius X-1  

NASA Astrophysics Data System (ADS)

Low mass X-ray binary star systems (LMXBs) are among the brightest and most well-studied objects in the X-ray sky-indeed, the first extrasolar X-ray source discovered, Sco X-1, is an LMXB. But despite the wealth of available data, LMXBs remain enigmatic, in large part due to the fact that they show little or no coherent periodicity. LMXBs show aperiodic and quasi-periodic variability, for which the underlying mechanisms are poorly understood. Much information remains locked in archival data. Here we address this issue by re-analyzing archival EXOSAT data of Sco X-1 using modern time-series techniques, including multi-tapering, wavelet transforms and scalegrams, and nonlinear dynamical modelling, which are not yet commonly used in the analysis of astronomical data, with the goal of characterizing Sco X-1's variability and developing a formalism to take us from timing data to mathematical models to astrophysical models. The power spectra of Sco X-1 show several components: (i) very low frequency noise (VLFN), a colored noise component seen below ~0.25 Hz, (ii) high frequency noise (HFN), a colored noise component seen above ~30-40 Hz, and (iii) quasi-periodic oscillations (QPOs), localized excesses of Fourier power. The VLFN contains ~1.3% [1/over2]-peak-to-peak pulsed power on the average, can be described by a power law with an index of ~1.4, and is correlated with the 'flickeriness' of the source. QPOs contain ~4.6% [1/over2]-peak-to-peak pulsed power, have centroid frequencies of 6.7 Hz or 15 Hz, and are associated with extended 'quiescent' states and with brief gaps in 'flaring' states. HFN is difficult to characterize (though others have had success describing it as a damped power law), and is not strongly associated with any other source feature. It contains ~2.1% [1/over2]-peak-to-peak pulsed power. Several models have been proposed to explain the VLFN, QPOs, and HFN in Sco X-1, but none are completely satisfactory. Most models seek to explain only QPOs. Here we investigate the dripping handrail model (DHR), a nonlinear dynamical model. The DHR is a deterministic, spatially extended, diffusive model which shows a complex variety of behaviors including QPOs and transient chaos. It can reproduce the entire observed power spectra of Sco X-1, from 0.5 mHz to 128 Hz, including VLFN, QPOs, and HFN.

Parker, Neil Ivan

35

Quasi-periodic fluctuations in default mode network electrophysiology.  

PubMed

The study of human brain electrophysiology has extended beyond traditional frequency ranges identified by the classical EEG rhythms, encompassing both higher and lower frequencies. Changes in high-gamma-band (>70 Hz) power have been identified as markers of local cortical activity. Fluctuations at infra-slow (<0.1 Hz) frequencies have been associated with functionally significant cortical networks elucidated using fMRI studies. In this study, we examined infra-slow changes in band-limited power across a range of frequencies (1-120 Hz) in the default mode network (DMN). Measuring the coherence in band-limited power fluctuations between spatially separated electrodes makes it possible to detect small, spatially extended, and temporally coherent fluctuating components in the presence of much larger incoherent fluctuations. We show that the default network is characterized by significant high-gamma-band (65-110 Hz) coherence at infra-slow (<0.1 Hz) frequencies. This coherence occurs over a narrow frequency range, centered at 0.015 Hz, commensurate with the frequency of BOLD signal fluctuations seen by fMRI, suggesting that quasi-periodic, infra-slow changes in local cortical activity form the neurophysiological basis for this network. PMID:21832202

Ko, Andrew L; Darvas, Felix; Poliakov, Andrew; Ojemann, Jeffrey; Sorensen, Larry B

2011-08-10

36

Quasi-periodic vertical structures of dusty plasma crystals  

NASA Astrophysics Data System (ADS)

A semi-analytical model is proposed for understanding the quasi-periodic vertical structures in a plasma crystal, which are shown to be sustained by the combined effects of an ion flow, gravity and horizontal bonds of the dust particles. These structures are the manifestations of large-amplitude standing wake fields that lead to strong vertical bonds for the formation of an oriented hexagonal lattice. The orientational symmetry breaking is caused by a gravity-induced thick sheath, which can preferentially accelerate a supersonic ion flow in the vertical direction. The electron and streaming ion densities and the electric potential are found to be all in phase in the plasma crystal, whereas the dust density is 180 degrees out of phase. With each dust layer playing a similar role as the plasma wall, the Bohm sheath criterion is also found to be satisfied. Crystal melting may also be qualitatively described by the present model when the horizontal bonds of the dust particles are sufficiently weakened.

Chiueh, Tzihong; Ming-Ting Kuo, D.

1999-04-01

37

Peculiar microwave quasi-periodic pulsations with zigzag pattern in a CME-related Flare on 2005-01-15  

NASA Astrophysics Data System (ADS)

A microwave quasi-periodic pulsation with zigzag pattern (Z-QPP) in a solar flare on 2005-01-15 is observed by the Chinese Solar Broadband Spectrometer in Huairou (SBRS/Huairou) at 1.10-1.34 GHz. The zigzag pulsation occurred just in the early rising phase of the flare with weakly right-handed circular polarization. Its period is only several decades millisecond. Particularly, before and after the pulsation, there are many spectral fine structures, such as zebra patterns, fibers, and millisecond spikes. The microwave Z-QPP can provide some kinematic information of the source region in the early rising phase of the flare, and the source width changes from ~1000 km to 3300 km, even if we have no imaging observations. The abundant spectral fine structures possibly reflect the dynamic features of non-thermal particles.

Tan, Baolin

2013-07-01

38

Omnidirectional reflection from Fibonacci quasi-periodic one-dimensional photonic crystal  

NASA Astrophysics Data System (ADS)

It is shown that omnidirectional reflection (ODR) is possible from quasi-periodic isotropic dielectric stacks following a Fibonacci sequence (FS). The transition from truly periodic to fully quasi-periodic structure is investigated by building periodic structures having unit cells made of FS of order j. The number of periods required to achieve ODR decreases as j increases until only a single period is required at which the structure is fully quasi-periodic. As compared to the periodic case, for the quasi-periodic structure the spectral range is wider, the thickness of the single layers is smaller and the tolerance on the layer thicknesses is smaller.

Lusk, D.; Abdulhalim, I.; Placido, F.

2001-11-01

39

Are Flare Quasi-periodic Pulsations Signatures of Intermittent Reconnection?  

NASA Astrophysics Data System (ADS)

Flare quasi-periodic pulsations (QPPs) have been observed over a vast energy spectrum, from radio to hard x-rays. The periodicities of these fine structures range from tens of milliseconds to tens of seconds and suggest highly structured but intermittent energy release. In some cases, the sources of microwaves and thermal hard x-rays are situated near the apex of the flare loop arcades and are not stationary. Although it is unclear whether all the observed varieties of QPPs can be explained via a single, unified process, our recent high-resolution simulations of a breakout eruptive flare (Karpen et al. 2012) indicate that spatially and temporally localized reconnection is a plausible candidate for these bursts of radiation. With our null-tracking capabilities, we follow the creation and evolution of X- and O-type nulls in the flare current sheet and characterize their periodicity. QPPs located at the apex of the flare arcade may result from the interaction of downward-moving islands in the sheet with the arcade below. Each island is composed of highly twisted magnetic field lines that comprise a single reconnected flux tube. Upon arrival at the top of the flare loops, secondary reconnection events between the island and the arcade produce discrete energy release events that could be related to observed QPPs in that region. Different regimes of current-sheet reconnection (slow/fast), island sizes, rates of island coalescence, and rates of reconnection between islands and arcades may all help to explain the variety of energy and time scales exhibited by the flare QPPs.Abstract (2,250 Maximum Characters): Flare quasi-periodic pulsations (QPPs) have been observed over a vast energy spectrum, from radio to hard x-rays. The periodicities of these fine structures range from tens of milliseconds to tens of seconds and suggest highly structured but intermittent energy release. In some cases, the sources of microwaves and thermal hard x-rays are situated near the apex of the flare loop arcades and are not stationary. Although it is unclear whether all the observed varieties of QPPs can be explained via a single, unified process, our recent high-resolution simulations of a breakout eruptive flare (Karpen et al. 2012) indicate that spatially and temporally localized reconnection is a plausible candidate for these bursts of radiation. With our null-tracking capabilities, we follow the creation and evolution of X- and O-type nulls in the flare current sheet and characterize their periodicity. QPPs located at the apex of the flare arcade may result from the interaction of downward-moving islands in the sheet with the arcade below. Each island is composed of highly twisted magnetic field lines that comprise a single reconnected flux tube. Upon arrival at the top of the flare loops, secondary reconnection events between the island and the arcade produce discrete energy release events that could be related to observed QPPs in that region. Different regimes of current-sheet reconnection (slow/fast), island sizes, rates of island coalescence, and rates of reconnection between islands and arcades may all help to explain the variety of energy and time scales exhibited by the flare QPPs.

Guidoni, Silvina; Karpen, J. T.; DeVore, C. R.

2013-07-01

40

Quasi-Periodicities, Magnetic Clusters and Solar Activity  

NASA Astrophysics Data System (ADS)

To investigate quasi-periodicities, 12 hour averages of the radial component of the interplanetary magnetic field and the solar wind speed, covering ~ 42 (1963-2005) years were analyzed. A Lomb periodogram for data up to 1998 showed a dominant period of 27.03 days as fpund in earlier results. Including cycle 23, a dominant period of 27.06 days was identified. Analysis of the solar cycles independently showed a dominant period of 27.03 days in solar cycle 20, but not in the other cycles. To investigate the degree of persistency of a particular signal, the technique of complex demodulation was applied since it permits the determination of continuous changes in time of the amplitude and frequency of the signal relative to the test signal. It was found that a period of ~27.6 days gave an overall flat phase function in time, while other periods < ~0.5 day shorter and longer, with comparable but lesser amplitude, come and go. To investigate the solar sources of these periods, the method of principal component analysis (PCA) was applied to ~ 27 years (1976-2003) of synoptic maps obtained with the NSO Kitt Peak Vaccum Telescope. Before the analysis, the original synoptic maps were shifted relative to the previous maps using the period under investigation. Using PCA the Empirical Orthogonal Functions (EOFs) and Pricipal Components (PCs) were found for the set of synoptic maps rescaled to the rotation rate 27.03 days in 1999-2003. The patterns characterized by EOFs 1 and 2 are mostly axisymmetric and PCs 1 and 2 show solar cycle variability. EOF3 shows only one well-localized pattern in the Southern Hemisphere which is markedly non-axisymmetric and PC3 has peaks at times when fast CMEs occur.

Cadavid, A. C.; Lawrence, J. K.; Sandor, C.; Ruzmaikin, A.

2006-12-01

41

Quasi-periodic emissions observed by Cluster and DEMETER spacecraft  

NASA Astrophysics Data System (ADS)

Quasi-periodic (QP) emissions are electromagnetic emissions in the frequency range of about 0.5-4 kHz that are characterized by a periodic modulation of wave intensity. Typical periods of this modulation are on the order of minutes. Although there are many observations of these events by ground-based instruments, satellite observations are still rather sparse. Nevertheless, these are of great importance, as they allow us to analyze wave properties in situ, close to the probable generation region, and, moreover, they are not affected by the wave propagation in the Earth-ionosphere waveguide. We present a survey of QP events observed by the WBD instruments on board the four Cluster spacecraft during their perigee passes at radial distances of about 4 RE. Moreover, a conjugate observation of a QP event by Cluster spacecraft and by the low-altitude DEMETER spacecraft has been identified. Simultaneous observations of the same event by several different spacecraft enable us to distinguish between spatial and temporal variations of the phenomenon. It is shown that during a QP event, the same modulation is observed at the same time at very different locations of the inner magnetosphere. The results of a detailed wave analysis based on multi-component measurements by the STAFF-SA instruments indicate that the emissions propagate unducted, with oblique wave normal angles at larger geomagnetic latitudes. Finally, ULF magnetic field data are inspected for the presence of magnetic field fluctuations with a period corresponding to the period of modulation and a possible generation mechanism of the events is discussed.

Nemec, F.; Santolik, O.; Parrot, M.; Hayosh, M.; Pickett, J. S.; Cornilleau-Wehrlin, N.

2012-12-01

42

Quasi-periodic solutions and periodic bursters in quasiperiodically driven oscillators  

Microsoft Academic Search

In this paper, we propose a perturbation method to determine an approximation and conditions of existence of quasi-periodic (QP) solutions and bursting dynamics in a quasi-periodically driven system. The QP forcing consists of two periodic excitations, one with a very slow frequency and the other with a frequency of the same order of the proper frequency of the oscillator. A

Faouzi Lakrad; Mohamed Belhaq

2009-01-01

43

Omnidirectional reflection from Fibonacci quasi-periodic one-dimensional photonic crystal  

Microsoft Academic Search

It is shown that omnidirectional reflection (ODR) is possible from quasi-periodic isotropic dielectric stacks following a Fibonacci sequence (FS). The transition from truly periodic to fully quasi-periodic structure is investigated by building periodic structures having unit cells made of FS of order j. The number of periods required to achieve ODR decreases as j increases until only a single period

D. Lusk; I. Abdulhalim; F. Placido

2001-01-01

44

Observation and modeling of quasi-periodic scintillations observed at low latitude  

NASA Astrophysics Data System (ADS)

Quasi-periodic scintillations are characterized as primary deep fade-out infield strength, associated with regular ringing patterns before and after it. In this paper, observations of quasi-periodic scintillation using geostationary satellite (FLEETSAT) transmissions operating at frequency 250 MHz at low latitude ground station, Varanasi (geomag. lat 14° 55' N, long. 154°E) are reported. The results indicate that the quasi-periodic scintillations are most likely produced by plasma blobs/bubbles present in the E and F-region of the ionosphere. The various characteristics features of the quasi periodic scintillations are discussed after the autocorrelation, power spectrum and scintillation index analysis. The computed horizontal scale size of the quasi periodic scintillation producing irregularity varies from 100 m to 1300 m which shows that the irregularities are of intermediate-scale sizes. The spectral index obtained from the slopes of power spectrum varies from -2 to -8. The observed fading patterns, especially the modulation of the diffraction pattern (fading envelope) can be explained by considering an obstacle called radio lens in the ionosphere elongated in one direction. We have simulated successfully the amplitude versus time plot of quasi periodic scintillation patches and found that our theoretical and experimental results of quasi periodic scintillation patches compares well with each other and also with the earlier published works.

Patel, Kalpana; Singh, A. K.; Singh, R. P.

2010-02-01

45

Construction of quasi-periodic solutions of delay differential equations via KAM techniques  

NASA Astrophysics Data System (ADS)

This work focuses on the existence of quasi-periodic solutions for linear autonomous delay differential equation under quasi-periodic time-dependent perturbation near an elliptic-hyperbolic equilibrium point. Using the time-1 map of the solution operator, Newton iteration scheme, space splitting and KAM techniques, it is shown that under appropriate hypothesis, there exist quasi-periodic solutions with the same frequencies as the perturbation for most parameters. We show that if the delay differential equation is analytic, we obtain analytic parameterizations of the solutions.

Li, Xuemei; de la Llave, Rafael

46

Quasi-periodic Oscillations in XMM-Newton Timing data of Blazars  

NASA Astrophysics Data System (ADS)

In the present talk, I will report our findings of Quasi-periodic Oscillations in XMM-Newton light curves of Blazars. I will also discuss the possible radio-loud active galactic nuclei models which can explain our findings.

Gupta, Alok Chandra

2012-07-01

47

The "Approximate 150 Day Quasi-Periodicity" in Interplanetary and Solar Phenomena During Cycle 23  

NASA Technical Reports Server (NTRS)

A"quasi-periodicity" of approx. 150 days in various solar and interplanetary phenomena has been reported in earlier solar cycles. We suggest that variations in the occurrence of solar energetic particle events, inter-planetary coronal mass ejections, and geomagnetic storm sudden commenceents during solar cycle 23 show evidence of this quasi-periodicity, which is also present in the sunspot number, in particular in the northern solar hemisphere. It is not, however, prominent in the interplanetary magnetic field strength.

Richardson, I. G.; Cane, H. V.

2004-01-01

48

Manipulation of quadratic cascading processes in a locally quasi-periodic ?(²) medium.  

PubMed

We theoretically and numerically investigate the quadratic cascading effect of third-harmonic (TH) generation in a locally quasi-periodic nonlinear photonic structure. We study the effect of structure parameters on the acceptance bandwidth and conversion efficiency of the cascading process. We demonstrate that the conversion efficiency of the cascading process can be enhanced by using a longer locally quasi-periodic nonlinear photonic crystal, without adversely affecting the acceptance bandwidth of the emitted radiation. PMID:24664046

Wang, Wenjie; Sheng, Yan; Liu, Shaoding; Niu, Xiaoying; Krolikowski, Wieslaw

2014-03-24

49

Quasi-Bloch electrons of the two-dimensional quasi-periodic system in a tile-dependent magnetic field  

Microsoft Academic Search

The general solution is obtained for a Schrodinger equation with a tile-dependent magnetic field as well as a quasi-periodic potential in two dimensions (2D). The behaviour of the noninteracting electrons (quasi-Bloch electrons) in this quasi-periodic system may be treated as the projection of the behaviour of the Bloch pseudo-electrons in D dimensions. The physical quasi-periodicity of the 2D quasi-periodic system

J. Q. You

1988-01-01

50

Dipolar mode localization and spectral gaps in quasi-periodic arrays of ferromagnetic nanoparticles  

NASA Astrophysics Data System (ADS)

In this paper we study the spectral, localization, and dispersion properties of the ferromagnetic dipolar modes around a stable, saturated, and spatially uniform equilibrium in quasi-periodically modulated arrays of ferromagnetic nanoparticles based on the Fibonacci sequence. The Fibonacci sequence is the chief example of deterministic quasi-periodic order. The problem is reduced to the study of a linear-generalized eigenvalue equation for a suitable Hermitian operator connected to the micromagnetic effective field, which accounts for the magnetostatic, anisotropy, and Zeeman interactions. The coupling with a weak applied magnetic field, varying sinusoidally in time, is dealt with and the role of the losses is highlighted. By calculating the resonance frequencies and eigenmodes of the Fibonacci arrays we demonstrate the presence of large spectral gaps and strongly localized modes and we evaluate the pseudodispersion diagrams. The magnetization oscillation modes in quasi-periodic arrays of magnetic nanoparticles show, at microwave frequencies, behaviors that are very similar to those shown, at optical frequencies, by plasmon modes in quasi-periodic arrays of metal nanoparticles. The presence of band gaps and strongly localized states in magnetic nanoparticle arrays based on quasi-periodic order may have an impact in the design and fabrication of new microwave nanodevices and magnetic nanosensors.

Forestiere, Carlo; Miano, Giovanni; Serpico, Claudio; D'Aquino, Massimiliano; Dal Negro, Luca

2009-06-01

51

Quasi-periodic breathers in Hamiltonian networks of long-range coupling  

NASA Astrophysics Data System (ADS)

This work is concerned with Hamiltonian networks of weakly and long-range coupled oscillators with either variable or constant on-site frequencies. We derive an infinite dimensional KAM-like theorem by which we establish that, given any N-sites of the lattice, there is a positive measure set of small amplitude, quasi-periodic breathers (solutions of the Hamiltonian network that are quasi-periodic in time and exponentially localized in space) having N-frequencies which are only slightly deformed from the on-site frequencies.

Geng, Jiansheng; Viveros, Jorge; Yi, Yingfei

2008-11-01

52

Acoustic lens: A thin plate with quasi-periodic array of holes  

NASA Astrophysics Data System (ADS)

A thin steel plate with quasi-periodic array of holes is fabricated, which is demonstrated to be able to function as an acoustic lens. With either a plane wave or a point source in object space, hotspots with the smallest size up to one-fifth wavelength are observed in the post-evanescent field regime in image space. Imaging of a point source with good resolution at different positions is also exhibited. The singular field distributions originate from the interference of the diffractive beams specific to quasi-periodic structures, which generates distinct and plentiful diffractive patterns.

Ye, Yangtao; Ke, Manzhu; Li, Chunhui; Wang, Tian; Qiu, Chunyin; Liu, Zhengyou

2014-05-01

53

Asymptotic solutions for a damped non-linear quasi-periodic Mathieu equation  

Microsoft Academic Search

Quasi-periodic (QP) solutions of a weakly damped non-linear QP Mathieu equation are investigated near a double primary parametric resonance. A double multiple scales method is applied to reduce the original QP oscillator to an autonomous system performing two successive reduction. The problem for approximating QP solutions of the original system is then transformed to the study of stationary regimes of

Mohamed Belhaq; Kamar Guennoun; Mohamed Houssni

2002-01-01

54

Scaling of torus-doubling terminal points in a quasi-periodically forced map  

NASA Astrophysics Data System (ADS)

The torus-doubling bifurcations of a quasi-periodically forced two-dimensional map are investigated numerically. The scaling law on the terminal points of the torus-doubling bifurcation sequences is obtained by a simple method, based on hyper-stable period point and phase sensitivity exponent analyses.

Fu, Wu-Jiu; He, Dai-Hai; Shi, Peng-Liang; Kang, Wei; Hu, Gang

2002-01-01

55

Quasi-periodic oscillations and chaos in a gas-discharge active mode-locked laser  

Microsoft Academic Search

It is shown that the quasi-periodic oscillations and chaos that appear on the destruction of active mode locking in an He-Ne laser operated at 1150 nm are connected with the high supermodes. Consideration is given to the different stationary pulse profiles that may be identified with these supermodes. A difference is found to exist between positive and negative tuning of

L. A. Melnikov; E. M. Rabinovich; V. V. Tuchin

1988-01-01

56

A numerically accessible criterion for the breakdown of quasi-periodic solutions and its rigorous justification  

Microsoft Academic Search

We formulate and justify rigorously a numerically efficient criterion for the computation of the analyticity breakdown of quasi-periodic solutions in symplectic maps (any dimension) and 1D statistical mechanics models. Depending on the physical interpretation of the model, the analyticity breakdown may correspond to the onset of mobility of dislocations, or of spin waves (in the 1D models) and to the

Renato Calleja; Rafael de la Llave

2010-01-01

57

Dripping handrails and the quasi-periodic oscillations of the AM Herculis objects  

NASA Technical Reports Server (NTRS)

AM Her objects exhibit periodic, quasi-periodic, and aperiodic variability on timescales ranging from seconds to years. Here, we investigate a process for the production of aperiodic and quasi-periodic accretion rate fluctuations. We consider the nonlinear dynamical model known as the dripping handrail (DHR). The DHR, basically a model for certain types of spatially extended systems and loosely based on water condensing on and dripping off a handrail, has recently been used as a model for the quasi-periodic oscillations (QPO) and very low frequency noise of the low-mass X-ray binary Sco X-1. Here, we show that (1) the DHR is a robust QPO generation process in that it leads to QPO production under a wide range of conditions and assumptions; (2) the phenomenology of the DHR is consistent with the observed aperiodic and quasi-periodic varibility of the AM Her QPO source VV Pup over timescales ranging from 16 ms to 20 s; and (3) a single DHR model can produce both broadband QPOs and features with quality Q greater than 20 as observed in several AM Her QPO sources.

Steiman-Cameron, Thomas Y.; Young, Karl; Scargle, Jeffrey D.; Crutchfield, James P.; Imamura, James N.; Wolff, Michael T.; Wood, Kent S.

1994-01-01

58

GENERAL: Quasi-Periodic Waves and Asymptotic Property for Boiti-Leon-Manna-Pempinelli Equation  

NASA Astrophysics Data System (ADS)

In this paper, multi-periodic (quasi-periodic) wave solutions are constructed for the Boiti-Leon-Manna-Pempinelli (BLMP) equation by using Hirota bilinear method and Riemann theta function. At the same time, we analyze in details asymptotic properties of the multi-periodic wave solutions and give their asymptotic relations between the periodic wave solutions and the soliton solutions.

Luo, Lin

2010-08-01

59

Pure Point Spectrum of the Floquet Hamiltonian for the Quantum Harmonic Oscillator Under Time Quasi-Periodic Perturbations  

Microsoft Academic Search

We prove that the 1-d quantum harmonic oscillator is stable under spatially localized, time quasi-periodic perturbations on a set of Diophantine\\u000a frequencies of positive measure. This proves a conjecture raised by Enss-Veselic in their 1983 paper [EV] in the general quasi-periodic\\u000a setting. The motivation of the present paper also comes from construction of quasi-periodic solutions for the corresponding\\u000a nonlinear equation.

W.-M. Wang

2008-01-01

60

Towards modeling quasi-periodic oscillations of microquasars with oscillating slender tori  

NASA Astrophysics Data System (ADS)

Context. One of the often discussed models for high-frequency quasi-periodic oscillations of X-ray binaries is the oscillating torus model, which considers oscillation modes of slender accretion tori. Aims: Here, we aim at developing this model by considering the observable signature of an optically thick slender accretion torus subject to simple periodic deformations. Methods: We compute light curves and power spectra of a slender accretion torus subject to simple periodic deformations: vertical or radial translation, rotation, expansion, and shear. Results: We show that different types of deformations lead to very different Fourier power spectra and therefore could be observationally distinguished. Conclusions: This work is a first step in a longer term study of the observable characteristics of the oscillating torus model. It gives promising perspectives on the possibility of constraining this model by studying the observed power spectra of quasi-periodic oscillations.

Mazur, G. P.; Vincent, F. H.; Johansson, M.; Šramková, E.; Török, G.; Bakala, P.; Abramowicz, M. A.

2013-06-01

61

The effect of quasi-periodicity on the resonant tunneling lifetimes of states in electrically biased semiconductor superlattices  

NASA Astrophysics Data System (ADS)

The tunneling lifetimes of quasi-resonant states for electrons in various kinds of generalized Fibonacci and generalized Thue-Morse GaAs-AlxGa1-xAs superlattices have been evaluated numerically under variable dc bias conditions. All the quasi-periodic systems have been framed using the generalized block model. The variation of the lifetime at different quasi-resonant levels with respect to the external dc field undergoes a remarkable change due to the effect of quasi-periodicity. The occurrence of a minimum value of the average lifetime and its dependence on quasi-periodicity have been analyzed. It is shown that the low-order quasi-periodicity in the case of the generalized Fibonacci superlattice and the high-order quasi-periodicity for the generalized Thue-Morse superlattice hold promise for potential device applications. The impact of an increase in the number of barriers on the tunneling lifetime has also been studied exhaustively.

Panchadhyayee, P.; Biswas, R.; Sinha, C.; Mahapatra, P. K.

2008-11-01

62

Quasi-periodic solutions of the spatial lunar three-body problem  

NASA Astrophysics Data System (ADS)

In this paper, we consider the spatial lunar three-body problem in which one body is far away from the other two. By applying a well-adapted version of KAM theorem to Lidov-Ziglin's global study of the quadrupolar approximation of the spatial lunar three-body problem, we establish the existence of several families of quasi-periodic orbits in the spatial lunar three-body problem.

Zhao, Lei

2014-05-01

63

Rayleigh-Taylor Gravity Waves and Quasi-periodic Oscillation Phenomena in X-Ray Binaries  

Microsoft Academic Search

Accretion onto compact objects in X-ray binaries (black hole, neutron star [NS], white dwarf) is characterized by nonuniform flow density profiles. Such an effect of heterogeneity in the presence of gravitational forces and pressure gradients causes Rayleigh-Taylor gravity waves. They should be seen as quasi-periodic wave oscillations (QPOs) of the accretion flow in the transition (boundary) layer between the Keplerian

Lev Titarchuk

2003-01-01

64

Periodic and quasi-periodic solutions for multi-instabilities involved in brake squeal  

Microsoft Academic Search

This paper is devoted to the computation of nonlinear dynamic steady-state solutions of autonomous systems subjected to multi-instabilities and proposes a new nonlinear method for predicting periodic and quasi-periodic solutions intended for application to the disc brake squeal phenomenon. Firstly, finite element models of a pad and a disc are reduced to include only their contact nodes by using a

N. Coudeyras; S. Nacivet; J.-J. Sinou

2009-01-01

65

Transmission properties of Fibonacci quasi-periodic one-dimensional superconducting photonic crystals  

Microsoft Academic Search

The transmission properties of Fibonacci quasi-periodic one-dimensional photonic crystals (1DPCs) containing superconducting material are theoretically investigated based on the transfer matrix method. It is shown that the 1DPCs can possess a same photonic band gap property as the periodic structure superconducting PC. The results of transmittance spectra show that the cutoff frequency can be manipulated through the thicknesses of the

Ji-jiang Wu; Jin-xia Gao

66

A broad omnidirectional reflection band obtained from deformed Fibonacci quasi-periodic one dimensional photonic crystals  

Microsoft Academic Search

By studying the deformed Fibonacci quasi-periodic structure, a broad omnidirectional reflection band covering all telecommunication bands is obtained. Deformation was introduced by applying a power law, so that the coordinates y of the deformed object were determined through the coordinates x of the non-deformed structure in accordance with the following rule: y = x1+k. Here k is the coefficient defining

K. Ben Abdelaziz; J. Zaghdoudi; M. Kanzari; B. Rezig

2005-01-01

67

Transmission properties of Fibonacci quasi-periodic one-dimensional photonic crystals containing indefinite metamaterials  

Microsoft Academic Search

The transmission properties of Fibonacci quasi-periodic one-dimensional photonic crystals (1DPCs) containing indefinite metamaterials are theoretically studied. It is found that 1DPCs can possess an omnidirectional zero average index (zero-n?) gap which exists in all Fibonacci sequences. In contrast to Bragg gaps, such zero-n? gap is less sensitive to the incidence angle, the scale length and the polarizations of electromagnetic waves.

Liwei Zhang; Kai Fang; Guiqiang Du; Haitao Jiang; Junfang Zhao

2011-01-01

68

Scattering theory for Jacobi operators with a steplike quasi-periodic background  

NASA Astrophysics Data System (ADS)

We develop direct and inverse scattering theory for Jacobi operators with a steplike quasi-periodic finite-gap background in the same isospectral class. We derive the corresponding Gel'fand-Levitan-Marchenko equation and find minimal scattering data which determine the perturbed operator uniquely. In addition, we show how the transmission coefficients can be reconstructed from the eigenvalues and one of the reflection coefficients.

Egorova, Iryna; Michor, Johanna; Teschl, Gerald

2007-06-01

69

Phase-rectified signal averaging detects quasi-periodicities in non-stationary data  

Microsoft Academic Search

We present an efficient technique for the study of quasi-periodic oscillations in noisy, non-stationary signals, which allows the assessment of system dynamics despite phase resetting and noise. It is based on the definition of anchor points in the signal (in the simplest case increases or decreases of the signal) which are used to align (i.e., phase-rectify) the oscillatory fluctuations followed

Axel Bauer; Jan W. Kantelhardt; Armin Bunde; Petra Barthel; Raphael Schneider; Marek Malik; Georg Schmidt

2006-01-01

70

Quasi-periodic hard X-ray oscillations before impulsive phase of solar flares  

NASA Astrophysics Data System (ADS)

Using observations from the YOHKOH Hard X-ray Telescope and Compton Gamma Ray Ob-servatory spectrometer we have found small-amplitude quasi-periodic hard X-ray oscillations before impulsive phase (OBIP) of solar flares. We have been investigating properties of the oscillations and transition from the OBIP to impulsive phase. Our results support the model of electron acceleration in oscillating magnetic traps (Jakimiec and Tomczak 2010, Solar Physics, 261, 233).

Tomczak, Michal; Jakimiec, Jerzy

71

Exact quasi-periodic solutions of the Konno–Oono equations  

NASA Astrophysics Data System (ADS)

On the basis of the Lax matrix and elliptic variables, the Konno–Oono equations are decomposed into solvable ordinary differential equations. The Konno–Oono flows are straightened with the aid of the theory of algebraic curves and the Abel–Jacobi coordinates. The asymptotic properties of the meromorphic function at infinite points and its algebro-geometric characteristics are studied, from which exact quasi-periodic solutions of the Konno–Oono equations are obtained.

Guan, Liang; Geng, Xianguo; Li, Zhu

2014-07-01

72

Quasi-periodical components in the radial distributions of cosmologically remote objects  

NASA Astrophysics Data System (ADS)

A statistical analysis of radial (line-of-sight) 1D-distributions of brightest cluster galaxies (BCGs) within the redshift interval 0.044 ? z ? 0.78 and Mg II absorption-line systems (0.37 ? z ? 2.28) is carried out. Power spectra and two-point radial correlation functions are calculated. It is found that both radial distributions of spectroscopic redshifts of 52 683 BCGs and 32 840 Mg II absorption systems incorporate similar quasi-periodical components relatively to the comoving distance. Significance of the components exceeds 4?-level and admits an increase ( ? 5?) for some broad subsamples. For the ? cold dark matter cosmological model the periodicities correspond to spatial comoving scales (98 ± 3) and (101 ± 2) h-1 Mpc, respectively. These quasi-periods turn out to be close to the characteristic scale (101 ± 6) h-1 Mpc of the quasi-periodical component obtained earlier for the radial distribution of luminous red galaxies (LRGs). On the other hand, the scales are close to the spatial scale corresponding to the baryon acoustic oscillations (BAOs) revealed by many authors at the last decade. Fourier transform phases obtained for the BCGs and LRGs are found to be close, while the phases calculated for the Mg II absorption systems and LRGs are opposite. Discussions of the results in a context of the BAO and large-scale structure characteristic scales are outlined.

Ryabinkov, A. I.; Kaminker, A. D.

2014-05-01

73

Quasi-periodic flares in Jupiter's aurora : new results  

NASA Astrophysics Data System (ADS)

Two recent Hubble Space Telescope observation campaigns have been dedicated to the Jovian Far-UV aurora (GO 12883 - PI: D. Grodent and GO 13035 - PI: S. Badman). Both of them made use of the Time-Tag mode of the Space Telescope Imaging Spectrograph (STIS), a high time resolution mode which allows to observe temporal variations on timescales of tens of seconds. In the present study, we focus on sudden and spectacular bursts of auroral emissions taking place in the active region located poleward of the main emissions and called "flares". A previous study, based on only two image sequences acquired with rather unfavorable viewing angles, showed that these flares could reappear quasi-periodically on time scales of 2-3 minutes. Phenomena with similar timescales have been identified by in-situ spacecraft in relativistic electron and radio data as well as in reconnection signatures, for example. But the physical mechanism behind these ubiquitous signatures remains to be unveiled. Here we make use of the most recent and much larger data set to study in further details the occurrence rate, the period, the location, the extent and the motion of these quasi-periodic flares and to compare their behavior in both hemispheres. Quantifying these parameters allows us to narrow down the possibilities among likely explanations and provide a tentative scenario for these short timescale quasi-periodic features.

Bonfond, Bertrand; Grodent, Denis; Badman, Sarah; Gérard, Jean-Claude; Radioti, Aikaterini; Gustin, Jacques; Kimura, Tomoki

2014-05-01

74

The 8 second optical quasi-periodic oscillations in GX 339 - 4  

NASA Technical Reports Server (NTRS)

Submillisecond optical photometry of the black hole candidate GX 339 - 4 was obtained on August 1, 1989, (UT) using the 1.5 m telescope of the Cerro Tololo Inter-American Observatory. Eight second quasi-periodic oscillations of width 0.02-0.04 Hz and root mean square amplitude 4-6 percent are found. The visual magnitude of GX 339 - 4 at the beginning of the observation was m(v) = 17.7. Motch et al. (1985) have previously reported 7 s optical quasi-periodic oscillations when GX 339 - 4 was also m(v) = 17.7 and in an X-ray off-state. No X-ray observations were made during the present optical observations and so the X-ray state of GX 339 - 4 cannot be ascertained. In addition, Motch et al. have also reported 20 s optical quasi-periodic oscillations with 30-40 percent full amplitude but when GX 339 - 4 was much brighter, m(v) = 15.4, and in a hard X-ray state.

Imamura, James N.; Kristian, Jerome; Middleditch, John; Steiman-Cameron, Thomas Y.

1990-01-01

75

Broad Omnidirectional Reflection Band Forming using the Combination of Fibonacci Quasi-Periodic and Periodic One-Dimensional Photonic Crystals  

NASA Astrophysics Data System (ADS)

By combining two Fibonacci quasi-periodic structures and a periodic structure to form a heterostructure, a broad omnidirectional reflection band is obtained. From the numerical results performed by the transfer matrix method, it is found that the reflection bands of the two Fibonacci quasi-periodic sub-structures and the periodic sub-structure can be compensated for each other. This method is expected to be useful in constructing a one-dimensional quasi-periodic photonic crystal structure with a broad omnidirectional reflection band.

Dong, Jian-Wen; Han, Peng; Wang, He-Zhou

2003-11-01

76

A broad omnidirectional reflection band obtained from deformed Fibonacci quasi-periodic one dimensional photonic crystals  

NASA Astrophysics Data System (ADS)

By studying the deformed Fibonacci quasi-periodic structure, a broad omnidirectional reflection band covering all telecommunication bands is obtained. Deformation was introduced by applying a power law, so that the coordinates y of the deformed object were determined through the coordinates x of the non-deformed structure in accordance with the following rule: y = x1+k. Here k is the coefficient defining the deformation degree. From the numerical results performed by the transfer matrix method, it is found that the reflection band of the deformed 15th generation Fibonacci sequence structure covered all optical telecommunication bands.

Ben Abdelaziz, K.; Zaghdoudi, J.; Kanzari, M.; Rezig, B.

2005-10-01

77

Transmission properties of Fibonacci quasi-periodic one-dimensional photonic crystals containing indefinite metamaterials  

NASA Astrophysics Data System (ADS)

The transmission properties of Fibonacci quasi-periodic one-dimensional photonic crystals (1DPCs) containing indefinite metamaterials are theoretically studied. It is found that 1DPCs can possess an omnidirectional zero average index (zero- n?) gap which exists in all Fibonacci sequences. In contrast to Bragg gaps, such zero- n? gap is less sensitive to the incidence angle, the scale length and the polarizations of electromagnetic waves. When an impurity is introduced, a defect mode appears inside the zero- n? gap with a very weak dependence on the incidence angle and scaling.

Zhang, Liwei; Fang, Kai; Du, Guiqiang; Jiang, Haitao; Zhao, Junfang

2011-02-01

78

Resonance in Forced Oscillations of an Accretion Disk and Kilohertz Quasi-periodic Oscillations  

NASA Astrophysics Data System (ADS)

We have performed numerical simulations of a radially perturbed ``accretion'' torus around a black hole or neutron star and find that the torus performs radial and vertical motions at the appropriate epicyclic frequencies. We find clear evidence that vertical motions are excited in a nonlinear resonance when the applied perturbation is periodic in time. The strongest resonant response occurs when the frequency difference of the two oscillations is equal to one-half the forcing frequency, precisely as recently observed in the accreting pulsar SAX J1808.4-3658, where the observed kilohertz quasi-periodic oscillation peak separation is half the spin frequency of 401 Hz.

Lee, William H.; Abramowicz, Marek A.; Klu?niak, W?odek

2004-03-01

79

Combined In-situ and Ground-based Observations of Quasi-periodic Radar Echoes  

NASA Astrophysics Data System (ADS)

A series of combined rocket/radar investigation of the electrodynamics and neutral- plasma coupling associated with sporadic-E layers and quasi-periodic backscatter radar echoes has been carried out from launch sites at both Puerto Rico and the Wallops Flight Facility, Virginia (USA) between 1998-2001. The instrumented rock- ets consisted of main and sub-payloads and were launched while strong quasi- periodic VHF echoes were observed simultaneously with the Univ. of Illinois 50 MHz backscatter radar. The rocket apogee was purposely limited so that the payloads would dwell in the sporadic-E region (90-115 km). The main payload included vector DC and AC electric field detectors, a DC magnetometer, an ion mass spectrometer, an ioniza- tion gauge, and spaced-electric field receivers to measure the wavelength and phase velocity of the unstable plasma waves. The sub-payload was instrumented to measure DC and wave electric fields and plasma density. In one case, a separate rocket was launched a few minutes later which released luminous TMA trails to measure the neu- tral wind, its velocity shear, and embedded neutral structures. In this experiment, the payloads successfully pierced a well-defined, 2-3 km thick metallic sporadic-E layer of approximately 10**5 e/cc near 103 km altitude. In-situ DC electric field measure- ments revealed ~5mV/m ambient meridional fields above and below the layer with 1-2 mV/m amplitude, large scale structures superimposed. The wavelengths of these structures were approximately 2-4 km and may be related to the seat of the quasi- periodic echoes. Intense (~5 mV/m), higher frequency (shorter scale) broadband waves were also observed in-situ, both above and below the layer, consistent with the VHF backscatter observations during the time of the launch. Neither the large scale nor short scale plasma waves appeared to be distinctly organized by the sporadic-E den- sity layer. The TMA release showed large amplitude (~ 100 m/s) meridional winds near 102-105 km, with the most intense shears directly below these altitudes, where the short scale electric field fluctuations were most intense. We summarize the ob- servations from the different experiments and discuss them in the context of current theories regarding quasi-periodic echoes.

Pfaff, R.; Kudeki, E.; Larsen, M.; Clemmons, J.; Earle, G.

80

Quasi-periodic behavior of ion acoustic solitary waves in electron-ion quantum plasma  

SciTech Connect

The ion acoustic solitary waves are investigated in an unmagnetized electron-ion quantum plasmas. The one dimensional quantum hydrodynamic model is used to study small as well as arbitrary amplitude ion acoustic waves in quantum plasmas. It is shown that ion temperature plays a critical role in the dynamics of quantum electron ion plasma, especially for arbitrary amplitude nonlinear waves. In the small amplitude region Korteweg-de Vries equation describes the solitonic nature of the waves. However, for arbitrary amplitude waves, in the fully nonlinear regime, the system exhibits possible existence of quasi-periodic behavior for small values of ion temperature.

Sahu, Biswajit [Department of Mathematics, West Bengal State University Barasat, Kolkata-700126 (India); Poria, Swarup [Department of Applied Mathematics, University of Calcutta Kolkata-700009 (India); Narayan Ghosh, Uday [Department of Mathematics, Siksha Bhavana, Visva Bharati University Santiniketan (India); Roychoudhury, Rajkumar [Physics and Applied Mathematics Unit, Indian Statistical Institute Kolkata-700108 (India)

2012-05-15

81

On quasi-periodic motions around the collinear libration points in the real Earth–Moon system  

Microsoft Academic Search

Due to various perturbations, the collinear libration points of the real Earth–Moon system are not equilibrium points anymore.\\u000a Under the assumption that the Moon’s motion is quasi-periodic, special quasi-periodic orbits called dynamical substitutes\\u000a exist. These dynamical substitutes replace the geometrical collinear libration points as time-varying equilibrium points.\\u000a In the paper, the dynamical substitutes of the three collinear libration points in

X. Y. Hou; L. Liu

2011-01-01

82

Broad Omnidirectional Reflection Band Forming using the Combination of Fibonacci Quasi-Periodic and Periodic One-Dimensional Photonic Crystals  

Microsoft Academic Search

By combining two Fibonacci quasi-periodic structures and a periodic structure to form a heterostructure, a broad omnidirectional reflection band is obtained. From the numerical results performed by the transfer matrix method, it is found that the reflection bands of the two Fibonacci quasi-periodic sub-structures and the periodic sub-structure can be compensated for each other. This method is expected to be

Jian-Wen Dong; Peng Han; He-Zhou Wang

2003-01-01

83

Quasi-Periodic Oscillations, Chaos and Suppression of Chaos in a Nonlinear Oscillator Driven by Parametric and External Excitations  

Microsoft Academic Search

An analysis is given of the dynamic of a one-degree-of-freedom oscillator with quadratic and cubic nonlinearities subjected to parametric and external excitations having incommensurate frequencies. A new method is given for constructing an asymptotic expansion of the quasi-periodic solutions. The generalized averaging method is first applied to reduce the original quasi-periodically driven system to a periodically driven one. This method

M. Belhaq; M. Houssni

1999-01-01

84

GENERATION OF QUASI-PERIODIC WAVES AND FLOWS IN THE SOLAR ATMOSPHERE BY OSCILLATORY RECONNECTION  

SciTech Connect

We investigate the long-term evolution of an initially buoyant magnetic flux tube emerging into a gravitationally stratified coronal hole environment and report on the resulting oscillations and outflows. We perform 2.5-dimensional nonlinear numerical simulations, generalizing the models of McLaughlin et al. and Murray et al. We find that the physical mechanism of oscillatory reconnection naturally generates quasi-periodic vertical outflows, with a transverse/swaying aspect. The vertical outflows consist of both a periodic aspect and evidence of a positively directed flow. The speed of the vertical outflow (20-60 km s{sup -1}) is comparable to those reported in the observational literature. We also perform a parametric study varying the magnetic strength of the buoyant flux tube and find a range of associated periodicities: 1.75-3.5 minutes. Thus, the mechanism of oscillatory reconnection may provide a physical explanation to some of the high-speed, quasi-periodic, transverse outflows/jets recently reported by a multitude of authors and instruments.

McLaughlin, J. A.; Verth, G. [School of Computing, Engineering and Information Sciences, Northumbria University, Newcastle Upon Tyne, NE1 8ST (United Kingdom); Fedun, V.; Erdelyi, R., E-mail: james.a.mclaughlin@northumbria.ac.uk, E-mail: gary.verth@northumbria.ac.uk, E-mail: v.fedun@sheffield.ac.uk, E-mail: robertus@sheffield.ac.uk [Solar Physics and Space Plasma Research Centre (SP2RC), School of Mathematics and Statistics, University of Sheffield, Hounsfield Road, Hicks Building, Sheffield, S3 7RH (United Kingdom)

2012-04-10

85

Low altitude quasi-periodic radar echoes observed by the Gadanki VHF radar  

NASA Astrophysics Data System (ADS)

We report here on the low altitude quasi-periodic (LQP) radar echoes from low latitude sporadic E layer (Es) observed by the Gadanki (13.5°N, 79.2°E geomagnetic latitude 6.3°N) VHF radar. The LQP echoes occurred both during daytime and nighttime and are confined to a slowly descending layer with a thickness of about 2-4 km in the height range of 90-100 km. The periods are found to range from tens of seconds to less than about 3 minutes. The Doppler velocities vary over a range of -20 to +20 m/s during daytime and 0 to 10 m/s during nighttime and are known to be sensitive to the layer height, being dominated by the effect of zonal electric field above and meridional neutral wind below a height of ~97 km for the type 2 irregularities [Krishna Murthy et al., 1998]. The spectral widths are found to be of the order of 50 to 75 m/s during daytime and 30 to 60 m/s during nighttime. The LQP echoes reported here are similar to that observed recently over midlatitudes [Rao et al., 2000; Urbina et al., 2000], but distinctly different from the widely reported quasi-periodic (QP) echoes occurring at higher altitudes (>100 km). The observations are discussed briefly in terms of the potential source mechanisms.

Pan, C. J.; Rao, P. B.

2002-06-01

86

The statistical study of quasi-periodic oscillations of the radio emission in solar quiet regions  

NASA Astrophysics Data System (ADS)

In this study we discuss variations of the radio emission from the Quiet Sun Areas (QSA) at centimeter wavelength (1.76 cm). Data were obtained from Nobeyama Radioheliograph (NoRH). Oscillations of selected areas were studied carefully from data taken over one week. We try to find quasi-periodic solar oscillations from the QSA. We used the traditional Fast Fourier Transform (FFT), Global Wavelet Spectrum (GWS) and Wavelet (Morlet) for studying signals in the frequency/time-frequency domain. We used the Fisher randomization test to verify the significance of the observed signal. Instrumental and sky noises were studied using a cross-correlation analysis. Additionally, a single pixel analysis were done. Wide ranges of solar oscillation periods were found from the Quiet Sun Area (QSA): 3-15, 35-70, and 90 minutes. Some physical explanations are suggested for these oscillations. However, it is not possible to give a conclusive statement about the origin of the long quasi-periodic (>60 min) oscillations from the QSA.

Kallunki, J.; Riehokainen, A.

2012-01-01

87

The Analyticity Breakdown for Frenkel-Kontorova Models in Quasi-periodic Media: Numerical Explorations  

NASA Astrophysics Data System (ADS)

We study numerically the "analyticity breakdown" transition in 1-dimensional quasi-periodic media. This transition corresponds physically to the transition between pinned down and sliding ground states. Mathematically, it corresponds to the solutions of a functional equation losing their analyticity properties. We implemented some recent numerical algorithms that are efficient and backed up by rigorous results so that we can compute with confidence even close to the breakdown. We have uncovered several phenomena that we believe deserve a theoretical explanation: (A) The transition happens in a smooth surface. (B) There are scaling relations near breakdown. (C) The scaling near breakdown is very anisotropic. Derivatives in different directions blow up at different rates. Similar phenomena seem to happen in other KAM problems.

Blass, Timothy; de la Llave, Rafael

2013-03-01

88

QUASI-PERIODIC FORMALDEHYDE MASER FLARES IN THE MASSIVE PROTOSTELLAR OBJECT IRAS 18566+0408  

SciTech Connect

We report results of an extensive observational campaign of the 6 cm formaldehyde maser in the young massive stellar object IRAS 18566+0408 (G37.55+0.20) conducted from 2002 to 2009. Using the Arecibo Telescope, the Very Large Array, and the Green Bank Telescope, we discovered quasi-periodic formaldehyde flares (P {approx} 237 days). Based on Arecibo observations, we also discovered correlated variability between formaldehyde (H{sub 2}CO) and methanol (CH{sub 3}OH) masers. The H{sub 2}CO and CH{sub 3}OH masers are not spatially coincident, as demonstrated by different line velocities and high angular resolution MERLIN observations. The flares could be caused by variations in the infrared radiation field, possibly modulated by periodic accretion onto a young binary system.

Araya, E. D. [Physics Department, Western Illinois University, 1 University Circle, Macomb, IL 61455 (United States); Hofner, P.; Goss, W. M. [National Radio Astronomy Observatory, P.O. Box O, Socorro, NM 87801 (United States); Kurtz, S. [Centro de RadioastronomIa y Astrofisica, Universidad Nacional Autonoma de Mexico, Apdo. Postal 3-72, 58089 Morelia, Michoacan (Mexico); Richards, A. M. S. [Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, University of Manchester, Manchester M13 9PL (United Kingdom); Linz, H. [Max-Planck-Institut fuer Astronomie, Koenigstuhl 17, D-69117 Heidelberg (Germany); Olmi, L. [University of Puerto Rico at Rio Piedras, Physics Department, P.O. Box 23343, San Juan, PR 00931 (Puerto Rico); Sewilo, M. [Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 (United States)

2010-07-10

89

Growth of Sobolev Norms in Linear Schrödinger Equations with Quasi-Periodic Potential  

NASA Astrophysics Data System (ADS)

In this paper, we consider the following problem. Let iut+?u+V(x,t)u= 0 be a linear Schrödinger equation ( periodic boundary conditions) where V is a real, bounded, real analytic potential which is periodic in x and quasi periodic in t with diophantine frequency vector ?. Denote S(t) the corresponding flow map. Thus S(t) preserves the L2-norm and our aim is to study its behaviour on Hs(TD), s> 0. Our main result is the growth in time is at most logarithmic; thus if ??Hs, then More precisely, (*) is proven in 1D and 2D when V is small. We also exhibit examples showing that a growth of higher Sobolev norms may occur in this context and (*) is thus essentially best possible.

Bourgain, J.

90

Quasi-periodic waves and an asymptotic property for the asymmetrical Nizhnik-Novikov-Veselov equation  

NASA Astrophysics Data System (ADS)

Based on a multi-dimensional Riemann theta function, the Hirota bilinear method is extended to explicitly construct multi-periodic (quasi-periodic) wave solutions for the asymmetrical Nizhnik-Novikov-Veselov equation. Among these periodic waves, two-periodic waves are a direct generalization of well-known cnoidal waves; their surface pattern is two dimensional. The main physical result is the description of the behavior of nonlinear waves in shallow water. A limiting procedure is presented to analyze asymptotic properties of the two-periodic waves in details. Relations between the periodic wave solutions and the well-known soliton solutions are established. It is rigorously shown that the periodic wave solutions tend to the soliton solutions under a 'small amplitude' limit.

Fan, Engui

2009-03-01

91

Quasi-periodic Wiggles of Microwave Zebra Structures in a Solar Flare  

NASA Astrophysics Data System (ADS)

Quasi-periodic wiggles of microwave zebra pattern (ZP) structures with periods ranging from about 0.5 s to 1.5 s are found in an X-class solar flare on 2006 December 13 at the 2.6-3.8 GHz with the Chinese Solar Broadband Radio Spectrometer (SBRS/Huairou). Periodogram and correlation analysis show that the wiggles have two to three significant periodicities and are almost in phase between stripes at different frequencies. The Alfvén speed estimated from the ZP structures is about 700 km s-1. We find the spatial size of the wave-guiding plasma structure to be about 1 Mm with a detected period of about 1 s. This suggests that the ZP wiggles can be associated with the fast magnetoacoustic oscillations in the flaring active region. The lack of a significant phase shift between wiggles of different stripes suggests that the ZP wiggles are caused by a standing sausage oscillation.

Yu, Sijie; Nakariakov, V. M.; Selzer, L. A.; Tan, Baolin; Yan, Yihua

2013-11-01

92

Quasi-periodic oscillations in the Z source GX 5-1  

NASA Technical Reports Server (NTRS)

A detailed study has been conducted of the time variability in the Z source GX 5-1 using Ginga, which observed the source in the horizontal and normal branches (HB, NB). Intensity-dependent HF, quasi-periodic oscillations (QPO) were observed in the HB, in which the source flux varied by a factor of 1.9. The QPO frequency in this portion of the HB ranges from about 13 to 17 Hz; this is lower than previously observed in any Z source. The HF and LF QPO were simultaneously observed in the NB. The strength of both forms of QPO and the strength of the LF noise increase rapidly with increasing photon energy.

Lewin, Walter H. G.; Lubin, Lori M.; Tan, Jianmin; Van Der Klis, Michiel; Van Paradijs, Jan; Penninx, Wim; Dotani, Tadayasu; Mitsuda, Kazuhisa

1992-01-01

93

Periodic and quasi-periodic solutions for multi-instabilities involved in brake squeal  

NASA Astrophysics Data System (ADS)

This paper is devoted to the computation of nonlinear dynamic steady-state solutions of autonomous systems subjected to multi-instabilities and proposes a new nonlinear method for predicting periodic and quasi-periodic solutions intended for application to the disc brake squeal phenomenon. Firstly, finite element models of a pad and a disc are reduced to include only their contact nodes by using a Craig and Bampton strategy. Secondly, a complex eigenvalue analysis is performed showing two unstable modes for a wide range of friction coefficients, after which a Generalized Constrained Harmonic Balance Method (GCHBM) is presented. This method can compute nonlinear periodic or pseudo-periodic responses depending on the number of unstable frequencies. The numerical results are in good agreement with those of time marching methods.

Coudeyras, N.; Nacivet, S.; Sinou, J.-J.

2009-12-01

94

Ginga observations of quasi-periodic oscillations in type II bursts from the Rapid Burster  

NASA Technical Reports Server (NTRS)

During Ginga observations of the 'Rapid Burster' in August 1988, strong quasi-periodic oscillations (QPOs) were detected in its X-ray intensity. The QPOs had centroid frequencies of 5 and 2 Hz during type II X-ray bursts which lasted for 10 and 30 s, respectively. The presence of the QPOs is correlated with the time scale-invariant burst profile. They are very strong during the initial peak in the burst, absent in the second peak, and strong again at the onset of the third peak. From an analysis of the X-ray spectrum as observed during the maxima and minima of the oscillations, it is found that the oscillations can be described by changes of the temperature of a blackbody emitter of constant apparent area.

Dotani, T.; Mitsuda, K.; Inoue, H.; Tanaka, Y.; Kawai, N.

1990-01-01

95

Singular Density of States Measure for Subshift and Quasi-Periodic Schrödinger Operators  

NASA Astrophysics Data System (ADS)

Simon's subshift conjecture states that for every aperiodic minimal subshift of Verblunsky coefficients, the common essential support of the associated measures has zero Lebesgue measure. We disprove this conjecture in this paper, both in the form stated and in the analogous formulation of it for discrete Schrödinger operators. In addition we prove a weak version of the conjecture in the Schrödinger setting. Namely, under some additional assumptions on the subshift, we show that the density of states measure, a natural measure associated with the operator family and whose topological support is equal to the spectrum, is singular. We also consider one-frequency quasi-periodic Schrödinger operators with continuous sampling functions and show that generically, the density of states measure is singular as well.

Avila, Artur; Damanik, David; Zhang, Zhenghe

2014-03-01

96

Time lags in the quasi-periodic oscillations of the rapid burster (MXB 1730-335)  

SciTech Connect

Time lags in the 0.4-5-Hz quasi-periodic oscillations (QPOs) of the rapid burster are investigated using two Exosat observations. Different QPO modes were noted during long type 2 bursts and in the persistent emission. The 1-5 keV X-ray signal lagged behind the 5-21-keV signal by 7.6 + or - 2.1 ms in the persistent emission QPO with frequencies of greater than 3.6 Hz. The fractional strength of the QPO was found to increase with photon energy during the persistent emission interval. The results provide evidence for a soft lag in QPOs which is suggested to be due to spectral softening during each QPO cycle. 16 references.

Stella, L.; Haberl, F.; Parmar, A.N.; Van Der Klis, M.; Lewin, W.H.G.

1988-04-01

97

Synchronizations of Quasi-period and Hyperchaos in Injected Two-section Semiconductor Lasers  

NASA Astrophysics Data System (ADS)

A novel hyperchaos synchronization system is presented. Hyperchaos synchronization in injection two-section semiconductor lasers was achieved for its application in secure communication. We found also a route from single-period to hyperchaos after passing quasi-period and chaos with increasing frequency detuning while the receiver synchronized with the transmitter in these dynamical regions. All optical private data communication encoded by a rate of 0.16 Gbit/s on/off phase shift key and a rate of 0.16 Gbit/s amplitude modulation and photoelectric private data communication encoded by a rate of 0.2 Gbit/s on/off current shift key and a current modulation of 0.12 GHz frequency, respectively, are simulated via this hyperchaos synchronization system. Decoding has been numerically demonstrated to achieve successfully.

Yan, Sen-lin

2013-03-01

98

Transmission Properties of Quasi-Periodic Fibonacci One-Dimensional Photonic Crystal Containing Negative Permittivity/permeability Material  

NASA Astrophysics Data System (ADS)

The transmission properties of one-dimensional quasi-periodic Fibonacci photonic crystal containing negative permittivity/permeability material are investigated by use of the transfer matrix method. We find that perfect transmission peaks exist at a series of dimensionless wavelength points in the transmission spectra, and the discrete localized modes appear inside the photonic band gap in the case of normal incidence. In the case of oblique incidence, the detailed numerical calculations show that the transmission peaks and angles strongly depend on the polarization of incident waves and the periodicity of the photonic crystals. In addition, we notice that the one-dimensional quasi-periodic photonic crystal can exhibit omni-directional reflection in a certain frequency region for all incident angles and polarizations. We also investigate the possibility of realizing the omni-directional reflection by means of the simple one-dimensional quasi-periodic Fibonacci photonic crystal.

Tao, Bo; Li, Fu-Li; Yu, Feng

99

Optimizing light absorption in a thin-film p-i-n solar cell using a quasi-periodic grating  

NASA Astrophysics Data System (ADS)

A p-i-n solar cell is best suited for strong absorbers with poor collection capabilities. However, the absorption naturally decreases at photon energies close to the electronic bandgap of the semiconductor. We hypothesized that a quasi-periodic surface textures in the role of diffraction gratings at the back contact can efficiently scatter light increasing the optical path length inside the absorber layer. The effect of quasi-periodic corrugated backing metallic contact of various types was studied theoretically. To help optimizing the design of the quasi periodic grating the corresponding canonical problem was considered. The absorption of light was calculated using the rigorous coupled-wave approach. The n- and i-layers consist of isotropic nonhomogeneous multilayered semiconductor.

Atalla, Mahmoud R. M.

2014-03-01

100

GB6 J1058+5628: A NEW QUASI-PERIODIC BL LAC OBJECT FROM THE ASIAGO PLATE ARCHIVE  

SciTech Connect

We present the historic photographic light curves of three little known blazars (two BL Lac objects and one FSRQ), GB6 J1058+5628, GB6 J1148+5254, and GB6 J1209+4119, spanning a time interval of about 50 years, mostly built using the Asiago plate archive. All objects show evident long-term variability, over which short-term variations are superposed. One source, GB6 J1058+5628, showed a marked quasi-periodic variability of 1 mag on timescale of about 6.3 years, making it one of the few BL Lac objects with a quasi-periodic behavior.

Nesci, R., E-mail: roberto.nesci@uniroma1.i [Physics Department, University of Roma La Sapienza, Piazzale A. Moro 2, I-00185 Roma (Italy)

2010-06-15

101

A Model for Backscattering from Quasi Periodic Corn Canopies at L-Band  

NASA Technical Reports Server (NTRS)

In this study, a model for backscattering at L-band from a corn canopy is proposed. The canopy consists of a quasi-periodic distribution of stalks and a random distribution of leaves. The Distorted Born Approximation (DBA) is employed to calculate the single scattered return from the corn field. The new feature of the method is that the coherence of the stalks in the row direction is incorporated in the model in a systematic fashion. Since the wavelength is on the order of the distance between corn stalks in a row, grating lobe behavior is observed at certain azimuth angles of incidence. The results are compared with experimental values measured in Huntsville, Alabama in 1998. The mean field and the effective dielectric constant of the canopy are obtained by using the Foldy approximation. The stalks are placed in the effective medium in a two dimensional lattice to simulate the row structure of a corn field. In order to mimic a real corn field, a quasi-periodic stalk distribution is assumed where the stalks are given small random perturbations about their lattice locations. Corn leaves are also embedded in the effective medium and the backscattered field from the stalks and the leaves is computed. The backscattering coefficient is calculated and averaged over successive stalk position perturbations. It is assumed that soil erosion has smoothed the soil sufficiently so that it can be assumed flat. Corn field backscatter data was collected from cornfields during the Huntsville 98 experimental campaign held at Alabama A&M University Research Station, Huntsville, Alabama in 1998 using the NASA/GW truck mounted radar. Extensive ground truth data was collected. This included soil moisture measurements and corn plant architectural data to be used in the model. In particular, the distances between the stalks in a single row have been measured. The L-band radar backscatter data was collected for both H and V polarizations and for look angles of 15o and 45o over a two week period under varying soil moisture conditions. These measured backscattering values will be compared with the model backscattering values and a discussion of the results will be presented.

Lang, R.; Utku, C.; Zhao, Q.; O'Neill, P.

2010-01-01

102

Combined in-situ and ground-based observations of quasi-periodic radar echoes  

NASA Astrophysics Data System (ADS)

A series of combined rocket/radar investigation of the electrodynamics and neutralplasma coupling associated with sporadic-E layers and quasi-periodic backscatter radar echoes has been carried out from launch sites at both Puerto Rico and the Wallops Flight Facility, Virginia (USA) between 1998-2001. The instrumented rockets consisted of main and sub-payloads and were launched while strong quasiperiodic VHF echoes were observed simultaneously with the Univ. of Illinois 50 MHz backscatter radar. The rocket apogee was purposely limited so that the payloads would dwell in the sporadic-E region (90-115 km). The main payload included vector DC and AC electric field detectors, a DC magnetometer, an ion mass spectrometer, an ionization gauge, and spaced-electric field receivers to measure the wavelength and phase velocity of the unstable plasma waves. The sub-payload was instrumented to measure DC and wave electric fields and plasma density. In one case, a separate rocket was launched a few minutes later which released luminous TMA trails to measure the neutral wind, its velocity shear, and embedded neutral structures. In this experiment, the payloads successfully pierced a well-defined, 2-3 km thick metallic sporadic-E layer of approximately 10**5 e/cc near 103 km altitude. In-situ DC electric field measurements revealed ~5mV/m ambient meridional fields above and below the layer with 1-2 mV/m amplitude, large scale structures superimposed. The wavelengths of these structures were approximately 2-4 km and may be related to the seat of the quasiperiodic echoes. Intense (~5 mV/m), higher frequency (shorter scale) broadband waves were also observed in-situ, both above and below the layer, consistent with the VHF backscatter observations during the time of the launch. Neither the large scale nor short scale plasma waves appeared to be distinctly organized by the sporadic-E density layer. The TMA release showed large amplitude (~ 100 m/s) meridional winds near 102-105 km, with the most intense shears directly below these altitudes, where the short scale electric field fluctuations were most intense. We summarize the observations from the different experiments and discuss them in the context of current theories regarding quasi-periodic echoes.

Pfaff, R.; Kudeki, E.; Larsen, M.; Clemmons, J.; Earle, G.

103

A parsec-scale 'superjet' and quasi-periodic structure in the HH 34 outflow?  

NASA Astrophysics Data System (ADS)

We report the detection of a new Herbig-Haro (HH) object, HH 173, near the young stellar object HH 34* in the L1641 molecular cloud in Orion. The new object appears to be part of a remarkable bipolar chain that includes known HH objects in this region and extends symmetrically about HH 34* for 1.5 pc. The chain terminates in the north at the position of HH 33 and includes HH 40, HH 85, HH 126, and HH 34N. Toward the south, the chain ends at the position of HH 88 and includes HH 87, HH 86, HH 173, HH 34X, HH 34, and the HH 34 jet. All HH objects in the chain that have recognizable bow shock morphologies point to a driving source in the HH 34* cloud core. We propose that this chain delineates a 3 pc long bipolar outflow from HH 34* with blueshifted gas in the south and redshifted gas in the north. The quasi-periodic spacing of the HH objects may be a consequence of episodic mass-loss events from HH 34* occurring roughly every 900/V300 yr (for a flow velocity V300 measured in units of 300 km/sec). The dynamic age of the most distant HH object from HH 34* is approximately 5000 yr. The S-shaped symmetry of the HH objects about the central source may result from jet precession with a period of approximately 104 yr.

Bally, John; Devine, David

1994-06-01

104

Submillimeter Quasi-periodic Oscillations in Magnetically Choked Accretion Flow Models of SgrA*  

NASA Astrophysics Data System (ADS)

High-frequency quasi-periodic oscillations (QPOs) appear in general-relativistic magnetohydrodynamic simulations of magnetically choked accretion flows around rapidly rotating black holes (BHs). We perform polarized radiative transfer calculations with the ASTRORAY code to explore the manifestations of these QPOs for SgrA*. We construct a simulation-based model of a radiatively inefficient accretion flow and find model parameters by fitting the mean polarized source spectrum. The simulated QPOs have a total submillimeter flux amplitude up to 5% and a linearly polarized flux amplitude up to 2%. The oscillations reach high levels of significance 10?-30? and high-quality factors Q ? 5. The oscillation period T ? 100 M ? 35 minutes corresponds to the rotation period of the BH magnetosphere that produces a trailing spiral in resolved disk images. The total flux signal is significant over noise for all tested frequencies 87 GHz, 230 GHz, and 857 GHz and inclination angles 10°, 37°, and 80°. The non-detection in the 230 GHz SubMillimeter Array light curve is consistent with a low signal level and a low sampling rate. The presence of submillimeter QPOs in SgrA* will be better tested with the Atacama Large Millimeter Array.

Shcherbakov, Roman V.; McKinney, Jonathan C.

2013-09-01

105

Search for Persistent Quasi-Periodicities in the Solar and Interplanetary Magnetic Fields  

NASA Astrophysics Data System (ADS)

Previous analysis of the radial component of the interplanetary magnetic field from 1962 - 1998 has revealed a dominant frequency of 27.03 days to 0.02 day accuracy (Neugebauer, et al., 2000). We have repeated and extended this analysis with OMNI data from 1963 - 2007 obtained from the Coordinated Heliospheric Observations (COHO) database. Over this longer data string we find that the 27.03 day Lomb-Scargle periodogram peak is reduced while two side peaks near 26.8 days and 27.6 days become almost as strong. In the interval 1999-2007 there are two dominant periods near 26.5 days and 27.2 days. As a solar counterpart to the above analysis we have searched for persistent rotation periods near 27 days of global patterns of photospheric magnetic fields derived from Wilcox Solar Observatory synoptic Carrington rotation maps. Techniques applied include, principal components analysis, independent component analysis, singular spectrum analysis, wavelet spectral analysis, and complex demodulation. We find a variety of quasi- periodicities between 26 and 29 days that remain coherent for 1 - 2 years. In the southern solar hemisphere the strongest periodicity is at 28.2 days, while in the northern hemisphere it is around 26.5 days. Neugebauer, M., Smith, Smith, E.J., Ruzmaikin, A., Feynman, J., Vaughan, A.H. 2000, J. Geophys. Res., 106, A5, 8363.

Lawrence, J. K.; Cadavid, A. C.; Ruzmaikin, A.

2007-12-01

106

High-frequency quasi-periodic oscillations in black hole binaries  

NASA Astrophysics Data System (ADS)

We present the results of the analysis of a large data base of X-ray observations of 22 galactic black hole transients with the Rossi X-Ray Timing Explorer throughout its operative life for a total exposure time of ˜12 ms. We excluded persistent systems and the peculiar source GRS 1915+105, as well as the most recently discovered sources. The semi-automatic homogeneous analysis was aimed at the detection of high-frequency (100-1000 Hz) quasi-periodic oscillations (QPO), of which several cases were previously reported in the literature. After taking into account the number of independent trials, we obtained 11 detections from two sources only: XTE J1550-564 and GRO J1655-40. For the former, the detected frequencies are clustered around 180 and 280 Hz, as previously found. For the latter, the previously reported dichotomy 300-450 Hz is found to be less sharp. We discuss our results in comparison with kHz QPO in neutron-star X-ray binaries and the prospects for future timing X-ray missions.

Belloni, T. M.; Sanna, A.; Méndez, M.

2012-11-01

107

The X-ray binary analogy to the first AGN quasi-periodic oscillation  

NASA Astrophysics Data System (ADS)

The narrow line Seyfert 1 galaxy REJ 1034+396 is so far unique amongst active galaxies (AGN) in showing a quasi-periodic oscillation (QPO) in its variability power spectrum. There are multiple types of QPO seen in black hole binary (BHB) systems, so we need to identify which BHB QPO corresponds to the one seen in the AGN. A key hint is the `hot disc dominated' energy spectrum of REJ 1034+396 which is sufficiently unusual that it suggests a mildly super-Eddington flow, also favoured by the most recent mass estimates for the AGN. This suggests the 67 Hz QPO seen occasionally in the mildly super-Eddington BHB GRS 1915+105 as the most likely counterpart, assuming mass scaling of the QPO frequency. This is supported by the fact that these data from GRS 1915+105 have an energy spectrum which is also dominated by a `hot disc' component. Here we show that the underlying broad band power spectral shape and normalization are also similar, providing further consistency checks for this identification. Thus the AGN QPO adds to the growing evidence for a simple mass scaling of the accretion flow properties between stellar and supermassive black holes.

Middleton, Matthew; Done, Chris

2010-03-01

108

Correlation between spectral state and quasi-periodic oscillation parameters in GX 5-1  

SciTech Connect

In a series of seven Exosat observations, the bimodal spectral behavior and the quasi-periodic oscillation (QPO)/red noise properties of GX 5-1 show a strict correlation. In one of the two spectral states (characterized by a 'horizontal branch' in the hardness-intensity diagram), strong 20-40 Hz QPO and red noise below about 60 Hz were always present. In the other ('normal branch'), no QPO between 6 and 60 Hz or red noise above 1 Hz were detected, but there was an indication for weak QPO near 5 Hz. In both states 'very low frequency noise' (VLFN) is detected below 0.1 Hz which has a power-law shape and and which extends down to the lowest observed frequencies (0.0001 Hz). The VLFN is probably not directly related to the QPO. The results are compared to those on Sco X-1 and Cyg X-2 and it is concluded that, although all three sources show bimodal spectral and QPO/red noise behavior, there is a qualitative difference between GX 5-1 and Cyg X-2 on one hand and Sco X-1 on the other. 25 references.

Van der klis, M.; Jansen, F.; Van paradijs, J.; Lewin, W.H.G.; Sztajno, M.

1987-02-01

109

Discovery of Millihertz ULTRAVIOLET Quasi-periodic Oscillations in Hercules X-1  

NASA Astrophysics Data System (ADS)

Observations of the ultraviolet continuum of the X-ray binary system Her X-1/HZ Herculis with the Space Telescope Imaging Spectrograph on the Hubble Space Telescope (HST) show quasi-periodic oscillations (QPOs) at frequencies of 8+/-2 and 43+/-2 mHz, with rms amplitudes of 2% and 4% of the steady flux. Observations with the Keck Telescope confirm the presence of the higher frequency QPO in the optical continuum, with a rms amplitude of 1.6%+/-0.2%. The QPOs are most prominent in the HST data near ?=0.5 (where ?=0 is the middle of the X-ray eclipse), suggesting that they arise not in the accretion disk but on the X-ray-heated face of the companion star. We discuss scenarios in which the companion star reprocesses oscillations in the disk which are caused by either Keplerian rotation or a beat frequency between the neutron star spin and Keplerian rotation at some radius in the accretion disk.

Boroson, Bram; O'Brien, Kieran; Horne, Keith; Kallman, Timothy; Still, Martin; Boyd, Patricia T.; Quaintrell, Hannah; Vrtilek, Saeqa Dil

2000-12-01

110

Kilo-Second Quasi-Periodic Oscillations in the Cataclysmic Variable DW Cancri  

NASA Astrophysics Data System (ADS)

Our photometric monitoring revealed that DWCnc, which was originally classified as a dwarf nova (V=15 - 17.5) remained at a bright state of Rc=14.68 +/- 0.07 for 61days. In conjunction with optical spectra lacking a strong He II emission line, we propose that the object is not a dwarf nova, but a non-magnetic nova-like variable. Throughout our monitoring, the object showed strong quasi-periodic oscillations (QPOs) with amplitudes reaching about 0.3mag. Our period analysis yielded a power spectrum with two peaks of QPOs, whose center periods are 37.5 +/- 0.1 and 73.4 +/- 0.4 min and, furthermore, with a significant power in frequencies lower than the QPOs. DWCnc is a unique cataclysmic variable in which kilo-second QPOs were continuously detected for 61days. We propose two possible interpretations of DWCnc: (i) A permanent superhumper below the period minimum of hydrogen-rich cataclysmic variab les. (ii) A nova-like variable having an orbital period over 3hours. In this case, the QPOs may be caused by trapped disk oscillations.

Uemura, Makoto; Kato, Taichi; Ishioka, Ryoko; Novak, Rudolf; Pietz, Jochen

2002-04-01

111

Conjugate observations of quasi-periodic emissions by Cluster and DEMETER spacecraft  

NASA Astrophysics Data System (ADS)

Abstract<p label="1"><span class="hlt">Quasi-periodic</span> (QP) emissions are electromagnetic emissions at frequencies of about 0.5-4 kHz that are characterized by a periodic time modulation of the wave intensity. Typical periods of this modulation are on the order of minutes. We present a case study of a large-scale long-lasting QP event observed simultaneously on board the DEMETER (Detection of Electro-Magnetic Emissions Transmitted from Earthquake Regions) and the Cluster spacecraft. The measurements by the Wide-Band Data instrument on board the Cluster spacecraft enabled us to obtain high-resolution frequency-time spectrograms of the event close to the equatorial region over a large range of radial distances, while the measurements by the STAFF-SA instrument allowed us to perform a detailed wave analysis. Conjugate observations by the DEMETER spacecraft have been used to estimate the spatial and temporal extent of the emissions. The analyzed QP event lasted as long as 5 h and it spanned over the L-shells from about 1.5 to 5.5. Simultaneous observations of the same event by DEMETER and Cluster show that the same QP modulation of the wave intensity is observed at the same time at very different locations in the inner magnetosphere. ULF magnetic field fluctuations with a period roughly comparable to, but somewhat larger than the period of the QP modulation were detected by the fluxgate magnetometers instrument on board the Cluster spacecraft near the equatorial region, suggesting these are likely to be related to the QP generation. Results of a detailed wave analysis show that the QP emissions detected by Cluster propagate unducted, with oblique wave normal angles at higher geomagnetic latitudes.</p> <div class="credits"> <p class="dwt_author">N?Mec, F.; SantolíK, O.; Parrot, M.; Pickett, J. S.; Hayosh, M.; Cornilleau-Wehrlin, N.</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">112</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/22086218"> <span id="translatedtitle">MASS-ANGULAR-MOMENTUM RELATIONS IMPLIED BY MODELS OF TWIN PEAK <span class="hlt">QUASI-PERIODIC</span> OSCILLATIONS</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">Twin peak <span class="hlt">quasi-periodic</span> oscillations (QPOs) appear in the X-ray power-density spectra of several accreting low-mass neutron star (NS) binaries. Observations of the peculiar Z-source Circinus X-1 display unusually low QPO frequencies. Using these observations, we have previously considered the relativistic precession (RP) twin peak QPO model to estimate the mass of the central NS in Circinus X-1. We have shown that such an estimate results in a specific mass-angular-momentum (M - j) relation rather than a single preferred combination of M and j. Here we confront our previous results with another binary, the atoll source 4U 1636-53 that displays the twin peak QPOs at very high frequencies, and extend the consideration to various twin peak QPO models. In analogy to the RP model, we find that these imply their own specific M - j relations. We explore these relations for both sources and note differences in the {chi}{sup 2} behavior that represent a dichotomy between high- and low-frequency sources. Based on the RP model, we demonstrate that this dichotomy is related to a strong variability of the model predictive power across the frequency plane. This variability naturally comes from the radial dependence of characteristic frequencies of orbital motion. As a consequence, the restrictions on the models resulting from observations of low-frequency sources are weaker than those in the case of high-frequency sources. Finally we also discuss the need for a correction to the RP model and consider the removing of M - j degeneracies, based on the twin peak QPO-independent angular momentum estimates.</p> <div class="credits"> <p class="dwt_author">Toeroek, Gabriel; Bakala, Pavel; Sramkova, Eva; Stuchlik, Zdenek; Urbanec, Martin; Goluchova, Katerina, E-mail: pavel.bakala@fpf.slu.cz, E-mail: martin.urbanec@fpf.slu.cz, E-mail: zdenek.stuchlik@fpf.slu.cz, E-mail: terek@volny.cz, E-mail: sram_eva@centrum.cz [Institute of Physics, Faculty of Philosophy and Science, Silesian University in Opava, Bezrucovo nam. 13, CZ-746 01 Opava (Czech Republic)</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-12-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">113</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/22127185"> <span id="translatedtitle">SOFT LAGS IN NEUTRON STAR kHz <span class="hlt">QUASI-PERIODIC</span> OSCILLATIONS: EVIDENCE FOR REVERBERATION?</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">High frequency soft reverberation lags have now been detected from stellar mass and supermassive black holes. Their interpretation involves reflection of a hard source of photons onto an accretion disk, producing a delayed reflected emission, with a time lag consistent with the light travel time between the irradiating source and the disk. Independently of the location of the clock, the kHz <span class="hlt">quasi-periodic</span> oscillation (QPO) emission is thought to arise from the neutron star boundary layer. Here, we search for the signature of reverberation of the kHz QPO emission, by measuring the soft lags and the lag energy spectrum of the lower kHz QPOs from 4U1608-522. Soft lags, ranging from {approx}15 to {approx}40 {mu}s, between the 3-8 keV and 8-30 keV modulated emissions are detected between 565 and 890 Hz. The soft lags are not constant with frequency and show a smooth decrease between 680 Hz and 890 Hz. The broad band X-ray spectrum is modeled as the sum of a disk and a thermal Comptonized component, plus a broad iron line, expected from reflection. The spectral parameters follow a smooth relationship with the QPO frequency, in particular the fitted inner disk radius decreases steadily with frequency. Both the bump around the iron line in the lag energy spectrum and the consistency between the lag changes and the inferred changes of the inner disk radius, from either spectral fitting or the QPO frequency, suggest that the soft lags may indeed involve reverberation of the hard pulsating QPO source on the disk.</p> <div class="credits"> <p class="dwt_author">Barret, Didier, E-mail: didier.barret@irap.omp.eu [Universite de Toulouse, UPS-OMP, IRAP, F-31400 Toulouse (France); CNRS, Institut de Recherche en Astrophysique et Planetologie, 9 Av. colonel Roche, BP 44346, F-31028 Toulouse cedex 4 (France)</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-06-10</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">114</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/22016134"> <span id="translatedtitle">MILLIHERTZ <span class="hlt">QUASI-PERIODIC</span> OSCILLATIONS AND THERMONUCLEAR BURSTS FROM TERZAN 5: A SHOWCASE OF BURNING REGIMES</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">We present a comprehensive study of the thermonuclear bursts and millihertz <span class="hlt">quasi-periodic</span> oscillations (mHz QPOs) from the neutron star (NS) transient and 11 Hz X-ray pulsar IGR J17480-2446, located in the globular cluster Terzan 5. The increase in burst rate that we found during its 2010 outburst, when persistent luminosity rose from 0.1 to 0.5 times the Eddington limit, is in qualitative agreement with thermonuclear burning theory yet contrary to all previous observations of thermonuclear bursts. Thermonuclear bursts gradually evolved into a mHz QPO when the accretion rate increased, and vice versa. The mHz QPOs from IGR J17480-2446 resemble those previously observed in other accreting NSs, yet they feature lower frequencies (by a factor {approx}3) and occur when the persistent luminosity is higher (by a factor 4-25). We find four distinct bursting regimes and a steep (close to inverse cubic) decrease of the burst recurrence time with increasing persistent luminosity. We compare these findings to nuclear burning models and find evidence for a transition between the pure helium and mixed hydrogen/helium ignition regimes when the persistent luminosity was about 0.3 times the Eddington limit. We also point out important discrepancies between the observed bursts and theory, which predicts brighter and less frequent bursts, and suggest that an additional source of heat in the NS envelope is required to reconcile the observed and expected burst properties. We discuss the impact of NS magnetic field and spin on the expected nuclear burning regimes, in the context of this particular pulsar.</p> <div class="credits"> <p class="dwt_author">Linares, M.; Chakrabarty, D. [Massachusetts Institute of Technology, Kavli Institute for Astrophysics and Space Research, Cambridge, MA 02139 (United States); Altamirano, D. [Astronomical Institute 'Anton Pannekoek', University of Amsterdam and Center for High-Energy Astrophysics, P.O. BOX 94249, 1090 GE Amsterdam (Netherlands); Cumming, A. [Department of Physics, McGill University, 3600 Rue University, Montreal, QC H3A 2T8 (Canada); Keek, L. [School of Physics and Astronomy, University of Minnesota, 116 Church Street SE, Minneapolis, MN 55455 (United States)</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-04-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">115</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2013EGUGA..15...52M"> <span id="translatedtitle">SDO/AIA observations of periodic and <span class="hlt">quasi-periodic</span> phenomenon associated with an EUV jet</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">It has long been advocated that explosive magnetic activity is responsible for the mass-balance in the solar atmosphere, supplying the corona and the solar wind with heated plasma. The explosive events are thought to be the result of emerging bi-polar (EB) regions reconnecting with pre-existing, open fields, with the size of the EB's (i.e., granular, super-granular) being related to size of the resulting feature (i.e., spicules, EUV/X-ray jets). Recent evidence has suggested a deeper relationship between spicules and EUV jets (Sterling et al., 2010). We present here observations of a EUV jet observed with SDO/AIA close to a southern coronal hole. The jet can be considered as a 'Blowout jet' (using the terminology of Moore et al., 2010), launching vast amounts of chromospheric plasma into the atmosphere along with hotter material. The hotter part of the jet appears to be composed of multiple, (<span class="hlt">quasi-)periodic</span> ejections that individually resemble fast moving (>100 km/s) spicules. The multiple ejections appear crucial for distributing the hotter material high into the corona, possibly suggesting that larger EUV/X-ray are composed of many smaller spicule-like events. Although the event is close to the limb, evidence for reconnection at the chromospheric level is provided. Further, evidence for helicity (or torsional motion) and the presence of slow and fast Magnetohydrodynamic waves is given, with the wave mode excitation likely due to the reconnection process. Exploiting the observed wave motion, we also use magneto-seismological techniques to determine local plasma parameters with sub-resolution accuracy along one of the jets unique features.</p> <div class="credits"> <p class="dwt_author">Morton, Richard; Verth, Gary; Erdelyi, Robertus; Srivastava, Abhi</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-04-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">116</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=20030022796&hterms=neutron+stars&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D50%26Ntt%3Dneutron%2Bstars"> <span id="translatedtitle">Effects of Resonance in <span class="hlt">Quasi-Periodic</span> Oscillators of Neutron Star Binaries</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">Using a large quantity of Rossi X-Ray Timing Explorer data presented in the literature, I offer a detailed investigation into the accuracy of the <span class="hlt">quasi-periodic</span> oscillation (QPO) frequency determination. The QPO phenomenon seen in X-ray binaries is possibly a result of the resonance of the intrinsic (eigen) oscillations and harmonic driving forces of the system. I show that the resonances, in the presence of the damping of oscillations, occur at frequencies that are systematically and randomly shifted with respect to the eigenfrequencies of the system. The shift value strongly depends on the damping rate that is measured by the half-width of the QPO feature. Taking into account this effect, I analyze the QPO data for four Z sources, Scorpius X-I, GX 340+0, GX 5-1, and GX 17+2, and two atoll sources, 4U 1728-34 and 4U 0614+09. The transition-layer model (TLM) predicts the existence of the invariant quantity delta, an inclination angle of the magnetospheric axis with respect to the normal to the disk. I calculate delta and the error bars of delta using the resonance shift, and I find that the inferred delta-values are consistent with constants for these four Z sources, in which horizontal-branch oscillation and kilohertz frequencies have been detected and correctly identified. It is shown that the inferred delta are in the range between 5.5 deg and 6.5 deg. I conclude that the TLM seems to be compatible with the data.</p> <div class="credits"> <p class="dwt_author">Titarchuk, Lev; White, Nicholas E. (Technical Monitor)</p> <p class="dwt_publisher"></p> <p class="publishDate">2002-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">117</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2012AGUFM.V33A2841B"> <span id="translatedtitle">The Hilbert-Huang Transform Applied to <span class="hlt">Quasi-Periodic</span> Volcanic Tremor</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">The Hilbert-Huang Transform (HHT) is applied to nonlinear, <span class="hlt">quasi-periodic</span> harmonic tremor on an erupting volcano to extract detailed variations in explosion dynamics. The HHT relies upon the Empirical Mode Decomposition (EMD) method to split signals into Intrinsic Mode Functions (IMFs) that are amenable to the Hilbert Transform. Instantaneous time/frequency/power traces of each transformed IMF can be combined to yield a composite Hilbert spectrogram of the signal's evolution through time. Unlike Fourier-based methods, the HHT does not use linear combinations of sinusoids to approximate signals. The advantage of the HHT is that it does not require its basis to be linear and stationary; furthermore, it can provide instantaneous amplitude and frequency for each sample in the data set. We use the HHT to examine tremor signals recorded at Santiaguito volcano, Guatemala, in 2009. The time interval between successive tremor pulses exhibits a linear relationship with amplitude over several sequences, suggesting a nonlinear process. This indicates that at least some of the pulse sequences cannot be modeled as sinusoidal signal. For this reason, the HHT, rather than a Fourier method, is used to examine how signal frequency and amplitude change through time. We focus on an example tremor signal that has both seismic and infrasound recordings. The infrasound portion of the example event includes two frequency modulated signals, one centered at 0.5 Hz and the other centered at 1 Hz. In contrast, the seismic portion of this event is a frequency modulated signal centered at 1 Hz with distributed energy in the 2-5 Hz range. Certain time intervals contain series of repeating frequency modulations that may indicate either nonlinear waveforms or the superposition of low amplitude riding waves on higher amplitude carrier waves. These frequency modulations do not correlate between infrasound and seismic records. Detailed deconstruction of the tremor via HHT provides a basis for examination of physical transients in the otherwise apparently harmonic signal. We have also applied the HHT method on harmonic tremor sequences at other volcanoes including Renventador and Karymsky.</p> <div class="credits"> <p class="dwt_author">Bowman, D. C.; Lees, J. M.; Johnson, J.</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-12-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">118</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2013MNRAS.435.2132M"> <span id="translatedtitle">The phase lags of high-frequency <span class="hlt">quasi-periodic</span> oscillations in four black hole candidates</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">We measured the phase-lag spectrum of the high-frequency <span class="hlt">quasi-periodic</span> oscillations (QPO) in the black hole systems (at QPO frequencies) GRS 1915+105 (35 Hz and 67 Hz), GRO J1655-40 (300 Hz and 450 Hz), XTE J1550-564 (180 Hz and 280 Hz) and IGR J17091-3624 (67 Hz). The lag spectra of the 67-Hz QPO in, respectively, GRS 1915+105 and IGR J17091-3624, and the 450-Hz QPO in GRO J1655-40 are hard (hard photons lag the soft ones) and consistent with each other, with the hard lags increasing with energy. On the contrary, the lags of the 35- Hz QPO in GRS 1915+105 are soft, with the lags becoming softer as the energy increases; the lag spectrum of the 35-Hz QPO is inconsistent with that of the 67-Hz QPO. The lags of the 300-Hz QPO in GRO J1655-40, and the 180-Hz and the 280-Hz QPO in XTE J1550-564 are independent of energy, consistent with each other and with being zero or slightly positive (hard lags). For GRO J1655-40, the lag spectrum of the 300-Hz QPO differs significantly from that of the 450-Hz QPOs. The similarity of the lag spectra of the 180-Hz and 280-Hz QPO in XTE J1550-564 suggests that these two are the same QPO seen at a different frequency in different observations. If this is correct, the lags could provide an alternative way to identify the high-frequency QPO features in galactic black hole systems. The lag spectrum of the 67-Hz QPO in GRS 1915+105 (hard lags) is significantly different from that of the 2.7 × 10-4 Hz QPO in the narrow-line Seyfert 1 galaxy RE J1034+396 (soft lags), which disproves the suggestion that the two QPOs are the same physical phenomenon with their frequencies scaled only by the black hole mass. The lag spectrum of the QPO in RE J1034+396 is similar to that of the 35-Hz QPO in GRS 1915+105, although identifying these two QPOs as being the same physical feature remains problematic. We compare our results with those for the lags of the kilohertz QPOs in neutron-star systems and the broad-band noise component in active galactic nuclei, and discuss possible scenarios for producing the lags in these systems.</p> <div class="credits"> <p class="dwt_author">Méndez, Mariano; Altamirano, Diego; Belloni, Tomaso; Sanna, Andrea</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-11-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">119</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2010PhLA..374.3001L"> <span id="translatedtitle">Bilinear approach to the <span class="hlt">quasi-periodic</span> wave solutions of Modified Nizhnik-Novikov-Vesselov equation in (2+1) dimensions</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">In the present Letter, by using Hirota bilinear method and Riemann theta function, the <span class="hlt">quasi-periodic</span> wave solutions are constructed for the (2+1)-dimensional Modified Nizhnik-Novikov-Vesselov equation, and we show asymptotic properties of the <span class="hlt">quasi-periodic</span> wave solutions.</p> <div class="credits"> <p class="dwt_author">Luo, Lin; Fan, Engui</p> <p class="dwt_publisher"></p> <p class="publishDate">2010-07-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">120</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/24487877"> <span id="translatedtitle">Rapid fabrication of a large-area close-packed <span class="hlt">quasi-periodic</span> microlens array on BK7 glass.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">Large-area close-packed microlens arrays (MLAs) are highly desirable for structured light and integrated optical applications. However, efficient realization of ultralarge area MLAs with a high fill factor is still technically challenging, especially on glass material. In this Letter we propose a high-efficiency MLA fabrication method using single-pulsed femtosecond laser wet etch and close-packed <span class="hlt">quasi-periodic</span> concave MLAs consisting of three million units fabricated on silica glass within an hour. The fabricated MLAs are demonstrated to have extreme optical smoothness (?8.5 nm) by an atomic force microscope. It has also been demonstrated that the profile of the <span class="hlt">quasi-periodic</span> concave structures could be easily tuned by changing the laser scanning speed or the pulse energy. Additionally, the optical performances of the MLA diffusers were investigated by using sharp focusing, high-resolution imaging, and flat-top illumination. PMID:24487877</p> <div class="credits"> <p class="dwt_author">Chen, Feng; Deng, Zefang; Yang, Qing; Bian, Hao; Du, Guangqing; Si, Jinhai; Hou, Xun</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-02-01</p> </div> </div> </div> </div> <div id="filter_results_form" class="filter_results_form floatContainer" style="visibility: visible;"> <div style="width:100%" id="PaginatedNavigation" class="paginatedNavigationElement"> <a id="FirstPageLink" onclick='return showDiv("page_1");' href="#" title="First Page"> <img id="FirstPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.first.18x20.png" alt="First Page" /></a> <a id="PreviousPageLink" onclick='return showDiv("page_5");' href="#" title="Previous Page"> <img id="PreviousPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.previous.18x20.png" alt="Previous Page" /></a> <span id="PageLinks" class="pageLinks"> <span> <a onClick='return showDiv("page_1");' href="#">1</a> <a 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<img id="NextPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.next.18x20.png" alt="Next Page" /></a> <a id="LastPageLink" onclick='return showDiv("page_25.0");' href="#" title="Last Page"> <img id="LastPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.last.18x20.png" alt="Last Page" /></a> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">121</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2011CeMDA.110...71H"> <span id="translatedtitle">On <span class="hlt">quasi-periodic</span> motions around the collinear libration points in the real Earth-Moon system</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Due to various perturbations, the collinear libration points of the real Earth-Moon system are not equilibrium points anymore. Under the assumption that the Moon's motion is <span class="hlt">quasi-periodic</span>, special <span class="hlt">quasi-periodic</span> orbits called dynamical substitutes exist. These dynamical substitutes replace the geometrical collinear libration points as time-varying equilibrium points. In the paper, the dynamical substitutes of the three collinear libration points in the real Earth-Moon system are computed. For the points L 1 and L 2, linearized motions around the dynamical substitutes are described, and the variational equations of the dynamical substitutes are reduced to a form with a near constant coefficient matrix. Then higher order analytical formulae of the central manifolds are constructed. Using these analytical solutions as initial seeds, Lissajous orbits and halo orbits are computed with numerical algorithms.</p> <div class="credits"> <p class="dwt_author">Hou, X. Y.; Liu, L.</p> <p class="dwt_publisher"></p> <p class="publishDate">2011-05-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">122</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2012AcAau..81..456P"> <span id="translatedtitle">Evolution of the out-of-plane amplitude for <span class="hlt">quasi-periodic</span> trajectories in the Earth-Moon system</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">The out-of-plane amplitude along <span class="hlt">quasi-periodic</span> trajectories in the Earth-Moon system is highly sensitive to perturbations in position and/or velocity as underscored recently by the ARTEMIS spacecraft. Controlling the evolution of the out-of-plane amplitude is non-trivial, but can be critical to satisfying mission requirements. The sensitivity of the out-of-plane amplitude evolution to perturbations due to lunar eccentricity, solar gravity, and solar radiation pressure is explored and a strategy for designing low-cost deterministic maneuvers to control the amplitude history is also examined. The method is sufficiently general and is applied to the L1 <span class="hlt">quasi-periodic</span> orbit that serves as a baseline for the ARTEMIS P2 trajectory.</p> <div class="credits"> <p class="dwt_author">Pavlak, Thomas A.; Howell, Kathleen C.</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-12-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">123</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2014EL....10540003L"> <span id="translatedtitle"><span class="hlt">Quasi-periodicity</span> of large avalanches in the long-range connective sandpile models and its implication in natural earthquakes</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">In this study, we investigated the <span class="hlt">quasi-periodicity</span> of large avalanches using a new modification of sandpile models, i.e., the long-range connective sandpile (LRCS) model. The LRCS model considers the random distant connection between two separated, instead of neighboring, cells and shows interesting precursory behavior before large avalanches. We explore the statistics of recurrence intervals between large events and find a strong dependence on the size L of the sandpile. In the LRCS model, the average recurrence interval W of large avalanches follows the relationship W\\propto L^{2.07} . Having the recurrence intervals of many earthquake fault systems around the world, we propose an empirical rule between those intervals and the corresponding earthquakes' magnitudes and provide evidence of the <span class="hlt">quasi-periodic</span> behavior of natural earthquakes.</p> <div class="credits"> <p class="dwt_author">Lee, Ya-Ting; Chen, Chien-chih; Lin, Chai-Yu; Chuang, Ya-Ting</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-02-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">124</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2014JCoPh.262..262B"> <span id="translatedtitle">Rapidly convergent two-dimensional <span class="hlt">quasi-periodic</span> Green function throughout the spectrum—including Wood anomalies</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">We introduce a new methodology, based on new <span class="hlt">quasi-periodic</span> Green functions which converge rapidly even at and around Wood-anomaly configurations, for the numerical solution of problems of scattering by periodic rough surfaces in two-dimensional space. As is well known the classical <span class="hlt">quasi-periodic</span> Green function ceases to exist at Wood anomalies. The approach introduced in this text produces fast Green function convergence throughout the spectrum on the basis of a certain "finite-differencing" approach and smooth windowing of the classical Green function lattice sum. The resulting Green-function convergence is super-algebraically fast away from Wood anomalies, and it reduces to an arbitrarily-high (user-prescribed) algebraic order of convergence at Wood anomalies.</p> <div class="credits"> <p class="dwt_author">Bruno, Oscar P.; Delourme, Bérangère</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-04-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">125</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2014JPhCS.482a2023K"> <span id="translatedtitle">Quantum corrections to <span class="hlt">quasi-periodic</span> solution of Sine-Gordon model and periodic solution of phi4 model</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Analytical form of quantum corrections to <span class="hlt">quasi-periodic</span> solution of Sine-Gordon model and periodic solution of phi4 model is obtained through zeta function regularisation with account of all rest variables of a d-dimensional theory. Qualitative dependence of quantum corrections on parameters of the classical systems is also evaluated for a much broader class of potentials u(x) = b2f(bx) + C with b and C as arbitrary real constants.</p> <div class="credits"> <p class="dwt_author">Kwiatkowski, G.; Leble, S.</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-03-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">126</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/18634977"> <span id="translatedtitle">Transmission Properties of <span class="hlt">Quasi-Periodic</span> Fibonacci One-Dimensional Photonic Crystal Containing Negative Permittivity\\/permeability Material</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">The transmission properties of one-dimensional <span class="hlt">quasi-periodic</span> Fibonacci photonic crystal containing negative permittivity\\/permeability material are investigated by use of the transfer matrix method. We find that perfect transmission peaks exist at a series of dimensionless wavelength points in the transmission spectra, and the discrete localized modes appear inside the photonic band gap in the case of normal incidence. In the case</p> <div class="credits"> <p class="dwt_author">Bo Tao; Fu-Li Li; Feng Yu</p> <p class="dwt_publisher"></p> <p class="publishDate">2007-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">127</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/12682823"> <span id="translatedtitle">Correlations in <span class="hlt">Quasi-periodic</span> Oscillation and Noise Frequencies among Neutron Star and Black Hole X-Ray Binaries</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">We study systematically the ~=0.1-1200 Hz <span class="hlt">quasi-periodic</span> oscillations (QPOs) and broad noise components observed in the power spectra of nonpulsing neutron star and black hole low-mass X-ray binaries. We show that among these components we can identify two, occurring over a wide range of source types and luminosities, whose frequencies follow a tight correlation. The variability components involved in this</p> <div class="credits"> <p class="dwt_author">Dimitrios Psaltis; Tomaso Belloni; Michiel van der Klis; W. H. G. Lewin; S. Dieters</p> <p class="dwt_publisher"></p> <p class="publishDate">1999-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">128</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/43144220"> <span id="translatedtitle">Lense-Thirring Precession and <span class="hlt">Quasi-periodic</span> Oscillations in Low-Mass X-Ray Binaries</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">Relativistic dragging of inertial frames around fast-rotating collapsed stars is substantial and can give rise to observable effects. We consider kHz <span class="hlt">quasi-periodic</span> oscillation (QPO) sources, low-mass X-ray binaries (LMXRBs) containing an accreting neutron star. Within beat frequency models, both the Keplerian frequency of the innermost region of the accretion disk ( ~0.3-1.2 kHz) and the neutron star spin frequency (</p> <div class="credits"> <p class="dwt_author">Luigi Stella; Mario Vietri</p> <p class="dwt_publisher"></p> <p class="publishDate">1998-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">129</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2009Nonli..22.1311C"> <span id="translatedtitle">Fast numerical computation of <span class="hlt">quasi-periodic</span> equilibrium states in 1D statistical mechanics, including twist maps</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">We develop fast algorithms to compute <span class="hlt">quasi-periodic</span> equilibrium states of one-dimensional models in statistical mechanics. The models considered include as particular cases Frenkel-Kontorova models, possibly with long-range interactions, Heisenberg XY models, possibly with long-range interactions as well as problems from dynamical systems such as twist mappings and monotone recurrences. In the dynamical cases, the <span class="hlt">quasi-periodic</span> solutions are KAM tori. The algorithms developed are highly efficient. If we discretize a <span class="hlt">quasi-periodic</span> function using N Fourier coefficients, the algorithms introduced here require O(N) storage and a Newton step for the equilibrium equation requires only O(N log(N)) arithmetic operations. These algorithms are also backed up by rigorous 'a posteriori estimates' that give conditions that ensure that approximate solutions correspond to true ones. We have implemented the algorithms and present comparisons of timings and accuracy with other algorithms. More substantially, we use the algorithms to study the analyticity breakdown transition, which for twist mappings becomes the breakdown of KAM tori. We use this method to explore the analyticity breakdown in some Frenkel-Kontorova models with extended interactions. In some ranges of parameters, we find that the breakdown presents scaling relations that, up to the accuracy of our calculations, are the same as those for the standard map. We also present results that indicate that, when the interactions decrease very slowly, the breakdown of analyticity is quantitatively very different.</p> <div class="credits"> <p class="dwt_author">Calleja, Renato; de la Llave, Rafael</p> <p class="dwt_publisher"></p> <p class="publishDate">2009-06-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">130</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/22066618"> <span id="translatedtitle">Spectral broadening and compression of high-intensity laser pulses in <span class="hlt">quasi-periodic</span> systems with Kerr nonlinearity</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">We report the results of theoretical studies and numerical simulations of optical high-power pulse compression systems based on the spectral broadening in a Kerr nonlinear medium with subsequent pulse compression in a dispersive delay line. It is shown that the effective spectral broadening requires suppressing a smallscale instability arising due to self-focusing, which is possible in <span class="hlt">quasi-periodic</span> systems consisting of a nonlinear medium and optical relay telescopes transmitting images of the laser beam through the system. The numerical calculations have shown the possibility of broadening the spectrum, followed by 15-fold pulse compression until the instability is excited. (control of laser radiation parameters)</p> <div class="credits"> <p class="dwt_author">Vlasov, Sergei N; Koposova, E V; Yashin, V E</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-11-30</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">131</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/4240099"> <span id="translatedtitle">Application of Computer Algebra for Construction of <span class="hlt">Quasi-periodic</span> Solutions for Restricted Circular Planar Three Body Problem</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">The algorithm is realized (with the help of computer algebra methods) for construction of numeric-analytical <span class="hlt">quasi-periodic</span>\\u000a solutions of precise(!) equations of restricted planar circular three-body problem (Sun–Jupiter-small planet) for an arbitrary\\u000a sufficiently wide variety of initial data. This algorithm and corresponding exe-code allows us to obtain solutions in automatic\\u000a mode (certainly, approximate but satisfying the motion equations with user-specified high</p> <div class="credits"> <p class="dwt_author">V. P. Borunov; Yu. A. Ryabov; O. V. Surkov</p> <p class="dwt_publisher"></p> <p class="publishDate">2006-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">132</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2012ApPhL.101v1901S"> <span id="translatedtitle">Fabrication of <span class="hlt">quasi-periodic</span> surface microcavities by selective etching of self-organized superalloys for high-temperature photonics</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Large-area fabrication of periodic microstructures on refractory metals surface is a key technology supporting the practical application of spectrally controlled thermal radiation using surface microcavities. This report describes large-area fabrication of two-dimensional submicron <span class="hlt">quasi-periodic</span> microcavities using self-organization on a nickel-based superalloy. The surface microcavities on a bulk metal are obtained by heat treatment and simple chemical etching. The emission peak attributed to the confined modes inside cavities can be tuned by controlling the microcavity size from 0.27 to 0.53 ?m. Emittance enhancement and thermal stability are also confirmed at 973 K.</p> <div class="credits"> <p class="dwt_author">Shimizu, Makoto; Konno, Kiyotaka; Iguchi, Fumitada; Yugami, Hiroo</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-11-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">133</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2013OptEL...9..289W"> <span id="translatedtitle">Extraordinary optical properties of Fibonacci <span class="hlt">quasi-periodic</span> 1D superconducting photonic crystals in near-zero-permittivity operation range</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">In near-zero-permittivity operation range, the position-dependent extraordinary optical properties of a one dimensional (1D) Fibonacci <span class="hlt">quasi-periodic</span> superconducting photonic crystal (PC), which consists of alternating superconductor and dielectric layers, are theoretically investigated by using the transfer matrix method. Based on the calculated reflectance spectrum, it is shown that the extraordinary optical properties depend on the relative positions of the threshold wavelength and the photonic band gaps (PBGs). By suitably choosing the thickness of the superconducting or dielectric layer, a transmission narrow band filter or resonator can be designed without introducing any physical defect in this structure.</p> <div class="credits"> <p class="dwt_author">Wu, Ji-jiang; Gao, Jin-xia</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-07-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">134</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/5345988"> <span id="translatedtitle"><span class="hlt">Quasi-periodic</span> oscillations in the X-ray flux of the rapid burster (MXB 1730-335)</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">The results of an Exosat observation of the Rapid Burster in August 1985 during an active state are presented. Forty 1-10 minute long type 2 bursts were detected together with constant emission. <span class="hlt">Quasi-periodic</span> oscillations (QPOs) were observed in 23 bursts with frequencies in the range of 2-5 Hz. Obscuration of the central X-ray source by an oscillating accretion disk rim is suggested as a possible scenario for the generation of the QPO from the Rapid Burster. 68 references.</p> <div class="credits"> <p class="dwt_author">Stella, L.; Haberl, F.; Parmar, A.N.; Lewin, W.H.G.; Van paradijs, J.</p> <p class="dwt_publisher"></p> <p class="publishDate">1988-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">135</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/27706773"> <span id="translatedtitle">Sonic-Point Model of Kilohertz <span class="hlt">Quasi-Periodic</span> Brightness Oscillations in Low-Mass X-ray Binaries</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">Strong, coherent, <span class="hlt">quasi-periodic</span> brightness oscillations (QPOs) with\\u000afrequencies ranging from about 300 Hz to 1200 Hz have been discovered with the\\u000aRossi X-ray Timing Explorer in the X-ray emission from some fifteen neutron\\u000astars in low-mass binary systems. Two simultaneous kilohertz QPOs differing in\\u000afrequency by 250 to 350 Hertz have been detected in twelve of the fifteen\\u000asources. Here</p> <div class="credits"> <p class="dwt_author">M. Coleman Miller; Frederick K. Lamb; Dimitrios Psaltis</p> <p class="dwt_publisher"></p> <p class="publishDate">1996-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">136</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2009MNRAS.392..264S"> <span id="translatedtitle">The magnetohydrodynamics model of twin kilohertz <span class="hlt">quasi-periodic</span> oscillations in low-mass X-ray binaries</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">We suggest an explanation for the twin kilohertz <span class="hlt">quasi-periodic</span> oscillations (kHz QPOs) in low-mass X-ray binaries (LMXBs) based on magnetohydrodynamics (MHD) oscillation modes in neutron star magnetospheres. Including the effect of the neutron star spin, we derive several MHD wave modes by solving the dispersion equations, and propose that the coupling of the two resonant MHD modes may lead to the twin kHz QPOs. This model naturally relates the upper, lower kHz QPO frequencies with the spin frequencies of the neutron stars, and can well account for the measured data of six LMXBs.</p> <div class="credits"> <p class="dwt_author">Shi, Changsheng; Li, Xiang-Dong</p> <p class="dwt_publisher"></p> <p class="publishDate">2009-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">137</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2012SSCom.152.2113Z"> <span id="translatedtitle">Omnidirectional photonic band gaps enlarged by Fibonacci <span class="hlt">quasi-periodic</span> one-dimensional ternary superconductor photonic crystals</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">First two omnidirectional photonic band gaps (OBGs) realized by one-dimensional (1D) Fibonacci <span class="hlt">quasi-periodic</span> structure which is composed of superconductor and two kinds of isotropic dielectric are theoretically studied by the transfer matrix method (TMM). From the numerical results, it has been shown that such OBGs are insensitive to the incident angle and the polarization of electromagnetic wave (EM wave), and the frequency ranges and central frequencies of OBGs cease to change with increasing Fibonacci order, but vary with the ambient temperature of system and the thickness of the superconductor, respectively. The bandwidths of OBGs can be notably enlarged. The damping coefficient of superconductor layers has no effect on the frequency ranges of OBGs. Those OBGs originate from a Bragg gap in contrast to zero-n˜ gap or single negative (negative permittivity or negative permeability) gap. It has been proved that Fibonacci <span class="hlt">quasi-periodic</span> 1D ternary superconductor dielectric photonic crystals (SDPCs) have a superior feature in the enhancement of OBGs frequency ranges compared with the conventional binary dielectric photonic crystals (DPCs).</p> <div class="credits"> <p class="dwt_author">Zhang, Hai-Feng; Liu, Shao-Bin; Kong, Xiang-Kun; Bian, Bo-Rui; Dai, Yi</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-12-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">138</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=19910055709&hterms=voronoi&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3D%2522voronoi%2522"> <span id="translatedtitle"><span class="hlt">Quasi-periodic</span> structures in the large-scale galaxy distribution and three-dimensional Voronoi tessellation</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">It has been suggested that the void and wall structure associated with the large-scale galaxy distribution might be qualitatively, or perhaps even physically, modeled by a Voronoi tessellation, and that such structure might account for the surprisingly regular, sharp peaks in the galaxy redshift distributions obtained from 'pencil beam' surveys. Taking cell wall crossings by random line segments to correspond to such redshift peaks, an exact expression is derived for the distribution of spacings of these intersections in a three-dimensional Voronoi tessellation. This result verifies that the spacings are nonrandom and <span class="hlt">quasi-periodic</span>, qualitatively resembling the observed pattern, even though the cell wall structure is generated from randomly placed seeds. Finally, moments of the spacing distribution are used to show that apparently periodic samples, similar to those recently reported, represent only one to two sigma fluctuations in a Voronoi tesselation.</p> <div class="credits"> <p class="dwt_author">Ikeuchi, Satoru; Turner, Edwin L.</p> <p class="dwt_publisher"></p> <p class="publishDate">1991-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">139</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2012ASPC..466..225P"> <span id="translatedtitle">Constraining the Mass and Moment of Inertia of Neutron Stars from <span class="hlt">Quasi-Periodic</span> Oscillations in X-ray Binaries</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">We put some constraints on the mass and moment of inertia of neutron stars based on the interpretation of high-frequency <span class="hlt">quasi-periodic</span> oscillations (HF-QPOs) observed in low mass X-ray binaries (LMXBs). We use available HF-QPOs observations to look for the average mass and moment of inertia of neutron stars by applying our parametric resonance model to discriminate between slow and fast rotators in relation with the innermost stable circular orbit (ISCO). We find an average mass M* ? (2.0 - 2.2) M?. The corresponding average moment of inertia is then I* ? (1 - 3) × 1038kg m2 ? (0.5 - 1.5) (10 km)2 M?.</p> <div class="credits"> <p class="dwt_author">Pétri, J.</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-12-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">140</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2013AcA....63..275K"> <span id="translatedtitle">Multi-Resonance Orbital Model Applied to High-Frequency <span class="hlt">Quasi-Periodic</span> Oscillations Observed in Sgr A*</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">The multi-resonance orbital model of high-frequency <span class="hlt">quasi-periodic</span> oscillations (HF QPOs) enables precise determination of the black hole dimensionless spin a if observed set of oscillations demonstrates three (or more) commensurable frequencies. The black hole spin a is related to the frequency ratio only, while its mass M is related to the frequency magnitude. The model is applied to the triple frequency set of HF QPOs observed in Sgr A* source with frequency ratio 3:2:1. Acceptable versions of the multi-resonance model are determined by the restrictions on the Sgr A* supermassive black hole mass. The version of strong resonances related to the black hole "magic" spin a=0.983 is acceptable but the version demonstrating the best agreement with the mass restrictions predicts spin a=0.980.</p> <div class="credits"> <p class="dwt_author">Kotrlová, A.; Stuchlík, Z.; Török, G.</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-06-01</p> </div> </div> </div> </div> <div id="filter_results_form" class="filter_results_form floatContainer" style="visibility: visible;"> <div style="width:100%" id="PaginatedNavigation" class="paginatedNavigationElement"> <a id="FirstPageLink" onclick='return showDiv("page_1");' href="#" title="First Page"> <img id="FirstPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.first.18x20.png" alt="First Page" /></a> <a id="PreviousPageLink" onclick='return showDiv("page_6");' href="#" title="Previous Page"> <img id="PreviousPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.previous.18x20.png" 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showDiv("page_25");' href="#">25</a> </span> </span> <a id="NextPageLink" onclick='return showDiv("page_9");' href="#" title="Next Page"> <img id="NextPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.next.18x20.png" alt="Next Page" /></a> <a id="LastPageLink" onclick='return showDiv("page_25.0");' href="#" title="Last Page"> <img id="LastPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.last.18x20.png" alt="Last Page" /></a> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">141</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2013MeScT..24e5305P"> <span id="translatedtitle">Phase identification of <span class="hlt">quasi-periodic</span> flow measured by particle image velocimetry with a low sampling rate</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">This work mainly deals with the proper orthogonal decomposition (POD) time coefficient method used for extracting phase information from <span class="hlt">quasi-periodic</span> flow. The mathematical equivalence between this method and the traditional cross-correlation method is firstly proved. A two-dimensional circular cylinder wake flow measured by time-resolved particle image velocimetry within a range of Reynolds numbers is then used to evaluate the reliability of this method. The effect of both the sampling rate and Reynolds number on the identification accuracy is finally discussed. It is found that the POD time coefficient method provides a convenient alternative for phase identification, whose feasibility in low-sampling-rate measurement has additional advantages for experimentalists.</p> <div class="credits"> <p class="dwt_author">Pan, Chong; Wang, Hongping; Wang, Jinjun</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-05-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">142</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=19910057597&hterms=Imamura&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D10%26Ntt%3DImamura"> <span id="translatedtitle">Noise-driven radiative shocks - A new model for the optical <span class="hlt">quasi-periodic</span> oscillations of the AM Herculis objects</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">A model for the 0.3-1.2 Hz optical <span class="hlt">quasi-periodic</span> oscillations (QPOs) observed in a number of AM Her-type binary systems has been developed. It is suggested that the observed optical modulation is the result of shock oscillations induced by nonsteady accretion flows. It is shown that time-dependent models of radiative shock waves in nonsteady accretion flows onto magnetic white dwarfs with mass 0.6 solar mass and magnetic field strength of 30 MG can produce optical QPOs similar to those observed in the AM Her objects. Theoretical calculations have shown that oscillations cannot be sustained for these white dwarf parameters when the accretion rate is constant.</p> <div class="credits"> <p class="dwt_author">Wolff, Michael T.; Wood, Kent S.; Imamura, James N.</p> <p class="dwt_publisher"></p> <p class="publishDate">1991-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">143</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=19930062263&hterms=Imamura&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3DImamura"> <span id="translatedtitle">The <span class="hlt">quasi-periodic</span> oscillations and very low frequency noise of Scorpius X-1 as transient chaos - A dripping handrail?</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">We present evidence that the <span class="hlt">quasi-periodic</span> oscillations (QPO) and very low frequency noise (VLFN) characteristic of many accretion sources are different aspects of the same physical process. We analyzed a long, high time resolution EXOSAT observation of the low-mass X-ray binary (LMXB) Sco X-1. The X-ray luminosity varies stochastically on time scales from milliseconds to hours. The nature of this variability - as quantified with both power spectrum analysis and a new wavelet technique, the scalegram - agrees well with the dripping handrail accretion model, a simple dynamical system which exhibits transient chaos. In this model both the QPO and VLFN are produced by radiation from blobs with a wide size distribution, resulting from accretion and subsequent diffusion of hot gas, the density of which is limited by an unspecified instability to lie below a threshold.</p> <div class="credits"> <p class="dwt_author">Scargle, Jeffrey D.; Steiman-Cameron, Thomas; Young, Karl; Donoho, David L.; Crutchfield, James P.; Imamura, James</p> <p class="dwt_publisher"></p> <p class="publishDate">1993-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">144</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3293861"> <span id="translatedtitle">Spike-Interval Triggered Averaging Reveals a <span class="hlt">Quasi-Periodic</span> Spiking Alternative for Stochastic Resonance in Catfish Electroreceptors</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p class="result-summary">Catfish detect and identify invisible prey by sensing their ultra-weak electric fields with electroreceptors. Any neuron that deals with small-amplitude input has to overcome sensitivity limitations arising from inherent threshold non-linearities in spike-generation mechanisms. Many sensory cells solve this issue with stochastic resonance, in which a moderate amount of intrinsic noise causes irregular spontaneous spiking activity with a probability that is modulated by the input signal. Here we show that catfish electroreceptors have adopted a fundamentally different strategy. Using a reverse correlation technique in which we take spike interval durations into account, we show that the electroreceptors generate a supra-threshold bias current that results in <span class="hlt">quasi-periodically</span> produced spikes. In this regime stimuli modulate the interval between successive spikes rather than the instantaneous probability for a spike. This alternative for stochastic resonance combines threshold-free sensitivity for weak stimuli with similar sensitivity for excitations and inhibitions based on single interspike intervals.</p> <div class="credits"> <p class="dwt_author">Lankheet, Martin J. M.; Klink, P. Christiaan; Borghuis, Bart G.; Noest, Andre J.</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">145</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2014SoPh..289...41B"> <span id="translatedtitle">Changes in <span class="hlt">Quasi-periodic</span> Variations of Solar Photospheric Fields: Precursor to the Deep Solar Minimum in Cycle 23?</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Possible precursor signatures in the <span class="hlt">quasi-periodic</span> variations of solar photospheric fields were investigated in the build-up to one of the deepest solar minima experienced in the past 100 years. This unusual and deep solar minimum occurred between Solar Cycles 23 and 24. We used both wavelet and Fourier analysis to study the changes in the <span class="hlt">quasi-periodic</span> variations of solar photospheric fields. Photospheric fields were derived using ground-based synoptic magnetograms spanning the period 1975.14 to 2009.86 and covering Solar Cycles 21, 22, and 23. A hemispheric asymmetry in the periodicities of the photospheric fields was seen only at latitudes above ± 45? when the data were divided into two parts based on a wavelet analysis: one prior to 1996 and the other after 1996. Furthermore, the hemispheric asymmetry was observed to be confined to the latitude range of 45? to 60?. This can be attributed to the variations in polar surges that primarily depend on both the emergence of surface magnetic flux and varying solar-surface flows. The observed asymmetry along with the fact that both solar fields above ± 45? and micro-turbulence levels in the inner-heliosphere have been decreasing since the early- to mid-nineties (Janardhan et al. in Geophys. Res. Lett. 382, 20108, 2011) suggest that around this time active changes occurred in the solar dynamo that governs the underlying basic processes in the Sun. These changes in turn probably initiated the build-up to the very deep solar minimum at the end of Cycle 23. The decline in fields above ± 45?, for well over a solar cycle, would imply that weak polar fields have been generated in the past two successive solar cycles, viz. Cycles 22 and 23. A continuation of this declining trend beyond 22 years, if it occurs, will have serious implications for our current understanding of the solar dynamo.</p> <div class="credits"> <p class="dwt_author">Bisoi, Susanta Kumar; Janardhan, P.; Chakrabarty, D.; Ananthakrishnan, S.; Divekar, Ankur</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">146</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2014PhyS...89g5202K"> <span id="translatedtitle">A new analytical approach for limit cycles and <span class="hlt">quasi-periodic</span> solutions of nonlinear oscillators: the example of the forced Van der Pol Duffing oscillator</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">In this paper we propose a technique to obtain limit cycles and <span class="hlt">quasi-periodic</span> solutions of forced nonlinear oscillators. We apply this technique to the forced Van der Pol oscillator and the forced Van der Pol Duffing oscillator and obtain for the first time their limit cycles (periodic) and <span class="hlt">quasi-periodic</span> solutions analytically. We introduce a modification of the homotopy analysis method to obtain these solutions. We minimize the square residual error to obtain accurate approximations to these solutions. The obtained analytical solutions are convergent and agree well with numerical solutions even at large times. Time trajectories of the solution, its first derivative and phase plots are presented to confirm the validity of the proposed approach. We also provide rough criteria for the determination of parameter regimes which lead to limit cycle or <span class="hlt">quasi-periodic</span> behaviour.</p> <div class="credits"> <p class="dwt_author">Kant Shukla, Anant; Ramamohan, T. R.; Srinivas, S.</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-07-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">147</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2001PhDT........22W"> <span id="translatedtitle">Rocket and radar observations of <span class="hlt">quasi-periodic</span> structures associated with mid-latitude sporadic E layers</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">This thesis concerns the experimental verification of current theories explaining the formation of <span class="hlt">quasi</span>- <span class="hlt">periodic</span> field-aligned irregularities (QP) associated with mid-latitude sporadic E layers. To address the gravity-wave modulation process common to both Woodman's and Tsunoda's theories, a detailed modelling study was performed with the full-wave model of Hickey et al. (2000). Both theories require short-wavelength, short-period gravity waves propagating in a region occupied by a ES layer, assumed to be organized by neutral winds according to wind-shear theory [Whitehead, 1961]. The results show that gravity waves with periods and wavelengths comparable to the required temporal and spatial <span class="hlt">quasi-periodicities</span> are unlikely to exist at E region altitudes. In the majority of cases examined, the waves dissipated well below the mesosphere and had propagation directions that varied considerably in the presence of even moderate winds. This contradicts both the stringent requirements of the Woodman model and also causes difficulties for the less restrictive Tsunoda model. In addition, the background polarization fields were determined from in situ electric field measurements. The conclusion must be that such fields, if they do exist, are by no means ubiquitous. This result causes difficulty for the Tsunoda theory, which is predicated on a mechanism that implies large fields should be observed regularly during QP-like conditions. To assess the Larsen model, a comprehensive analysis of E S and QP data was performed. Generation of Kelvin-Helmholtz (K-H) instabilities is likely whenever a neutral wind shear becomes unstable in the Richardson number sense. A large number of region wind studies indicate that large wind shears are common and often fulfill the requirements for instability. The very shear that is assumed to organize the ES layer, if unstable, would subsequently generate K-H structures. These K-H billows have been shown to exhibit primary horizontal wavelengths of approximately 8 times the shear layer depth. In the case of the observed shears during ES with vertical scales of 1-2 km, this gives horizontal wavelengths of approximately 8-16 km, which agrees well with the spatial separations observed for QP structures. (Abstract shortened by UMI.)</p> <div class="credits"> <p class="dwt_author">Wilson, William Robert</p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">148</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2012AnGeo..30.1655M"> <span id="translatedtitle">New type of ensemble of <span class="hlt">quasi-periodic</span>, long-lasting VLF emissions at the auroral zone</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">A new type of the series of <span class="hlt">quasi-periodic</span> (QP) very low frequency (VLF) emissions in frequency range of 1-5 kHz, and not associated with geomagnetic pulsations, has been discovered at auroral latitudes (L = 5.3) during the Finnish VLF campaign (held in December 2011). At least five unusually spectacular events, each with a duration of several hours, have been observed during the night under conditions of quiet geomagnetic activity (Kp = 0-1), although QPs usually occur during the daytime. Contrary to the QP emissions typically occurring during the day, the spectral structure of these QP events represented an extended, complicated sequence of repeated discrete rising VLF signals. Their duration was about 2-3 min each, with the repetition periods ranging from ~1 min to ~10 min. Two such nighttime non-typical events are reported in this paper. The fine structure of the separated QP elements may represent a mixture of the different frequency band signals, which seem to have independent origins. It was found that the periodic signals with lower frequency appear to trigger the strong dispersive upper frequency signals. The temporal dynamics of the spectral structure of the QPs studied were significantly controlled by some disturbances in the solar wind and interplanetary magnetic field (IMF). This finding is very important for future theoretical investigations because the generation mechanism of this new type of QP emissions is not yet understood.</p> <div class="credits"> <p class="dwt_author">Manninen, J.; Kleimenova, N. G.; Kozyreva, O. V.</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-12-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">149</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/22078460"> <span id="translatedtitle">LOW-FREQUENCY <span class="hlt">QUASI-PERIODIC</span> OSCILLATION FROM THE 11 Hz ACCRETING PULSAR IN TERZAN 5: NOT FRAME DRAGGING</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">We report on six RXTE observations taken during the 2010 outburst of the 11 Hz accreting pulsar IGR J17480-2446 located in the globular cluster Terzan 5. During these observations we find power spectra which resemble those seen in Z-type high-luminosity neutron star low-mass X-ray binaries, with a <span class="hlt">quasi-periodic</span> oscillation (QPO) in the 35-50 Hz range simultaneous with a kHz QPO and broadband noise. Using well-known frequency-frequency correlations, we identify the 35-50 Hz QPOs as the horizontal branch oscillations, which were previously suggested to be due to Lense-Thirring (LT) precession. As IGR J17480-2446 spins more than an order of magnitude more slowly than any of the other neutron stars where these QPOs were found, this QPO cannot be explained by frame dragging. By extension, this casts doubt on the LT precession model for other low-frequency QPOs in neutron stars and perhaps even black hole systems.</p> <div class="credits"> <p class="dwt_author">Altamirano, D.; Van der Klis, M.; Wijnands, R. [Astronomical Institute, 'Anton Pannekoek', University of Amsterdam, Science Park 904, 1098XH Amsterdam (Netherlands); Ingram, A. [Department of Physics, University of Durham, South Road, Durham DH1 3LE (United Kingdom); Linares, M.; Homan, J., E-mail: d.altamirano@uva.nl [Massachusetts Institute of Technology, Kavli Institute for Astrophysics and Space Research, Cambridge, MA 02139 (United States)</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-11-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">150</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2014ApJ...788...31H"> <span id="translatedtitle">Tracking the Evolution of <span class="hlt">Quasi-periodic</span> Oscillation in RE J1034+396 Using the Hilbert-Huang Transform</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">RE J1034+396, a narrow-line Seyfert 1 active galactic nucleus (AGN), is the first example of AGNs that exhibited a nearly coherent <span class="hlt">quasi-periodic</span> oscillation (QPO) for the data collected by XMM-Newton in 2007. The spectral behaviors and timing properties of the QPO have been studied since its discovery. We present an analysis of the QPO in RE J1034+396 based on the Hilbert-Huang transform. Comparing with other time-frequency analysis methods, the Hilbert spectrum reveals the variation of the QPO period in great detail. Furthermore, the empirical mode decomposition provides bandpass-filtered data that can be used in the O - C and correlation analysis. We suggest that it is better to divide the evolution of the QPO in this observation into three epochs according to their different periodicities. In addition to the periodicities, the correlations between the QPO periods and corresponding mean count rates are also different in these three epochs. Further examining the phase lags in these epochs, we found no significant phase lags between the soft and hard X-ray bands, which is also confirmed in the QPO phase-resolved spectral analysis. Finally, we discuss the indications of current models including a spotted accretion disk, diskoseismology, and oscillation of shock according to the observed time-frequency and spectral behaviors.</p> <div class="credits"> <p class="dwt_author">Hu, Chin-Ping; Chou, Yi; Yang, Ting-Chang; Su, Yi-Hao</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-06-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">151</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/1998GeoRL..25.1533A"> <span id="translatedtitle"><span class="hlt">Quasi-periodic</span> behavior of ion events and wave activity upstream from Jupiter's Bow Shock: Ulysses' observations</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">A new insight into the ways that the Jovian magnetosphere influences the near Jupiter interplanetary space becomes possible thanks to Ulysses' collection of magnetic field, plasma and energetic ion (HI-SCALE) data during its inbound trajectory (d22-d34, 1992). The most striking new results from the analysis of those data are the following: a) presence of large amplitude (?B?/B?1) near plane polarized Alfvén waves upstream from the Jovian bow shock with a period equal to the planet’s rotation (˜10h) at times when the Interplanetary Magnetic Field (IMF) was in contact with the bow shock/magnetopause and lay well outside the ecliptic; b) observation of ˜10h <span class="hlt">quasi-periodic</span> variation in the ion plasma and energetic ion data up to energies of ˜2 MeV, c) existence of a variation with a period 2.5 h ?T ?6.5 h in the magnetic field and the ion data, in several cases, d) detection of magnetic waves and charged particle modulation with a period of ˜40min, e) observation of an ˜10 h inward/outward motion of the Jovian magnetopause. The observations are consistent with generation of the low frequency upstream (Alfvén) waves through periodic injection of plasma/energetic ions from within the magnetosphere into the upstream region.</p> <div class="credits"> <p class="dwt_author">Anagnostopoulos, G. C.; Balogh, A.; Marhavilas, P. K.; Rigas, A. G.; Sarris, E. T.; Trochoutsos, P. C.</p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">152</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=19930071533&hterms=vortices+plasma&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3Dvortices%2Bplasma"> <span id="translatedtitle"><span class="hlt">Quasi-periodic</span> transverse plasma flow associated with an evolving MHD vortex street in the outer heliosphere</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">We study a transverse plasma flow induced by the evolution of a Karman vortex street using a Chebyshev-Fourier spectral algorithm to solve both the compressible Navier-Stokes and MHD equations. The evolving vortex street is formed by the nonlinear interaction of two vortex sheets initially in equilibrium. We study spatial profiles of the total plasma velocity, the density, the meridional flow angle and the location of sector boundaries and find generally good agreement with Voyager 2 measurements of <span class="hlt">quasi-periodic</span> transverse flow in the outer heliosphere. The pressure pulses associated with the meridional flows in the simulation are too small, although they are correctly located, and this may be due to the lack of any 'warp' in the current sheet in this model. A strong, flow-aligned magnetic field, such as would occur in the inner heliosphere, is shown to lead to weak effects that would be masked by the background interplanetary turbulence. We also study the plasma and magnetic transport resulting from the meridional flow and find that deficits of magnetic quantities do occur near the ecliptic. While the effect is relatively small, it is in general agreement with the most recent analysis of 'flux deficit' in the outer heliosphere.</p> <div class="credits"> <p class="dwt_author">Siregar, Edouard; Roberts, D. A.; Goldstein, Melvyn L.</p> <p class="dwt_publisher"></p> <p class="publishDate">1993-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">153</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=20060009467&hterms=gsm&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3D%2522gsm%2522"> <span id="translatedtitle">Cluster observations of <span class="hlt">quasi-periodic</span> impulsive signatures in the dayside northern lobe: High-latitude flux transfer events?</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">We report on a series of <span class="hlt">quasi-periodic</span> reversals in GSM B(sub Z) observed by the four Cluster spacecraft in the northern dayside lobe poleward of the cusp on 23 February 2001. During an interval of about 35 min, multiple reversals (negative to positive) in B(sub Z) of approximately 1-min duration with an approximate 8-min recurrence time were observed. The individual structures do not resemble low-latitude flux transfer events (FTE) [Russell and Elphic, 1979] but the 8-min recurrence frequency suggests that intermittent reconnection may be occurring .Measurements (appropriately lagged) of the solar wind at ACE show that the IMF was southward-oriented with a strong B(sub X) and that a modest dynamic pressure increased as the events started. The multi-point observations afforded by the Cluster spacecraft were used to infer the motion (direction and speed) of the observed magnetic field reversals. The associated currents were also calculated and they are consistent with the spatial confinement of the observed magnetic field reversals. We propose that the observed reversals are due to flux tubes reconnecting with closed field lines on the dayside. Ancillary data from the Cluster Ion Spectrometry (CIS) and Plasma Electron And Current Experiment (PEACE) instruments were used to develop a physical picture of the reversals.</p> <div class="credits"> <p class="dwt_author">Thompson, S. M.; Kivelson, M. G.; Khurana, K. K.; Balogh, A.; Reme, H.; Fazakerley, A. N.; Kistler, L. M.</p> <p class="dwt_publisher"></p> <p class="publishDate">2004-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">154</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2014ApJ...787..128H"> <span id="translatedtitle"><span class="hlt">Quasi-periodic</span> Oscillations in Short Recurring Bursts of the Soft Gamma Repeater J1550-5418</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">The discovery of <span class="hlt">quasi-periodic</span> oscillations (QPOs) in magnetar giant flares has opened up prospects for neutron star asteroseismology. The scarcity of giant flares makes a search for QPOs in the shorter, far more numerous bursts from soft gamma repeaters (SGRs) desirable. In Huppenkothen et al., we developed a Bayesian method for searching for QPOs in short magnetar bursts, taking into account the effects of the complicated burst structure, and have shown its feasibility on a small sample of bursts. Here we apply the same method to a much larger sample from a burst storm of 286 bursts from SGR J1550-5418. We report a candidate signal at 260 Hz in a search of the individual bursts, which is fairly broad. We also find two QPOs at ~93 Hz, and one at 127 Hz, when averaging periodograms from a number of bursts in individual triggers, at frequencies close to QPOs previously observed in magnetar giant flares. Finally, for the first time, we explore the overall burst variability in the sample and report a weak anti-correlation between the power-law index of the broadband model characterizing aperiodic burst variability and the burst duration: shorter bursts have steeper power-law indices than longer bursts. This indicates that longer bursts vary over a broader range of timescales and are not simply longer versions of the short bursts.</p> <div class="credits"> <p class="dwt_author">Huppenkothen, D.; D'Angelo, C.; Watts, A. L.; Heil, L.; van der Klis, M.; van der Horst, A. J.; Kouveliotou, C.; Baring, M. G.; Gö?ü?, E.; Granot, J.; Kaneko, Y.; Lin, L.; von Kienlin, A.; Younes, G.</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-06-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">155</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2009MNRAS.394..250M"> <span id="translatedtitle">RE J1034+396: the origin of the soft X-ray excess and <span class="hlt">quasi-periodic</span> oscillation</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">The X-ray <span class="hlt">quasi-periodic</span> oscillation (QPO) seen in RE J1034+396 is so far unique amongst active galactic nuclei (AGN). Here, we look at another unique feature of RE J1034+396, namely its huge soft X-ray excess, to see if this is related in any way to the detection of the QPO. We show that all potential models considered for the soft energy excess can fit the 0.3-10 keV X-ray spectrum, but the energy dependence of the rapid variability (which is dominated by the QPO) strongly supports a spectral decomposition where the soft excess is from low-temperature Comptonization of the disc emission and remains mostly constant, while the rapid variability is produced by the power-law tail changing in normalization. The presence of the QPO in the tail rather than in the disc is a common feature in black hole binaries (BHBs), but low-temperature Comptonization of the disc spectrum is not generally seen in these systems. The main exception to this is GRS 1915+105, the only BHB which routinely shows super-Eddington luminosities. We speculate that the super-Eddington accretion rates lead to a change in disc structure, and that this also triggers the X-ray QPO.</p> <div class="credits"> <p class="dwt_author">Middleton, Matthew; Done, Chris; Ward, Martin; Gierli?ski, Marek; Schurch, Nick</p> <p class="dwt_publisher"></p> <p class="publishDate">2009-03-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">156</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2014MNRAS.437.1329G"> <span id="translatedtitle"><span class="hlt">Quasi-periodic</span> oscillations in a radiative transonic flow: results of a coupled Monte Carlo-TVD simulation</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Low- and intermediate-frequency <span class="hlt">quasi-periodic</span> oscillations (QPOs) in black hole candidates are believed to be due to oscillations of the Comptonizing regions in an accretion flow. Assuming that the general structure of an accretion disc is a two-component advective flow (TCAF), we numerically simulate the light curves emitted from an accretion disc for different accretion rates and find how the QPO frequencies vary. We use a standard Keplerian disc residing at the equatorial plane as a source of soft photons. These soft photons, after suffering multiple scattering with the hot electrons of the low angular momentum, sub-Keplerian, flow emerge out as hard radiation. The hydrodynamic and thermal properties of the electron cloud is simulated using a total variation diminishing (TVD) code. The TVD code is then coupled with a radiative transfer code which simulates the energy exchange between the electron and radiation using Monte Carlo technique. The resulting localized heating and cooling are included also. We find that the QPO frequency increases and the spectrum becomes softer as we increase the Keplerian disc rate. However, the spectrum becomes harder if we increase the sub-Keplerian accretion rate. We find that an earlier prediction that QPOs occur when the infall time-scale roughly matches with the cooling time-scale, originally obtained using a power-law cooling, remains valid even for Compton cooling. Our findings agree with the general observations of low-frequency QPOs in black hole candidates.</p> <div class="credits"> <p class="dwt_author">Garain, Sudip K.; Ghosh, Himadri; Chakrabarti, Sandip K.</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">157</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=20010073051&hterms=lewin&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D10%26Ntt%3Dlewin"> <span id="translatedtitle">High-Frequency <span class="hlt">Quasi-Periodic</span> Oscillations in the 2000 Outburst of the Galactic Microquasar XTE J1550-564</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">We present an analysis of the high-frequency timing properties of the April-May 2000 outburst of the black hole candidate and Galactic microquasar XTE J1550-564, measured with the Rossi X-ray Timing Explorer, The rapid X-ray variability we measure is consistent with the source being in either the "very high" or "intermediate" canonical black hole state. A strong (5-8% RMS) <span class="hlt">quasi-periodic</span> oscillation (QPO) is found between 249-278 Hz; this may represent the first recurrence of the same high-frequency QPO in subsequent outbursts of a transient black hole candidate. We also present possible evidence for a lower-frequency QPO at approximately 187 Hz, also reported previously and likely present simultaneously with the higher-frequency QPO. We discuss these findings within the context of the 1998 outburst of XTE J1550-564, and comment on implications for models of QPOs, accretion flows, and black hole spin.</p> <div class="credits"> <p class="dwt_author">Miller, J. M.; Wijnands, R.; Homan, J.; Belloni, T.; Pooley, D.; Kouveliotou, C.; vanderKlis, M.; Lewin, W. H. G.; Whitaker, Ann F. (Technical Monitor)</p> <p class="dwt_publisher"></p> <p class="publishDate">2001-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">158</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/doepatents/biblio/1014014"> <span id="translatedtitle">Fuel injector utilizing <span class="hlt">non-thermal</span> plasma activation</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/doepatents">DOEpatents</a></p> <p class="result-summary">A <span class="hlt">non-thermal</span> plasma assisted combustion fuel injector that uses an inner and outer electrode to create an electric field from a high voltage power supply. A dielectric material is operatively disposed between the two electrodes to prevent arcing and to promote the formation of a <span class="hlt">non-thermal</span> plasma. A fuel injector, which converts a liquid fuel into a dispersed mist, vapor, or aerosolized fuel, injects into the <span class="hlt">non-thermal</span> plasma generating energetic electrons and other highly reactive chemical species.</p> <div class="credits"> <p class="dwt_author">Coates, Don M. (Santa Fe, NM); Rosocha, Louis A. (Los Alamos, NM)</p> <p class="dwt_publisher"></p> <p class="publishDate">2009-12-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">159</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2013SPD....44...50L"> <span id="translatedtitle"><span class="hlt">Quasi-periodic</span> Fast-mode Magnetosonic Wave Trains Inside and Outside CME Bubbles Detected by SDO/AIA</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary"><span class="hlt">Quasi-periodic</span> fast-mode magnetosonic wave trains both inside and outside expanding CME bubbles have recently been discovered by SDO/AIA (Liu et al. 2011, 2012; Shen & Liu 2012). In general, a wave train inside a CME bubble originates from a flare site and propagates along a funnel of coronal loops at typically 1000-2000 km/s (Ofman et al. 2011). A wave train outside a CME usually originates from a CME flank and propagates in the low corona along the solar surface following the leading front of a global EUV wave at typically 500-1000 km/s. The former is primarily seen in the cooler 171 Angstrom channel with a characteristic temperature of 0.8 MK, while the latter is pronounced in the hotter 193 and 211 Angstrom channels of typically 1.6-2.0 MK. What is the relationship between the two types of wave trains? Why do they appear differently in location and wavelength (temperature)? To answer these questions, we report here for the first time the evidence that the wave train beyond the CME bubble is the continuation of the same wave train along the funnel within the CME. The continuous deceleration of the waves is consistent with the expected decrease of the local fast-mode speed with distance from the active region (e.g., Ofman et al. 2011; Downs et al. 2012). There is an abrupt change of the wave speed at the topological interface where the expanding CME flank is located, indicative of contrasting magnetic and plasma conditions, which can give rise to different (fast-mode) speeds and wavelength (temperature) dependent appearances of these wave trains.Abstract (2,250 Maximum Characters): <span class="hlt">Quasi-periodic</span> fast-mode magnetosonic wave trains both inside and outside expanding CME bubbles have recently been discovered by SDO/AIA (Liu et al. 2011, 2012; Shen & Liu 2012). In general, a wave train inside a CME bubble originates from a flare site and propagates along a funnel of coronal loops at typically 1000-2000 km/s (Ofman et al. 2011). A wave train outside a CME usually originates from a CME flank and propagates in the low corona along the solar surface following the leading front of a global EUV wave at typically 500-1000 km/s. The former is primarily seen in the cooler 171 Angstrom channel with a characteristic temperature of 0.8 MK, while the latter is pronounced in the hotter 193 and 211 Angstrom channels of typically 1.6-2.0 MK. What is the relationship between the two types of wave trains? Why do they appear differently in location and wavelength (temperature)? To answer these questions, we report here for the first time the evidence that the wave train beyond the CME bubble is the continuation of the same wave train along the funnel within the CME. The continuous deceleration of the waves is consistent with the expected decrease of the local fast-mode speed with distance from the active region (e.g., Ofman et al. 2011; Downs et al. 2012). There is an abrupt change of the wave speed at the topological interface where the expanding CME flank is located, indicative of contrasting magnetic and plasma conditions, which can give rise to different (fast-mode) speeds and wavelength (temperature) dependent appearances of these wave trains.</p> <div class="credits"> <p class="dwt_author">Liu, Wei; Ofman, L.; Downs, C.; Title, A. M.</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-07-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">160</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2012ApJ...756...55M"> <span id="translatedtitle">Fractional Amplitude of Kilohertz <span class="hlt">Quasi-periodic</span> Oscillation from 4U 1728-34: Evidence of Decline at Higher Energies</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">A kilohertz <span class="hlt">quasi-periodic</span> oscillation (kHz QPO) is an observationally robust high-frequency timing feature detected from neutron star low-mass X-ray binaries (LMXBs). This feature can be very useful to probe the superdense core matter of neutron stars and the strong gravity regime. Although many models exist in the literature, the physical origin of kHz QPO is not known, and hence this feature cannot be used as a tool yet. The energy dependence of kHz QPO fractional rms amplitude is an important piece of the jigsaw puzzle to understand the physical origin of this timing feature. It is known that the fractional rms amplitude increases with energy at lower energies. At higher energies, the amplitude is usually believed to saturate, although this is not established. We combine tens of lower kHz QPOs from a neutron star LMXB 4U 1728-34 in order to improve the signal-to-noise ratio. Consequently, we, for the first time to the best of our knowledge, find a significant and systematic decrease of the fractional rms amplitude with energy at higher photon energies. Assuming an energy spectrum model, blackbody+powerlaw, we explore if the sinusoidal variation of a single spectral parameter can reproduce the above-mentioned fractional rms amplitude behavior. Our analysis suggests that the oscillation of any single blackbody parameter is favored over the oscillation of any single power-law parameter, in order to explain the measured amplitude behavior. We also find that the quality factor of a lower kHz QPO does not plausibly depend on photon energy.</p> <div class="credits"> <p class="dwt_author">Mukherjee, Arunava; Bhattacharyya, Sudip</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-09-01</p> </div> </div> </div> </div> <div id="filter_results_form" class="filter_results_form floatContainer" style="visibility: visible;"> <div style="width:100%" id="PaginatedNavigation" class="paginatedNavigationElement"> <a id="FirstPageLink" onclick='return showDiv("page_1");' href="#" title="First Page"> <img id="FirstPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.first.18x20.png" alt="First Page" /></a> <a id="PreviousPageLink" onclick='return showDiv("page_7");' href="#" title="Previous Page"> <img id="PreviousPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.previous.18x20.png" alt="Previous Page" /></a> <span id="PageLinks" class="pageLinks"> <span> <a onClick='return 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id="PaginatedNavigation" class="paginatedNavigationElement"> <a id="FirstPageLink" onclick='return showDiv("page_1");' href="#" title="First Page"> <img id="FirstPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.first.18x20.png" alt="First Page" /></a> <a id="PreviousPageLink" onclick='return showDiv("page_8");' href="#" title="Previous Page"> <img id="PreviousPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.previous.18x20.png" alt="Previous Page" /></a> <span id="PageLinks" class="pageLinks"> <span> <a onClick='return showDiv("page_1");' href="#">1</a> <a onClick='return showDiv("page_2");' href="#">2</a> <a onClick='return showDiv("page_3");' href="#">3</a> <a onClick='return showDiv("page_4");' href="#">4</a> <a onClick='return showDiv("page_5");' href="#">5</a> <a onClick='return showDiv("page_6");' href="#">6</a> <a onClick='return showDiv("page_7");' href="#">7</a> <a onClick='return showDiv("page_8");' href="#">8</a> <a 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showDiv("page_10");' href="#" title="Next Page"> <img id="NextPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.next.18x20.png" alt="Next Page" /></a> <a id="LastPageLink" onclick='return showDiv("page_25.0");' href="#" title="Last Page"> <img id="LastPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.last.18x20.png" alt="Last Page" /></a> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">161</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2014MNRAS.440.3275S"> <span id="translatedtitle">Broad iron emission line and kilohertz <span class="hlt">quasi-periodic</span> oscillations in the neutron star system 4U 1636-53</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Both the broad iron (Fe) line and the frequency of the kilohertz <span class="hlt">quasi-periodic</span> oscillations (kHz QPOs) in neutron star low-mass X-ray binaries (LMXBs) can potentially provide independent measures of the inner radius of the accretion disc. We use XMM-Newton and simultaneous Rossi X-ray Timing Explorer observations of the LMXB 4U 1636-53 to test this hypothesis. We study the properties of the Fe K? emission line as a function of the spectral state of the source and the frequency of the kHz QPOs. We find that the inner radius of the accretion disc deduced from the frequency of the upper kHz QPO varies as a function of the position of the source in the colour-colour diagram, in accordance with previous work and with the standard scenario of accretion disc geometry. On the contrary, the inner disc radius deduced from the profile of the iron line is not correlated with the spectral state of the source. The values of the inner radius inferred from kHz QPOs and iron lines, in four observations, do not lead to a consistent value of the neutron star mass, regardless of the model used to fit the iron line. Our results suggest that either the kHz QPO or the standard relativistic Fe line interpretation does not apply for this system. Furthermore, the simultaneous detection of kHz QPOs and broad iron lines is difficult to reconcile with models in which the broadening of the iron line is due to the reprocessing of photons in an outflowing wind.</p> <div class="credits"> <p class="dwt_author">Sanna, Andrea; Méndez, Mariano; Altamirano, Diego; Belloni, Tomaso; Hiemstra, Beike; Linares, Manuel</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-06-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">162</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2014EGUGA..16.4868S"> <span id="translatedtitle">Acoustic-gravity waves in the nonisothermal atmosphere and its influence on the magnetospheric <span class="hlt">quasi-periodic</span> vlf emissions</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">We examine two mutually complementing tasks related to the theoretical analysis of acoustic-gravity disturbances in the Earth's atmosphere and its influence on magnetosphere processes. Our research is based on modern atmospherical models. We study waves propagation, absorption, and filtration. The atmospheric nonisothermicity is taken into account, for example, by introduction of a two-layered atmosphere temperature model. For a study of more delicate effects, a piecewise-linear model, for which the analytical solution is written by the hypergeometric functions, is employed. Also we consider an influence of acoustic-gravity waves on VLF electromagnetic wave excitation in the magnetosphere. This influence occurs as a result of the following processes: a modulation of the plasma density by acoustic-gravity waves in the ionosphere, a modulation of reflection from the ionosphere for VLF waves, and a modification of the magnetospheric resonator Q-factor for VLF waves. Variation of the magnetospheric resonator Q-factor has an influence on the operation of the plasma magnetospheric maser, where the active substances are radiation belts particles and the working modes are electromagnetic VLF waves (whistler-type waves). The plasma magnetospheric maser can be responsible for an excitation of self-oscillations. These self-oscillations are frequently characterized by alternating stages of accumulation and precipitation of energetic particles into the ionosphere during a pulse of whistler emissions. Numerical and analytical investigations of the response of self-oscillations to harmonic oscillations of the whistler reflection coefficient shows that even a small modulation rate can significantly changes the magnetospheric VLF emissions. Our results can explain the causes of the modulation of energetic electron fluxes and whistler wave intensity with a time scale from 10 to 150 seconds in the day-side magnetosphere. Such <span class="hlt">quasi-periodic</span> VLF emissions are often observed in the sub-auroral and auroral magnetosphere and have a noticeable effect on the formation of the space weather phenomena.</p> <div class="credits"> <p class="dwt_author">Savina, Olga; Bespalov, Peter; Misonova, Vera; Petrov, Kiril</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-05-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">163</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=20000012411&hterms=lewin&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D20%26Ntt%3Dlewin"> <span id="translatedtitle"><span class="hlt">Quasi-Periodic</span> Oscillations in Black Hole Candidates as an Indicator of Transition Between Low and High States</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">By comparing positions on a spectral color-color diagram from 10 black hole candidates (BHCS) observed with Ginga (1354-64, 1826-24, 1630-47, LMC X-1, LMC X-3, GS 2000+25, GS 2023+33, GS 1124-68, Cyg X-1, and GX 339-4) with the observed broadband noise (BBN) (0.001-64 Hz) and <span class="hlt">quasi-periodic</span> oscillation (QPO) variability, we find that the "very high state" is spectrally intermediate to the soft/high state and hard/low state. We find a transition point in spectral hardness where the dependence of the BHC QPO centroid frequency (of GS 1124-68 and GX 339-4) on spectral hardness switches from a correlation to an anticorrelation; where the BBN variability switches from high state to low state; and where the spectral hardness of the QPO relative to that of the BBN variability is a maximum. This coincidence of changing behavior in both the QPO and the broadband variability leads us to hypothesize that the QPO is due to interaction between the physical components which dominate the behaviors of BHCs when they occupy the hard/low and soft/high states. We conclude that these QPOs should be observed from BHCs during transition between these two states. Comparison with QPO and BBN behavior observed during the 1996 transition of Cyg X-1 supports this hypothesis. We also report 1-3 Hz QPOs observed in GS 2000+25 and Cyg X-1 in the hard/low state, and we compare these to the QPOs observed in GS 1124-68 and GX 339-4.</p> <div class="credits"> <p class="dwt_author">Rutledge, Robert E.; Lewin, Walter H. G.; VanDerKlis, Michiel; vanParadijs, Jan; Dotani, Tadayasu; Vaughan, Brian; Belloni, Tomaso; Oosterbroek, Tim; Kouvewliotou, Chryssa</p> <p class="dwt_publisher"></p> <p class="publishDate">1999-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">164</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=19990064602&hterms=lewin&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D30%26Ntt%3Dlewin"> <span id="translatedtitle"><span class="hlt">Quasi-Periodic</span> Oscillations in Black Hole Candidates as an Indicator of Transition Between Low and High States</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">By comparing positions on a spectral color-color diagram from 10 black hole candidates (BHCS) observed with Ginga (1354-64, 1826-24, 1630-47, LMC X-1, LMC X-3, GS 2000+25, GS 2023+33, GS 1124-68, Cyg X-1, and GX 339-4) with the observed broad-band noise (0.001- 64 Hz; BBN) and <span class="hlt">quasi-periodic</span> oscillation (QPO) variability, we find that the so-called "Very High State" is spectrally intermediate to the Soft/High-State and Hard/Low-State. We find a transition point in spectral hardness where the dependence of the BHC QPO centroid frequency (of GS 1124-68 and GX 339-4) on spectral hardness switches from a correlation to an anti-correlation; where the BBN variability switches from High-State to Low-State; and where the spectral hardness of the QPO relative to that of the BBN variability is a maximum. This coincidence of changing behavior in both the QPO and the broad-band variability leads us to hypothesize that the QPO is due to interaction between the physical components which dominate the behaviors of BHCs when they occupy the Hard/Low and Soft/High States. We conclude that these QPO should be observed from BHCs during transition between these two states. Comparison with QPO and BBN behavior observed during the 1996 transition of Cyg X-1 supports this hypothesis. We also report 1-3 Hz QPO observed in GS 2000+25 and Cyg X-1 in the Hard/Low State, and we compare these to the QPO observed in GS 1124-68 and GX 339-4.</p> <div class="credits"> <p class="dwt_author">Rutledge, Robert E; Lewin, Walter H. G.; vanderKlis, Michiel; vanParadijs, Jan; Dotani, Tadayasu; Vaughan, Brian; Belloni, Tomaso; Oosterbroek, Tim; Kouveliotou, Chryssa</p> <p class="dwt_publisher"></p> <p class="publishDate">1998-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">165</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/22092460"> <span id="translatedtitle">FRACTIONAL AMPLITUDE OF KILOHERTZ <span class="hlt">QUASI-PERIODIC</span> OSCILLATION FROM 4U 1728-34: EVIDENCE OF DECLINE AT HIGHER ENERGIES</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">A kilohertz <span class="hlt">quasi-periodic</span> oscillation (kHz QPO) is an observationally robust high-frequency timing feature detected from neutron star low-mass X-ray binaries (LMXBs). This feature can be very useful to probe the superdense core matter of neutron stars and the strong gravity regime. Although many models exist in the literature, the physical origin of kHz QPO is not known, and hence this feature cannot be used as a tool yet. The energy dependence of kHz QPO fractional rms amplitude is an important piece of the jigsaw puzzle to understand the physical origin of this timing feature. It is known that the fractional rms amplitude increases with energy at lower energies. At higher energies, the amplitude is usually believed to saturate, although this is not established. We combine tens of lower kHz QPOs from a neutron star LMXB 4U 1728-34 in order to improve the signal-to-noise ratio. Consequently, we, for the first time to the best of our knowledge, find a significant and systematic decrease of the fractional rms amplitude with energy at higher photon energies. Assuming an energy spectrum model, blackbody+powerlaw, we explore if the sinusoidal variation of a single spectral parameter can reproduce the above-mentioned fractional rms amplitude behavior. Our analysis suggests that the oscillation of any single blackbody parameter is favored over the oscillation of any single power-law parameter, in order to explain the measured amplitude behavior. We also find that the quality factor of a lower kHz QPO does not plausibly depend on photon energy.</p> <div class="credits"> <p class="dwt_author">Mukherjee, Arunava; Bhattacharyya, Sudip, E-mail: arunava@tifr.res.in, E-mail: sudip@tifr.res.in [Tata Institute of Fundamental Research, Mumbai-400005 (India)</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-09-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">166</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2013AN....334..101P"> <span id="translatedtitle"><span class="hlt">Non-thermal</span> processes in coronae and beyond</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">This contribution summarizes the splinter session ``<span class="hlt">Non-thermal</span> processes in coronae and beyond'' held at the Cool Stars 17 workshop in Barcelona in 2012. It covers new developments in high energy <span class="hlt">non-thermal</span> effects in the Earth's exosphere, solar and stellar flares, the diffuse emission in star forming regions and reviews the state and the challenges of the underlying atomic databases.</p> <div class="credits"> <p class="dwt_author">Poppenhaeger, K.; Günther, H. M.; Beiersdorfer, P.; Brickhouse, N. S.; Carter, J. A.; Hudson, H. S.; Kowalski, A.; Lalitha, S.; Miceli, M.; Wolk, S. J.</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-02-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">167</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/26923948"> <span id="translatedtitle"><span class="hlt">Non-Thermal</span> Plasma Applications at Very Low Temperature</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">Application of <span class="hlt">non-thermal</span> plasma for gas cleaning is gaining prominence in the recent years. Normally, the gas treatment was carried out at or above room temperature, by the dry type plasma reactor. However, this treatment is still inadequate in the removal of certain stable gases present in the flue gas mixture. We propose the <span class="hlt">non-thermal</span> plasma process at very low</p> <div class="credits"> <p class="dwt_author">A. MIZUNO; B. S. RAJANIKANTH; K. SHIMIZU; K. KINOSHITA; K. YANAGIHARA; M. OKUMOTO; S. KATSURA</p> <p class="dwt_publisher"></p> <p class="publishDate">1998-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">168</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2007AGUFM.P43A1010G"> <span id="translatedtitle">A <span class="hlt">non</span> <span class="hlt">Thermal</span> Model for the Titan Extended Exosphere</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">The recent results of the INMS instrument, onboard Cassini, have shown evidence for a hot Titan corona, with <span class="hlt">non</span> <span class="hlt">thermal</span> profiles for N2 and CH4 in the lower exosphere (below 2000 km altitude). We propose here to use these observations for modelling the extended <span class="hlt">non</span> <span class="hlt">thermal</span> exosphere of Titan, through the use of <span class="hlt">non</span> <span class="hlt">thermal</span> distributions at the exobase. <span class="hlt">Non</span> <span class="hlt">thermal</span> extended exospheric profiles are first deduced for the Titan flybys Ta (26th october 2004), Tb (13th december 2004) and T5 (16th april 2005). Then, we propose a <span class="hlt">non</span> <span class="hlt">thermal</span> exosphere model averaged over the two first two flybys, whose conditions were very similar, for the five main species at the exobase : H, H2, N, N2 and CH4. This model is then used to simulate the production of energetic neutral atoms (ENAs) in the Titan exosphere, and the results are compared to the observations of the MIMI INCA ENA imager onboard Cassini.</p> <div class="credits"> <p class="dwt_author">Garnier, P.; Dandouras, I.; Toublanc, D.; Mitchell, D. G.; Roelof, E. C.; Brandt, P. C.; Krimigis, S. M.; Krupp, N.; Hamilton, D. C.; Waite, H.</p> <p class="dwt_publisher"></p> <p class="publishDate">2007-12-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">169</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2000arxt.confE..60T"> <span id="translatedtitle">Timing Spectroscopy of <span class="hlt">Quasi-Periodic</span> Oscillations in the Low-Mass X-ray Neutron Star Binaries</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Precise simultaneous measurements of the frequencies of the two kiloHertz <span class="hlt">quasi-periodic</span> oscillations (referred in the literature as upper and lower kHz QPOs) cast doubts on the validity of the simple beat-frequency interpretation and some of the modifications introduced to explain the results of the varying frequency difference. A new model explains the variation of the frequency difference suggesting that the upper kHz QPO, namely, ?h is an upper hybrid frequency of the Keplerian oscillator under the influence of the Coriolis force and the lower kHz QPO is the Keplerian frequency ?K. Such an oscillator has two branches characterized by high frequency ?h (around 1 kHz) and by low frequency ?L (around 50 Hz). The frequency ?L depends strongly on the angle, ? between the normal to the neutron star disk and ? - the angular velocity of the magnetosphere surrounding the neutron star. In the lower part of the QPO spectrum (around 10 Hz), this model identifies the frequency of radial viscous oscillations ?v (previously called ``extra noise component") and the break frequency ?b which is associated with the diffusive process in the transition region (the innermost part of the disk). According to this model, all frequencies (namely ?h, ?L, ?b and ?v) have specific dependences on ?K. This talk focuses on the verification of the predicted relations. For three sources, namely Sco X-1, 4U 1728-34 and 4U 0614+09 we present a comprehensive classification of QPO within the framework of this model. We also demonstrate that for four sources the data confirm the constancy of ? angle (an analytic combination of the observable frequencies) for a given source in the wide range of kHz QPO frequencies. For the source 4U 0614+09 it is 15.5o +/- 1o, for 4U 1728-34 it is 8.3 +/- 1.0o, which is slightly larger than ?=5.5 +/- 0.5o previously found for Sco X-1 and ?=3.9 +/- 0.2o for 4U 1702-42.</p> <div class="credits"> <p class="dwt_author">Titarchuk, L.; Osherovich, V.</p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">170</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.agu.org/journals/ja/v101/iA01/95JA02223/95JA02223.pdf"> <span id="translatedtitle">Frequency variations of <span class="hlt">quasi-periodic</span> ELF-VLF emissions: A possible new ground-based diagnostic of the outer high-latitude magnetosphere</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">Magnetic pulsations and <span class="hlt">quasi-periodic</span> (QP) amplitude modulations of ELF-VLF waves at Pc 3-4 frequencies (15-50 mHz) are commonly observed simultaneously in cusp-latitude data. The naturally occurring ELF-VLF emissions are believed to be modulated within the magnetosphere by the compressional component of geomagnetic pulsations formed external to the magnetosphere. We have examined data from South Pole Station (L~14) to determine the</p> <div class="credits"> <p class="dwt_author">Jennifer Alford; Mark Engebretson; Roger Arnoldy; Umran Inan</p> <p class="dwt_publisher"></p> <p class="publishDate">1996-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">171</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/19255627"> <span id="translatedtitle">Real-Time Lock-In Amplifier Implementation Using a Kalman Filter for <span class="hlt">Quasi-Periodic</span> Signal Processing in Fusion Plasma Diagnostics</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">The prospects for the real-time amplitude estimation of selected harmonic components of <span class="hlt">quasi-periodic</span> signals from a motional Stark effect (MSE) tokamak plasma diagnostic is addressed using Kalman filtering techniques. The proposed method is shown to be more competitive than a standard low-pass filter lock-in amplifier scheme. In particular, when block data processing is limited to a small number of samples</p> <div class="credits"> <p class="dwt_author">R. Coelho; D. Alves</p> <p class="dwt_publisher"></p> <p class="publishDate">2009-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">172</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/43131850"> <span id="translatedtitle">Independence of short time scale fluctuations of <span class="hlt">quasi-periodic</span> oscillations and low-frequency noise in GX 5-1</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">The short time-scale variability in the X-ray flux of the <span class="hlt">quasi-periodic</span> oscillations (QPOs) and low-frequency noise (LFM) in GX 5-1 is examined, using data from Ginga observations and simulations of the GX 5-1 power spectrum, with the purpose of determining whether there is an association between the LFN and the QPO in GX 5-1 on the horizontal branch (i.e., whether</p> <div class="credits"> <p class="dwt_author">J. P. Norris; P. Hertz; K. S. Wood; B. A. Vaughan; P. F. Michelson; K. Mitsuda; T. Dotani</p> <p class="dwt_publisher"></p> <p class="publishDate">1990-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">173</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2014ApJ...788...32W"> <span id="translatedtitle"><span class="hlt">Quasi-periodic</span> Variations in X-Ray Emission and Long-term Radio Observations: Evidence for a Two-component Jet in Sw J1644+57</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">The continued observations of Sw J1644+57 in X-ray and radio bands accumulated a rich data set to study the relativistic jet launched in this tidal disruption event. The X-ray light curve of Sw J1644+57 from 5-30 days presents two kinds of <span class="hlt">quasi-periodic</span> variations: a 200 s <span class="hlt">quasi-periodic</span> oscillation (QPO) and a 2.7 day <span class="hlt">quasi-periodic</span> variation. The latter has been interpreted by a precessing jet launched near the Bardeen-Petterson radius of a warped disk. Here we suggest that the ~200 s QPO could be associated with a second, narrower jet sweeping the observer line-of-sight periodically, which is launched from a spinning black hole in the misaligned direction with respect to the black hole's angular momentum. In addition, we show that this two-component jet model can interpret the radio light curve of the event, especially the re-brightening feature starting ~100 days after the trigger. From the data we infer that inner jet may have a Lorentz factor of ?j ~ 5.5 and a kinetic energy of E k, iso ~ 3.0 × 1052 erg, while the outer jet may have a Lorentz factor of ?j ~ 2.5 and a kinetic energy of E k, iso ~ 3.0 × 1053 erg.</p> <div class="credits"> <p class="dwt_author">Wang, Jiu-Zhou; Lei, Wei-Hua; Wang, Ding-Xiong; Zou, Yuan-Chuan; Zhang, Bing; Gao, He; Huang, Chang-Yin</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-06-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">174</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2014MNRAS.442..521S"> <span id="translatedtitle">Analytical model for <span class="hlt">non-thermal</span> pressure in galaxy clusters</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary"><span class="hlt">Non-thermal</span> pressure in the intracluster gas has been found ubiquitously in numerical simulations, and observed indirectly. In this paper we develop an analytical model for intracluster <span class="hlt">non-thermal</span> pressure in the virial region of relaxed clusters. We write down and solve a first-order differential equation describing the evolution of <span class="hlt">non-thermal</span> velocity dispersion. This equation is based on insights gained from observations, numerical simulations, and theory of turbulence. The <span class="hlt">non-thermal</span> energy is sourced, in a self-similar fashion, by the mass growth of clusters via mergers and accretion, and dissipates with a time-scale determined by the turnover time of the largest turbulence eddies. Our model predicts a radial profile of <span class="hlt">non-thermal</span> pressure for relaxed clusters. The <span class="hlt">non-thermal</span> fraction increases with radius, redshift, and cluster mass, in agreement with numerical simulations. The radial dependence is due to a rapid increase of the dissipation time-scale with radii, and the mass and redshift dependence comes from the mass growth history. Combing our model for the <span class="hlt">non-thermal</span> fraction with the Komatsu-Seljak model for the total pressure, we obtain thermal pressure profiles, and compute the hydrostatic mass bias. We find typically 10 per cent bias for the hydrostatic mass enclosed within r500.</p> <div class="credits"> <p class="dwt_author">Shi, Xun; Komatsu, Eiichiro</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-07-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">175</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2014CNSNS..19.4080N"> <span id="translatedtitle">Detection of <span class="hlt">quasi-periodic</span> processes in repeated measurements: New approach for the fitting and clusterization of different data</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Many experimentalists were accustomed to think that any independent measurement forms a non-correlated measurement that depends weakly from others. We are trying to reconsider this conventional point of view and prove that similar measurements form a strongly-correlated sequence of random functions with memory. In other words, successive measurements "remember" each other at least their nearest neighbors. This observation and justification on real data help to fit the wide set of data based on the Prony's function. The Prony's decomposition follows from the <span class="hlt">quasi-periodic</span> (QP) properties of the measured functions and includes the Fourier transform as a partial case. New type of decomposition helps to obtain a specific amplitude-frequency response (AFR) of the measured (random) functions analyzed and each random function contains less number of the fitting parameters in comparison with its number of initial data points. Actually, the calculated AFR can be considered as the generalized Prony's spectrum (GPS), which will be extremely useful in cases where the simple model pretending on description of the measured data is absent but vital necessity of their quantitative description is remained. These possibilities open a new way for clusterization of the initial data and new information that is contained in these data gives a chance for their detailed analysis. The electron paramagnetic resonance (EPR) measurements realized for empty resonator (pure noise data) and resonator containing a sample (CeO2 in our case) confirmed the existence of the QP processes in reality. But we think that the detection of the QP processes is a common feature of many repeated measurements and this new property of successive measurements can attract an attention of many experimentalists. To formulate some general conditions that help to identify and then detect the presence of some QP process in the repeated experimental measurements. To find a functional equation and its solution that yields the description of the identified QP process. To suggest some computing algorithm for fitting of the QP data to the analytical function that follows from the solution of the corresponding functional equation. The content of this paper is organized as follows. In the Section 2 we will try to find the answers on the problem posed in this introductory section. It contains also the mathematical description of the QP process and interpretation of the meaning of the generalized Prony's spectrum (GPS). The GPS includes the conventional Fourier decomposition as a partial case. Section 3 contains the experimental details associated with receiving of the desired data. Section 4 includes some important details explaining specific features of application of general algorithm to concrete data. In Section 5 we summarize the results and outline the perspectives of this approach for quantitative description of time-dependent random data that are registered in different complex systems and experimental devices. Here we should notice that under the complex system we imply a system when a conventional model is absent[6]. Under simplicity of the acceptable model we imply the proper hypothesis ("best fit" model) containing minimal number of the fitting parameters that describes the behavior of the system considered quantitatively. The different approaches that exist in nowadays for description of these systems are collected in the recent review [7].</p> <div class="credits"> <p class="dwt_author">Nigmatullin, R.; Rakhmatullin, R.</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-12-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">176</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2013ApPhL.103y2905Z"> <span id="translatedtitle"><span class="hlt">Quasi-periodic</span> self-assembled sub-micrometer ferroelectric bulk domain gratings in Rb-doped KTiOPO4</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">We present a simple technique for fabricating <span class="hlt">quasi-periodic</span> bulk sub-?m ferroelectric domain gratings in Rb-doped KTiOPO4 (RKTP) based on self-organized ferroelectric domain formation. One-dimensional ferroelectric domain structures, with an average periodicity of 650 ± 200 nm and extending throughout 1 mm thick crystals, are obtained by etching and subsequent electric field poling using planar electrodes. The sub-?m structures in RKTP were used to demonstrate 5th order non-collinear quasi-phase matched backward second harmonic generation.</p> <div class="credits"> <p class="dwt_author">Zukauskas, Andrius; Pasiskevicius, Valdas; Canalias, Carlota</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-12-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">177</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/18545310"> <span id="translatedtitle">Electro- and thermo-optic effects on multi-wavelength Solc filters based on chi(2) nonlinear <span class="hlt">quasi-periodic</span> photonic crystals.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">We investigate electro- and thermo-optic effects on multi-wavelength Solc filters based on chi(2) nonlinear <span class="hlt">quasi-periodic</span> photonic crystals. The multi-wavelength Solc filters are composed of two building blocks A and B, in which each containing a pair of antiparallel poled domains, arranged as a Fibonacci sequence. The transmittances at filtering wavelengths can be modulated from 0 to 100% by applying an external voltage but the filtering wave-lengths are unchanged. The filtering wavelengths can be tuned by varying temperature. As temperature decreases, the filtering wavelengths increase (approximately -0.45 nm/degrees C). PMID:18545310</p> <div class="credits"> <p class="dwt_author">Kee, Chul-Sik; Lee, Yeong Lak; Lee, Jongmin</p> <p class="dwt_publisher"></p> <p class="publishDate">2008-04-28</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">178</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3025030"> <span id="translatedtitle">Effects of <span class="hlt">Non-Thermal</span> Plasma on Mammalian Cells</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p class="result-summary">Thermal plasmas and lasers have been widely used in medicine to cut, ablate and cauterize tissues through heating; in contrast, <span class="hlt">non-thermal</span> plasma produces no heat, so its effects can be selective. In order to exploit the potential for clinical applications, including wound healing, sterilization, blood coagulation, and cancer treatment, a mechanistic understanding of the interaction of <span class="hlt">non-thermal</span> plasma with living tissues is required. Using mammalian cells in culture, it is shown here that <span class="hlt">non-thermal</span> plasma created by dielectric barrier discharge (DBD) has dose-dependent effects that range from increasing cell proliferation to inducing apoptosis. It is also shown that these effects are primarily due to formation of intracellular reactive oxygen species (ROS). We have utilized ?-H2AX to detect DNA damage induced by <span class="hlt">non-thermal</span> plasma and found that it is initiated by production of active neutral species that most likely induce formation of organic peroxides in cell medium. Phosphorylation of H2AX following <span class="hlt">non-thermal</span> plasma treatment is ATR dependent and ATM independent, suggesting that plasma treatment may lead to replication arrest or formation of single-stranded DNA breaks; however, plasma does not lead to formation of bulky adducts/thymine dimers.</p> <div class="credits"> <p class="dwt_author">Kalghatgi, Sameer; Kelly, Crystal M.; Cerchar, Ekaterina; Torabi, Behzad; Alekseev, Oleg; Fridman, Alexander; Friedman, Gary; Azizkhan-Clifford, Jane</p> <p class="dwt_publisher"></p> <p class="publishDate">2011-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">179</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2008POBeo..84..250N"> <span id="translatedtitle">Atmospheric pressure <span class="hlt">non-thermal</span> plasma: Sources and applications</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary"><span class="hlt">Non-thermal</span> plasma at atmospheric pressure is an inherently unstable object. Nature of discharge plasma instabilities and conditions for observation of uniform <span class="hlt">non-thermal</span> plasma at atmospheric pressure in different environments will be discussed. Various discharge techniques have been developed, which could support uniform <span class="hlt">non-thermal</span> plasma with parameters varied in a wide range. Time limitation by plasma instabilities can be overcome by shortening pulse length or by restriction of plasma plug residence time with a fast gas flow. Discharge instabilities leading to formation of filaments or sparks are provoked by a positive feedback between the electric field and plasma density, while the counteracting process is plasma and thermal diffusion. With gas pressure growth the size of plasma fluctuation, which could be stabilized by diffusion, diminishes. As a result, to have long lived uniform plasma one should miniaturize discharge. There exist a number of active methods to organize negative feedback between the electric field and plasma density in order to suppress or, at least, delay the instability. Among them are ballast resistors in combination with electrode sectioning, reactive ballast, electronic feedback, and dielectric barrier across the electric current. The last methods are relevant for ac discharges. In the lecture an overview will be given of different discharge techniques scalable in pressure up to one atmosphere. The interest in this topic is dictated by a potential economic benefit from numerous <span class="hlt">non-thermal</span> plasma technologies. The spectrum of <span class="hlt">non-thermal</span> plasma applications is continuously broadening. An incomplete list of known applications includes: plasma-assisted chemical vapor deposition, etching, polymerization, gas-phase synthesis, protective coating deposition, toxic and harmful gas decomposition, destruction of warfare agents, electromagnetic wave shielding, polymer surface modifications, gas laser excitation, odor control, plasma assisted combustion, and gas dynamic flow control. Many of these applications have been developed with low-pressure plasma. Atmospheric pressure <span class="hlt">non-thermal</span> plasma technologies possess such advantages as simplicity of operation and relatively low cost of equipments. A variety of available discharge techniques provides <span class="hlt">non-thermal</span> plasma at atmospheric pressure in various gases with parameters covering a wide range in power densities, reduced electric field strengths and current densities. Requirements to <span class="hlt">non-thermal</span> plasma parameters and sorts of gas for various applications vary widely, too. For any specific application the most appropriate discharge type can be found. The spectrum of discharge devices already existing is surprisingly broad. The problem of a successful choice of a discharge type for a specific application will be discussed. A particular emphasis will be placed on the problem of plasma removal of toxic and harmful species from the gas flow.</p> <div class="credits"> <p class="dwt_author">Napartovich, A. P.</p> <p class="dwt_publisher"></p> <p class="publishDate">2008-07-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">180</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/23952601"> <span id="translatedtitle"><span class="hlt">Non-thermal</span> plasmas induced electrostatic stress on corneocyte desquamation.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">The advent of <span class="hlt">non-thermal</span> plasma brought a breakthrough in exploring its clinical applications in dermatology to bolster tissue generation in the domain of plasma medicine. This study aimed to investigate the effect of <span class="hlt">non-thermal</span> plasma on the corneocyte of the skin cells, in treating superficial skin diseases via the process of corneocyte desquamation, a probable mechanism for skin cell proliferation. The postulated brick and mortar arrangement of corneocytes in the stratum corneum was modeled consisting of three corneocytes and three corneodesmosomes in a simulation domain of 40.30 × 3.00 ?m² using Maxwell 2D finite element analyzer. The corneocyte desquamation was quantified by the weakening of corneodesmosomes due to electrostatic pressure (~530 MV/m) on the corneodesmosome surface exceeding its tensile strength (~76 MPa). A mathematical model displaying a relationship between the plasma potential and the skin tensile strength is also presented in this investigation. The <span class="hlt">non-thermal</span> plasma could emerge as a clean and dry therapy to treat superficial skin diseases. Our study propels investigating the interaction of <span class="hlt">non-thermal</span> plasma with the wet tissue in the deeper layer (dermis) of the skin cells and also, the development of such instruments for a comprehensive skin treatment. PMID:23952601</p> <div class="credits"> <p class="dwt_author">Tiwari, Pawan K; Lee, Yeon Soo</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-01-01</p> </div> </div> </div> </div> <div id="filter_results_form" class="filter_results_form floatContainer" style="visibility: visible;"> <div style="width:100%" id="PaginatedNavigation" class="paginatedNavigationElement"> <a id="FirstPageLink" onclick='return showDiv("page_1");' href="#" title="First Page"> <img id="FirstPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.first.18x20.png" alt="First Page" /></a> <a id="PreviousPageLink" onclick='return showDiv("page_8");' href="#" title="Previous Page"> <img id="PreviousPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.previous.18x20.png" alt="Previous Page" /></a> <span id="PageLinks" class="pageLinks"> <span> <a onClick='return showDiv("page_1");' href="#">1</a> <a onClick='return showDiv("page_2");' href="#">2</a> <a 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onClick='return showDiv("page_11");' href="#">11</a> <a onClick='return showDiv("page_12");' href="#">12</a> <a onClick='return showDiv("page_13");' href="#">13</a> <a onClick='return showDiv("page_14");' href="#">14</a> <a onClick='return showDiv("page_15");' href="#">15</a> <a onClick='return showDiv("page_16");' href="#">16</a> <a onClick='return showDiv("page_17");' href="#">17</a> <a onClick='return showDiv("page_18");' href="#">18</a> <a onClick='return showDiv("page_19");' href="#">19</a> <a onClick='return showDiv("page_20");' href="#">20</a> <a onClick='return showDiv("page_21");' href="#">21</a> <a onClick='return showDiv("page_22");' href="#">22</a> <a onClick='return showDiv("page_23");' href="#">23</a> <a onClick='return showDiv("page_24");' href="#">24</a> <a onClick='return showDiv("page_25");' href="#">25</a> </span> </span> <a id="NextPageLink" onclick='return showDiv("page_11");' href="#" title="Next Page"> <img id="NextPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.next.18x20.png" alt="Next Page" /></a> <a id="LastPageLink" onclick='return showDiv("page_25.0");' href="#" title="Last Page"> <img id="LastPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.last.18x20.png" alt="Last Page" /></a> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">181</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/23675617"> <span id="translatedtitle">Electromagnetic field occupational exposure: <span class="hlt">non-thermal</span> vs. thermal effects.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">There are a variety of definitions for "<span class="hlt">non-thermal</span> effects" included in different international standards. They start by the simple description that they are "effects of electromagnetic energy on a body that are not heat-related effects", passing through the very general definition related to low-level effects: "biological effects ascribed to exposure to low-level electric, magnetic and electromagnetic fields, i.e. at or below the corresponding dosimetric reference levels in the frequency range covered in this standard (0 Hz-300 GHz)", and going to the concrete definition of "the stimulation of muscles, nerves, or sensory organs, vertigo or phosfenes". Here, we discuss what kind of effect does the <span class="hlt">non-thermal</span> one has on human body and give data of measurements in different occupations with low-frequency sources of electromagnetic field such as electric power distribution systems, transformers, MRI systems and : video display units (VDUs), whereas thermal effects should not be expected. In some of these workplaces, values above the exposure limits could be found, nevertheless that they are in the term "<span class="hlt">non-thermal</span> effects" on human body. Examples are workplaces in MRI, also in some power plants. Here, we will not comment on <span class="hlt">non-thermal</span> effects as a result of RF or microwave exposure because there are not proven evidence about the existance of such effects and mechanisms for them are not clear. PMID:23675617</p> <div class="credits"> <p class="dwt_author">Israel, M; Zaryabova, V; Ivanova, M</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-06-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">182</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://oaspub.epa.gov/eims/eimsapi.dispdetail?deid=18854"> <span id="translatedtitle">FEASIBILITY ANALYSIS REPORT FOR HYBRID <span class="hlt">NON-THERMAL</span> PLASMA REACTORS</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://oaspub.epa.gov/eims/query.page">EPA Science Inventory</a></p> <p class="result-summary">The purpose of SERDP project CP-1038 is to evaluate and develop <span class="hlt">non-thermal</span> plasma (NTP) reactor technology for DoD air emissions control applications. The primary focus is on oxides of nitrogen (NOx) and a secondary focus on hazardous air pollutants (HAPs), especially volatile o...</p> <div class="credits"> <p class="dwt_author"></p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">183</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/12672176"> <span id="translatedtitle">Discovery of Soft Spectral Component and Transient 22.7s <span class="hlt">Quasi</span> <span class="hlt">Periodic</span> Oscillations of SAX J2103.5+4545</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">XMM-Newton observed SAX J2103.5+4545 on January 6, 2003, while RXTE was\\u000amonitoring the source. Using RXTE-PCA dataset between December 3, 2002 and\\u000aJanuary 29, 2003, the spin period and average spin-up rate during the\\u000aXMM-Newton observations were found to be $354.7940\\\\pm0.0008$ s and\\u000a$(7.4\\\\pm0.9)\\\\times10^{-13}$Hz s$^{-1}$ respectively. In the power spectrum of\\u000athe 0.9-11 keV EPIC-PN lightcurve, we found <span class="hlt">quasi</span> <span class="hlt">periodic</span></p> <div class="credits"> <p class="dwt_author">J. Swank; A. Baykal; M. J. Stark</p> <p class="dwt_publisher"></p> <p class="publishDate">2004-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">184</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2014MNRAS.440.3011O"> <span id="translatedtitle">The 2:3:6 <span class="hlt">quasi-periodic</span> oscillation structure in GRS 1915+105 and cubic subharmonics in the context of relativistic discoseismology</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">We propose a simple toy model to explain the 2:3:6 <span class="hlt">quasi-periodic</span> oscillation (QPO) structure in GRS 1915+105 and, more generally, the 2:3 QPO structure in XTE J1550-564, GRO J1655-40 and H1743-322. The model exploits the onset of subharmonics in the context of discoseismology. We suggest that the observed frequencies may be the consequence of a resonance between a fundamental g mode and an unobservable p wave. The results include the prediction that, as better data become available, a QPO with a frequency of twice the higher twin frequency and a large quality factor will be observed in twin peak sources, as it might already have been observed in the especially active GRS 1915+105.</p> <div class="credits"> <p class="dwt_author">Ortega-Rodríguez, M.; Solís-Sánchez, H.; López-Barquero, V.; Matamoros-Alvarado, B.; Venegas-Li, A.</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-06-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">185</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=19910053084&hterms=Yoshida&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D40%26Ntt%3DYoshida"> <span id="translatedtitle">Relation between the <span class="hlt">quasi-periodic</span> oscillations and the low-frequency noise of GX 5-1 in the horizontal branch</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">Ginga observations of <span class="hlt">quasi-periodic</span> oscillations (QPOs) and the low-frequency noise (LFN) from GX 5-1 in its horizontal-branch spectral state are presented. Power spectral fits were attempted using model functions based on simple oscillating shot models. A clear second-harmonic peak of QPO was detected. Variations in the powers of QPO and LFN on timescales of 8-256 s were also studied. These variations were significant for all of the timescales studied, and were uncorrelated with each other on timescales shorter than a few tens of seconds, and correlated on longer timescales. From simulations based on a simple shot model, it was found that the variation amplitude and the lack of correlation on short timescales are not inconsistent with the oscillating shot models. A more complex model is necessary to fully explain the observed properties.</p> <div class="credits"> <p class="dwt_author">Mitsuda, Kazuhisa; Dotani, Tadayasu; Yoshida, Atsumasa; Vaughan, Brian; Norris, Jay P.</p> <p class="dwt_publisher"></p> <p class="publishDate">1991-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">186</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/54018631"> <span id="translatedtitle"><span class="hlt">Non-thermal</span> Air Plasma at Atmospheric Pressure</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">An AC-driven, <span class="hlt">non-thermal</span>, atmospheric pressure air plasma is generated within the gap separating a disk-shaped metal electrode and a water electrode. The plasma species are identified by emission spectroscopy. The ignition phase and the steady-state are studied by a high-speed CCD camera. It is found that the plasma always initiates at the surface of the water electrode. The plasma exhibits</p> <div class="credits"> <p class="dwt_author">Xinpei Lu; Leipold Frank; O. Minayeva; Mounir Laroussi</p> <p class="dwt_publisher"></p> <p class="publishDate">2003-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">187</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2013JASTP..99..123M"> <span id="translatedtitle">Non-typical ground-based <span class="hlt">quasi-periodic</span> VLF emissions observed at L˜5.3 under quiet geomagnetic conditions at night</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Non-typical long lasting <span class="hlt">quasi-periodic</span> (QP) VLF emissions have been recorded in Northern Finland at L˜5.3 during the recent Finnish VLF campaign held in December 2011. Contrary to the typical daytime QP emissions, the night-time and early morning (00-05UT) event reported here for the first time is a sequence of 1.5-3.5kHz noise bursts lasting for several tens of seconds with an unusually long repetition period which gradually decreases from ˜700s to ˜50s. These QP emissions were observed under conditions of very quiet geomagnetic activity (Kp=0). In spite of that, the interplanetary magnetic field generally had a small southward component, and a high-latitude substorm occurred on the night-side. After this substorm, the repetition period of the VLF bursts suddenly dropped from ˜200s to˜60s and the spectral structure of QP wave changed. We attribute these QP emissions to auto-oscillations of the cyclotron instability of the Earth's radiation belts. According to the theory, the repetition period of the QP should be inversely proportional to the flux of the gyroresonant energetic electrons. Thus the increased flux of energetic electrons injected by the substorm probably led to the decreasing QP repetition periods.</p> <div class="credits"> <p class="dwt_author">Manninen, J.; Kleimenova, N. G.; Kozyreva, O. V.; Bespalov, P. A.; Kozlovsky, A. E.</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-07-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">188</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2012MNRAS.427..595M"> <span id="translatedtitle">Discovery of two simultaneous non-harmonically related <span class="hlt">quasi-periodic</span> oscillations in the 2005 outburst of the black hole binary GRO J1655-40</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">We studied the low-frequency <span class="hlt">quasi-periodic</span> oscillations (LFQPOs) in the black hole GRO J1655-40 during the 2005 outburst, using data from the Rossi X-ray Timing Explorer. All LFQPOs could be identified as either type B or type C using previously proposed classification schemes. In the soft state of the outburst the type-C LFQPOs reached frequencies that are among the highest ever seen for LFQPOs in black holes. At the peak of the outburst, in the ultraluminous state, the power spectrum showed two simultaneous, non-harmonically related peaks which we identified as a type-B and a type-C QPO. The simultaneous presence of a type-C and type-B QPO shows that at least two of the three known LFQPO types are intrinsically different and likely the result of distinct physical mechanisms. We also studied the properties of a broad peaked noise component in the power spectra of the ultraluminous state. This noise component becomes more coherent with count rate and there are strong suggestions that it evolves into a type-B QPO at the highest observed count rates.</p> <div class="credits"> <p class="dwt_author">Motta, S.; Homan, J.; Muñoz Darias, T.; Casella, P.; Belloni, T. M.; Hiemstra, B.; Méndez, M.</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-11-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">189</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/24071524"> <span id="translatedtitle"><span class="hlt">Quasi-periodic</span> patterns (QPP): large-scale dynamics in resting state fMRI that correlate with local infraslow electrical activity.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">Functional connectivity measurements from resting state blood-oxygen level dependent (BOLD) functional magnetic resonance imaging (fMRI) are proving a powerful tool to probe both normal brain function and neuropsychiatric disorders. However, the neural mechanisms that coordinate these large networks are poorly understood, particularly in the context of the growing interest in network dynamics. Recent work in anesthetized rats has shown that the spontaneous BOLD fluctuations are tightly linked to infraslow local field potentials (LFPs) that are seldom recorded but comparable in frequency to the slow BOLD fluctuations. These findings support the hypothesis that long-range coordination involves low frequency neural oscillations and establishes infraslow LFPs as an excellent candidate for probing the neural underpinnings of the BOLD spatiotemporal patterns observed in both rats and humans. To further examine the link between large-scale network dynamics and infraslow LFPs, simultaneous fMRI and microelectrode recording were performed in anesthetized rats. Using an optimized filter to isolate shared components of the signals, we found that time-lagged correlation between infraslow LFPs and BOLD is comparable in spatial extent and timing to a <span class="hlt">quasi-periodic</span> pattern (QPP) found from BOLD alone, suggesting that fMRI-measured QPPs and the infraslow LFPs share a common mechanism. As fMRI allows spatial resolution and whole brain coverage not available with electroencephalography, QPPs can be used to better understand the role of infraslow oscillations in normal brain function and neurological or psychiatric disorders. PMID:24071524</p> <div class="credits"> <p class="dwt_author">Thompson, Garth John; Pan, Wen-Ju; Magnuson, Matthew Evan; Jaeger, Dieter; Keilholz, Shella Dawn</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">190</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2014CRPhy..15..468S"> <span id="translatedtitle"><span class="hlt">Non-thermal</span> plasma potentialities for microwave device reconfigurability</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Three examples of results achieved from cooperative works with microwave and plasma research groups in Toulouse (France) are presented in this paper. They are focused on the use of few <span class="hlt">non-thermal</span> plasmas to make a microwave device reconfigurable. The relative permittivity of such a plasma medium can be tuned from unity to negative values. This special feature appears to be very attractive, although the electromagnetic losses are significant. The use of plasmas with planar waveguides and within metamaterials is discussed. In addition, the basic principles of a scanning antenna built with a leaky wave in a plasma layer are presented.</p> <div class="credits"> <p class="dwt_author">Sokoloff, Jérôme; Pascal, Olivier; Callegari, Thierry; Pascaud, Romain; Pizarro, Francisco; Liard, Laurent; Lo, Juslan; Kallel, Asma</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-05-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">191</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2011SJRUE...6...31I"> <span id="translatedtitle"><span class="hlt">Non-thermal</span> Plasma for VOC Treatment in Flue Gases</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">The paper discusses <span class="hlt">non-thermal</span> plasmas, their generation and characteristics, formation mechanisms of ozone and the treatment of volatile organic compounds (VOCs). In the experimental part, undecane (C11H24 as model VOCs) was treated with assistance of low temperature plasma at an atmospheric pressure which was generated in the so-called stack reactor. The gas composition was 13% of oxygen in nitrogen with impurities of carbon dioxide, carbon monoxide and undecane. The formation of by-products, as well as the removal efficiency, were investigated.</p> <div class="credits"> <p class="dwt_author">Ikaunieks, Janis; Mezmale, Liga; Zandeckis, Aivars; Pubule, Jelena; Blumberga, Andra; Veidenbergs, Ivars</p> <p class="dwt_publisher"></p> <p class="publishDate">2011-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">192</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2012PSST...21c4018Z"> <span id="translatedtitle">A dc <span class="hlt">non-thermal</span> atmospheric-pressure plasma microjet</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">A direct current (dc), <span class="hlt">non-thermal</span>, atmospheric-pressure plasma microjet is generated with helium/oxygen gas mixture as working gas. The electrical property is characterized as a function of the oxygen concentration and show distinctive regions of operation. Side-on images of the jet were taken to analyze the mode of operation as well as the jet length. A self-pulsed mode is observed before the transition of the discharge to normal glow mode. Optical emission spectroscopy is employed from both end-on and side-on along the jet to analyze the reactive species generated in the plasma. Line emissions from atomic oxygen (at 777.4 nm) and helium (at 706.5 nm) were studied with respect to the oxygen volume percentage in the working gas, flow rate and discharge current. Optical emission intensities of Cu and OH are found to depend heavily on the oxygen concentration in the working gas. Ozone concentration measured in a semi-confined zone in front of the plasma jet is found to be from tens to ˜120 ppm. The results presented here demonstrate potential pathways for the adjustment and tuning of various plasma parameters such as reactive species selectivity and quantities or even ultraviolet emission intensities manipulation in an atmospheric-pressure <span class="hlt">non-thermal</span> plasma source. The possibilities of fine tuning these plasma species allows for enhanced applications in health and medical related areas.</p> <div class="credits"> <p class="dwt_author">Zhu, WeiDong; Lopez, Jose L.</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-06-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">193</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2002NuPhB.647..252A"> <span id="translatedtitle"><span class="hlt">Non-thermal</span> leptogenesis from the heavier Majorana neutrinos</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">We investigate a scheme for making leptogenesis by means of the /CP violating decays of the seesaw Majorana neutrinos proposed by Fukugita and Yanagida. However, in order to avoid the wash-out of the produced lepton number we propose the production of the Majorana neutrinos to occur <span class="hlt">non-thermally</span> and sufficiently late. After this time, in consequence, the /B-L (baryon minus lepton) quantum number becomes a good ``accidental symmetry'' protecting the asymmetry produced. This <span class="hlt">non-thermal</span> leptogenesis at late time is realized by a boson decaying into the Majorana neutrinos with a long lifetime. Suggestively this boson could correspond to a scalar field which causes the cosmic inflation, the inflaton, and thus its decay means really the reheating of the Universe. We find that this mechanism works well even if the lightest Majorana neutrinos are not produced sufficiently or not present, and the decays of the heavier seesaw Majorana neutrinos can be responsible to the baryon asymmetry in the present Universe, as we illustrate by the example of the family replicated gauge group model.</p> <div class="credits"> <p class="dwt_author">Asaka, T.; Nielsen, H. B.; Takanishi, Y.</p> <p class="dwt_publisher"></p> <p class="publishDate">2002-12-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">194</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/servlets/purl/839988"> <span id="translatedtitle">MERCURY OXIDIZATION IN <span class="hlt">NON-THERMAL</span> PLASMA BARRIER DISCHARGE SYSTEM</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">In the past decade, the emission of toxic elements from human activities has become a matter of great public concern. Hg, As, Se and Cd typically volatilize during a combustion process and are not easily caught with conventional air pollution control techniques. In addition, there is no pollution prevention technique available now or likely be available in the foreseeable future that can prevent the emission of these trace elements. These trace elements pose additional scientific challenge as they are present at only ppb levels in large gas streams. Mercury, in particular, has attracted significant attention due to its high volatility, toxicity and potential threat to human health. In the present research work, a <span class="hlt">non-thermal</span> plasma dielectric barrier discharge technique has been used to oxidize Hg{sup 0}(g) to HgO. The basic premise of this approach is that Hg{sup 0} in vapor form cannot be easily removed in an absorption tower whereas HgO as a particulate is amiable to water scrubbing. The work presented in this report consists of three steps: (1) setting-up of an experimental apparatus to generate mercury vapors at a constant rate and modifying the existing <span class="hlt">non-thermal</span> plasma reactor system, (2) solving the analytical challenge for measuring mercury vapor concentration at ppb level, and (3) conducting experiments on mercury oxidation under plasma conditions to establish proof of concept.</p> <div class="credits"> <p class="dwt_author">V.K. Mathur</p> <p class="dwt_publisher"></p> <p class="publishDate">2003-02-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">195</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2006MNRAS.367.1562W"> <span id="translatedtitle">Dwarf nova oscillations and <span class="hlt">quasi-periodic</span> oscillations in cataclysmic variables - IV. Observations of frequency doubling and tripling in VW Hyi</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">We present new observations of the rapid oscillations in the dwarf nova VW Hyi, made late in outburst. These dwarf nova oscillations (DNOs) increase in period until they reach 33 s, when a transition to a strong 1st harmonic and weak fundamental takes place. After further period increase, the 2nd harmonic appears; often all three components are present simultaneously. This 1:2:3 frequency suite is similar to what has been seen in some neutron star and black hole X-ray binaries, but has not previously been seen in a cataclysmic variable. When studied in detail, the fundamental and 2nd harmonic vary similarly in phase, but the 1st harmonic behaves independently, though keeping close to twice the frequency of the fundamental. The fundamental period of the DNOs, as directly observed or inferred from the harmonics, increases to ~100 s before the oscillation disappears as the star reaches quiescence. Its maximum period is close to that of the `longer-period' DNOs observed in VW Hyi. The <span class="hlt">quasi-periodic</span> oscillations (QPOs), which have fundamental periods 400-1000 s, behave in the same way, showing 1st and 2nd harmonics at approximately the same times as the DNOs. We explore some possible models. One in which the existence of the 1st harmonic is due to the transition from viewing a single accretion region to viewing two regions, and the rate of accretion on to the primary is modulated at the frequency of the 1st harmonic, as in the `beat frequency model', can generate the suite of DNO frequencies observed. But the behaviour of the QPOs is not yet understood.</p> <div class="credits"> <p class="dwt_author">Warner, Brian; Woudt, Patrick A.</p> <p class="dwt_publisher"></p> <p class="publishDate">2006-04-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">196</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=20120012493&hterms=AIDS+controversy&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D60%26Ntt%3DAIDS%2Bcontroversy"> <span id="translatedtitle">Evidence for <span class="hlt">Quasi-Periodic</span> X-ray Dips from an ULX: Implications for the Binary Motion and the Orbital Inclination</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">We report results from long-term X-ray (0.3-8.0 keY) monitoring of the ultraluminous X-ray source NGC 5408 X-1 with the Swift/X-Ray Telescope. Our primary results are: (1) the discovery of <span class="hlt">quasi-periodic</span> dips in the X-ray intensity that recur on average every 243 days, (2) the detection of an energy-dependent (variability amplitude decreases with increasing energy), quasi-sinusoidal X-ray modulation with a period of 112.6 +/- 4 days the amplitude of which decreases during the second half of the light curve and (3) energy spectral evidence for an increase in photoelectric absorption during the last continuous segment of the data, possibly due to a change in the ionization state of the circumbinary material. We interpret the X-ray modulations in the context of binary motion in analogy to that seen in high-inclination low-mass X-ray binaries. If correct, this implies that NGC 5408 X-1 is in a binary with an orbital period of 243 +/- 23 days in contrast to the 115.5 day quasi-sinusoidal period previously reported. In addition, if the X-ray modulation is caused by vertically structured obscuring material in the accretion disk (similar to the phenomenon of dipping LMXBs), this would imply a high value for the inclination of the orbit. A comparison with estimates from accreting X-ray binaries suggests an inclination approx > 60 deg. We note that, in principle, a precessing accretion disk could also produce the observed X-ray modulations.</p> <div class="credits"> <p class="dwt_author">Pasham, Dheeraj R.; Strohmayer, Tod E.</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">197</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2004ApJ...616..463I"> <span id="translatedtitle">Discovery of a Soft Spectral Component and Transient 22.7 Second <span class="hlt">Quasi-periodic</span> Oscillations of SAX J2103.5+4545</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">XMM-Newton observed SAX J2103.5+4545 on 2003 January 6, while the Rossi X-Ray Timing Explorer (RXTE) was also monitoring the source. Using the RXTE Proportional Counter Array data set between 2002 December 3 and 2003 January 29, the spin period and average spin-up rate during the XMM-Newton observations were found to be 354.7940+/-0.0008 s and (7.4+/-0.9)×10-13 Hz s-1, respectively. In the power spectrum of the 0.9-11 keV EPIC PN light curve, we found <span class="hlt">quasi-periodic</span> oscillations (QPOs) around 0.044 Hz (22.7 s) with an rms fractional amplitude of ~6.6%. We interpreted this QPO feature as the Keplerian motion of inhomogeneities through the inner disk. In the X-ray spectrum, in addition to the power-law component with high-energy cutoff and the ~6.4 keV fluorescent iron emission line, we discovered a soft component consistent with blackbody emission with kT~1.9 keV. The pulse phase spectroscopy of the source revealed that the blackbody flux peaked at the peak of the pulse with an emission radius of ~0.3 km, suggesting the polar cap on the neutron star surface as the source of the blackbody emission. The flux of the iron emission line at ~6.42 keV was shown to peak at the off-pulse phase, supporting the idea that this feature arises from fluorescent emission of the circumstellar material around the neutron star rather than the hot region in the vicinity of the neutron star polar cap.</p> <div class="credits"> <p class="dwt_author">?nam, S. Ç.; Baykal, A.; Swank, J.; Stark, M. J.</p> <p class="dwt_publisher"></p> <p class="publishDate">2004-11-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">198</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2010EP%26S...62..413K"> <span id="translatedtitle">Substorm and pseudo-substorm Pi2 pulsations observed during the interval of <span class="hlt">quasi-periodic</span> magnetotail flow bursts: A case study</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">We studied the relationship between midtail flow bursts observed by the Geotail spacecraft and eight Pi2 pulsations near midnight observed at low-latitude Kakioka (KAK, L = 1.26) and high-latitude Tixie (TIX, L = 5.9) stations on 26 October (day 299) 1997, 1100-1600 UT. The Pi2 pulsations at KAK have a great similarity with those at TIX with an out of phase signature. Three of the Pi2 bursts were associated with substorm onsets/intensifications and other five events were associated with pseudo-substorm onsets. The pseudo-substorm Pi2 pulsations exhibited longitudinal phase variations similar to substorm-related Pi2 pulsations. From this observation we suggest that pseudo-substorm associated current system is morphologically the same as substorm current wedge. The substorm Pi2s are enhanced at higher frequency band (˜15-20 mHz) than the frequency band (˜6-15 mHz) of pseudo-substorm Pi2s. We do not attribute these frequency variations to the change of the plasmapause distance, which is favored in the plasmaspheric resonance model. During the five-hour interval, Geotail observed <span class="hlt">quasi-periodic</span> high-speed flow bursts (perpendicular flow velocity V?x > 300 km/s) preceding the low-latitude Pi2 pulsations by ˜35-150 s. It is found that there is no obvious relationship between the speed of the earthward flow burst events and the power of the Pi2 events. This means that enhanced flow speed is not a main factor in controlling a Pi2 power. The waveform and period of the Pi2 pulsations are different from those of the flow bursts except for one event, which was previously reported as BBF-driven Pi2.</p> <div class="credits"> <p class="dwt_author">Kim, K.-H.; Takahashi, K.; Ohtani, S.; Yumoto, K.; Lee, D.-H.; Jin, H.; Seon, J.; Sung, S.-K.</p> <p class="dwt_publisher"></p> <p class="publishDate">2010-04-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">199</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/254432"> <span id="translatedtitle">Frequency variations of <span class="hlt">quasi-periodic</span> ELF-VLF emissions: A possible new ground-based diagnostic of the outer high-latitude magnetosphere</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">Magnetic pulsations and <span class="hlt">quasi-periodic</span> (QP) amplitude modulations of ELF-VLF waves at Pc 3-4 frequencies (15-50 mHz) are commonly observed simultaneously in cusp-latitude data. The naturally occurring ELF-VLF emissions are believed to be modulated within the magnetosphere by the compressional component of geomagnetic pulsations formed external to the magnetosphere. The authors have examined data from South Pole Station (L {approximately} 14) to determine the occurrence and characteristics of QP emissions. On the basis of 14 months of data during 1987 and 1988 they found that QP emissions typically appeared in both the 0.5-1 kHz and 1-2 kHz receiver channels at South Pole Station and ocassionally in the 2-4 kHz channel. The QP emission frequency appeared to depend on solar wind parameters and interplanetary magnetic field (IMF) direction, and the months near fall equinox in both 1987 and 1988 showed a significant increase in the percentage of QP emissions only in the lowest-frequency channel. The authors present a model consistent with these variations in which high-latitude (nonequatorial) magnetic field minima near the magnetopause play a major role, because the field magnitude governs both the frequency of ELF-VLF emissions and the whistler mode propagation cutoffs. Because the field in these regions will be strongly influenced by solar wind and IMF parameters, variations in the frequency of such emissions may be useful in providing ground-based diagnostics of the outer high-latitude magnetosphere. 32 refs., 13 figs.</p> <div class="credits"> <p class="dwt_author">Alford, J.; Engebretson, M. [Ausburg College, Minneapolis, MN (United States)] [Ausburg College, Minneapolis, MN (United States); Arnoldy, R. [Univ. of New Hampshire, Durham, NH (United States)] [Univ. of New Hampshire, Durham, NH (United States); Inan, U. [Stanford Univ., CA (United States)] [Stanford Univ., CA (United States)</p> <p class="dwt_publisher"></p> <p class="publishDate">1996-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">200</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2013NewA...19..109M"> <span id="translatedtitle">The origin of the most probable 3:2 twin-peak <span class="hlt">quasi-periodic</span> oscillations (QPOs) frequency ratio in the micro-quasars</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">In the present study, we notice that within a few gravitational radii, where the X-ray emission originates, the perturbations in the accretion disk may excite high frequency <span class="hlt">quasi-periodic</span> oscillations (QPOs). The vertical and the radial disk oscillations frequencies due to the perturbation exhibit a 3:2 twin-peak ratio which is most commonly detected in the X-ray fluxes in many Galactic micro-quasars. The high frequency QPOs happen most likely if the oscillations occur very close to the center. We further notice that the perturbations originate in the neighborhood of the shock transition or from a discontinuity in the disk, and could be the possible mechanism to excite the high frequency QPOs. The shocks are more probable in the X-ray emission region and may form very close to the horizon particularly, when the black hole spin is very high. Studying the shock locations as a function of the black hole spin in a fully general relativistic inviscid transonic accretion flows, we calculate the disk oscillation frequencies and their ratios in that perturbed orbit. Further, from the spin dependence, we estimate the 'most probable spin interval' in the micro-quasars by considering the 1/M scaling hypothesis in high frequency QPOs. Finally, we find the spin (a) interval which lies for XTE 1550-564, at a ˜ (0.89-0.99), for the GRO 1655-40, at a ˜ (0.96-0.99) and for the GRS 1915+105, at a ˜ (0.74-0.999). The uncertainty in the mass analysis corresponds to the above spin intervals.</p> <div class="credits"> <p class="dwt_author">Mondal, Soumen; Choi, C. S.</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-02-01</p> </div> </div> </div> </div> <div id="filter_results_form" class="filter_results_form floatContainer" style="visibility: visible;"> <div style="width:100%" id="PaginatedNavigation" class="paginatedNavigationElement"> <a id="FirstPageLink" onclick='return showDiv("page_1");' href="#" title="First Page"> <img id="FirstPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.first.18x20.png" alt="First Page" /></a> <a id="PreviousPageLink" onclick='return showDiv("page_9");' href="#" title="Previous Page"> <img id="PreviousPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.previous.18x20.png" alt="Previous Page" /></a> <span id="PageLinks" class="pageLinks"> <span> <a onClick='return showDiv("page_1");' href="#">1</a> <a onClick='return showDiv("page_2");' href="#">2</a> <a onClick='return showDiv("page_3");' href="#">3</a> <a onClick='return showDiv("page_4");' 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onclick='return showDiv("page_25.0");' href="#" title="Last Page"> <img id="LastPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.last.18x20.png" alt="Last Page" /></a> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">201</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2013ApJ...775...28S"> <span id="translatedtitle">A Spectral Study of the Rapid Transitions of Type-B <span class="hlt">Quasi-periodic</span> Oscillations in the Black Hole Transient XTE J1859+226</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">The fast transitions of type-B and type-A <span class="hlt">quasi-periodic</span> oscillations (QPOs) are rarely found, and they are observed at the peak of the outburst in black hole transient (BHT) sources. The associated spectral variations during such events are crucial to understand the origin and location of such QPOs in the accretion disk. During the 1999 outburst of XTE J1859+226, on four occasions a rapid transition of type-B/A QPOs was noted. We performed broadband spectral analysis on these four observations to unveil the responsible spectral parameter causing the rapid transitions. After invoking simple spectral models, it was observed that disk parameters were consistently varying along with disk and power-law fluxes, and almost no change was noted in the power-law index parameter. Though using a complex physical model showed consistent results, the spectral parameter variations across the transitions were not significant. It was observed that the type-B QPO was always associated with an inner disk front which is closer to the BH. In one observation, a type-A QPO appeared as the source count rate suddenly dropped, and the power-law index as well as disk normalization parameter considerably changed during this transition. The spectral changes in this particular observation were similar to the changes observed in XTE J1817-330, indicating a common underlying mechanism. We have also examined a similar observation of BHT source GX 339-4, where a sudden transition of a type-A/B QPO was noted. Similar spectral study again revealed that the disk parameters were changing. We discuss the results in the framework of a truncated disk model and conclude that the movement of the coupled inner disk-corona region is responsible for such rapid transitions of type-B QPOs.</p> <div class="credits"> <p class="dwt_author">Sriram, K.; Rao, A. R.; Choi, C. S.</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-09-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">202</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/22036924"> <span id="translatedtitle"><span class="hlt">QUASI-PERIODIC</span> FAST-MODE WAVE TRAINS WITHIN A GLOBAL EUV WAVE AND SEQUENTIAL TRANSVERSE OSCILLATIONS DETECTED BY SDO/AIA</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">We present the first unambiguous detection of <span class="hlt">quasi-periodic</span> wave trains within the broad pulse of a global EUV wave (so-called EIT wave) occurring on the limb. These wave trains, running ahead of the lateral coronal mass ejection (CME) front of 2-4 times slower, coherently travel to distances {approx}> R{sub Sun }/2 along the solar surface, with initial velocities up to 1400 km s{sup -1} decelerating to {approx}650 km s{sup -1}. The rapid expansion of the CME initiated at an elevated height of 110 Mm produces a strong downward and lateral compression, which may play an important role in driving the primary EUV wave and shaping its front forwardly inclined toward the solar surface. The wave trains have a dominant 2 minute periodicity that matches the X-ray flare pulsations, suggesting a causal connection. The arrival of the leading EUV wave front at increasing distances produces an uninterrupted chain sequence of deflections and/or transverse (likely fast kink mode) oscillations of local structures, including a flux-rope coronal cavity and its embedded filament with delayed onsets consistent with the wave travel time at an elevated (by {approx}50%) velocity within it. This suggests that the EUV wave penetrates through a topological separatrix surface into the cavity, unexpected from CME-caused magnetic reconfiguration. These observations, when taken together, provide compelling evidence of the fast-mode MHD wave nature of the primary (outer) fast component of a global EUV wave, running ahead of the secondary (inner) slow component of CME-caused restructuring.</p> <div class="credits"> <p class="dwt_author">Liu Wei; Nitta, Nariaki V.; Aschwanden, Markus J.; Schrijver, Carolus J.; Title, Alan M.; Tarbell, Theodore D. [Lockheed Martin Solar and Astrophysics Laboratory, 3251 Hanover Street, Palo Alto, CA 94304 (United States); Ofman, Leon, E-mail: weiliu@lmsal.com [Department of Physics, Catholic University of America, Washingtom, DC 20064 (United States)</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-07-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">203</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/5950697"> <span id="translatedtitle"><span class="hlt">Non-thermal</span> observations using EISCAT: Aspect angle dependence</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">Recent observations with the EISCAT incoherent scatter radar have shown large rises in dayside, auroral plasma velocities (>2 km s/sup -1/) over a wide range of latitudes and lasting about an hour. These are larger than the neutral thermal speed, and allow, for the first time, observations of a <span class="hlt">non-thermal</span> plasma over a range of observing angles, revealing a clear angular dependence. The observed ion temperature anisotropy, deduced by assuming a Maxwellian line-of-sight ion velocity distribution, is at least 1.75, which exceeds the theoretical value for a bi-Maxwellian based on a realistic ion-neutral collision model. The apsect angle dependence of the signal spectra also indicates non-Maxwellian plasma. copyright American Geophysical Union 1987</p> <div class="credits"> <p class="dwt_author">Winser, K.J.; Lockwood, M.; Jones, G.O.L.</p> <p class="dwt_publisher"></p> <p class="publishDate">1987-09-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">204</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2000AdSpR..25..741K"> <span id="translatedtitle">Thermal and <span class="hlt">Non-Thermal</span> Emission from Clusters</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">The first results of BeppoSAX on clusters of galaxies are presented. BeppoSAX offers broad-band spectroscopy in the 0.1-100keV band with in addition imaging spectroscopy (arcminute resolution) in the 0.1-10keV band. The high sensitivity and well-behaved point-spread function at high energies allows a study of the spatial distribution of both the iron K? (6.7keV) and K? (8 keV) complex. In the Perseus cluster the observed K?/K? ratio is significantly higher than that predicted by standard thermal emission codes. This ratio decreases significantly outwards, providing evidence for resonance scattering of the iron K? line. Taking this into account the iron abundance in the core of the Perseus cluster is nearly twice as large as previously thought. In A 2199 there is evidence for a hard <span class="hlt">non-thermal</span> tail in the spectrum. Spatially resolved spectroscopy with the MECS instrument shows spectral hardening in the outer parts of the cluster. Moreover the simultaneously taken PDS spectrum of this cluster shows a tail extending up to at least 50keV. Apart from the high-energy spectral component, the LECS data also show evidence for excess emission at large radii. The soft excess was also detected by the DS instrument of EUVE. This together is very suggestive for the presence of inverse Compton emission in A 2199. Recent EUVE and BeppoSAX observations of the Coma cluster also support the presence of strong <span class="hlt">non-thermal</span> emission, in addition to the thermal component. We shorthly discuss a few consequences of these new results for the dynamics of clusters</p> <div class="credits"> <p class="dwt_author">Kaastra, J. S.</p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">205</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2004AGUFM.V13D..04P"> <span id="translatedtitle">Coupling Between Fluid Flow and Heat Transfer - A Mechanism for <span class="hlt">Quasi-Periodic</span> Variations in CO2 Discharges from Deep Underground Sources</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Leakage of CO2 from underground sources is of interest in connection with volcanic hazards assessment, and with the integrity and safety of geologic disposal reservoirs for CO2 that have been proposed as a means for mitigating global warming from atmospheric emissions. Underground accumulations of CO2, whether naturally occurring or man-made, store vast amounts of compressional energy. At subsurface temperature and pressure conditions, CO2 is always buoyant relative to aqueous fluids, and its upward migration may conceivably give rise to a self-enhancing runaway release due to decompression and the much lower viscosity as compared to water. Natural occurrences of CO2 have been implicated in hydrothermal eruptions, and may be capable of causing "pneumatic" eruptions that are not powered by thermal energy. We have performed numerical simulations of CO2 release through fracture zones and faults in order to determine under what conditions, if any, a self-enhancing, eruptive release may be possible. Our simulations include coupling between multiphase fluid flow and associated heat transfer effects, and accurately represent the thermophysical properties of CO2 in sub-critical (liquid or gaseous) and supercritical conditions, as well as transitions between different phase compositions, and phase partitioning between CO2-rich and aqueous phases. The behavior of rising CO2 plumes is found to be strongly affected by heat transfer effects. As supercritical CO2 migrates upward it cools due to expansion. Much stronger cooling may arise from boiling of liquid CO2 that may occur after temperatures and pressures drop below critical values (Tcrit = 31.04 deg-C, Pcrit = 73.82 bar). Our simulations of CO2 migration up a fault zone produce <span class="hlt">quasi-periodic</span> cycling of thermodynamic conditions and substantial variations of CO2 fluxes discharged at the land surface on a time scale of order 1 year. This behavior is explained in terms of an interplay between multiphase flow in the fault zone and conductive heat exchange with surrounding country rock of low permeability. CO2 upflow rates are reduced by heat transfer limitations, which give rise to substantial increase in fluid density as temperatures decline. A better understanding of natural hydrothermal and pneumatic eruptions is necessary in order that the effectiveness and safety of geologic disposal systems for CO2 may be evaluated. This work was supported by the Office of Basic Energy Sciences of the U.S. Department of Energy under Contract No. DE-AC03-76SF00098.</p> <div class="credits"> <p class="dwt_author">Pruess, K.</p> <p class="dwt_publisher"></p> <p class="publishDate">2004-12-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">206</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2011MNRAS.417..250M"> <span id="translatedtitle">Searching for the trigger of the active galactic nucleus <span class="hlt">quasi-periodic</span> oscillation: 8 years of RE J1034+396</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">RE J1034+396 is one of the most extreme narrow-line type 1 Seyfert galaxies detected thus far, showing the only <span class="hlt">quasi-periodic</span> oscillation (QPO) reliably detected in an active galactic nucleus (AGN). Comparison with similar spectral and timing properties observed in the black hole X-ray binary (BHB) GRS 1915+105 suggests that RE J1034+396 is a super-Eddington accretor. A more complete understanding of the behaviour of RE J1034+396 can therefore lead to a unification of the accretion physics between such extreme AGN and super-Eddington BHBs. Here we report on our latest XMM-Newton observations of RE J1034+396, which no longer show the QPO, indicating that this source shows a non-stationary power spectrum. We use spectral and temporal analysis across all five XMM-Newton observations of the source to probe the evolution of the object. The combination of the shape of the fractional variability with energy and the inferred velocity of absorbing material in the line of sight rules out an absorption-only method of creating the QPO. Instead the periodically changing absorption may be produced by the QPO causing a change in ionization state. We extend our analysis by including the covariance spectra which give much better signal-to-noise ratio than an rms spectrum. These reveal a new aspect of the QPO, which is that there is also a small contribution from a soft component which is hotter than the soft excess seen in the mean spectrum. Folding the light curve on the QPO period shows that this component lags behind the hard X-rays. If this is due to reprocessing, then the lag corresponds to a light traveltime across ˜30Rg. Some of the remaining observations have similar energy spectra and covariance spectra, but none of them shows a significant QPO, so we conclude that none of these features is the trigger for the appearance of the QPO in this object.</p> <div class="credits"> <p class="dwt_author">Middleton, Matthew; Uttley, Phil; Done, Chris</p> <p class="dwt_publisher"></p> <p class="publishDate">2011-10-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">207</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2003MNRAS.344L...1L"> <span id="translatedtitle">On the importance of searching for oscillations of the Jovian inner radiation belt with a <span class="hlt">quasi-period</span> of 40 minutes</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Experiments aboard the Ulysses spacecraft discovered <span class="hlt">quasi-periodic</span> bursts of relativistic electrons and of radio emissions with ~40-min period (QP-40) from the south polar direction of Jupiter in 1992 February. Such polar QP-40 burst activities were found to correlate well with arrivals of high-speed solar winds at Jupiter. We advance the physical scenario that the inner radiation belt (IRB) within a distance of ~2-3 RJ (where RJ is the radius of Jupiter), where relativistic electrons are known to be trapped using the diagnostics of synchrotron emissions, can execute global QP-40 magnetoinertial oscillations excited by arrivals of high-speed solar winds at the Jovian magnetosphere. Modulated by such QP-40 IRB oscillations, relativistic electrons trapped in the IRB may escape from the magnetic circumpolar regions during a certain phase of each 40-min period to form circumpolar QP-40 relativistic electron bursts. Highly beamed synchrotron emissions from such QP-40 burst electrons with small pitch angles relative to Jovian magnetic fields at ~30-40 RJ give rise to QP-40 radio bursts with typical frequencies <~0.2 MHz. We predict that the synchrotron brightness of the IRB should vary on QP-40 time-scales upon arrivals of high-speed solar winds with estimated magnitudes >~0.1 Jy, detectable by existing ground-based radio telescopes. The recent discovery of ~45-min pulsations of Jupiter's north polar X-ray hot spot by the High-Resolution Camera (HRC) of the Chandra spacecraft provides strong supporting circumstantial evidence that the IRB neighborhood did oscillate with QP-40 time-scales. Using the real-time solar wind data from the spacecraft Advanced Composition Explorer (ACE), we show here that such QP-40 pulsations of Jupiter's north polar X-ray hot spot did in fact coincide with the arrival of high-speed solar wind at Jupiter. We note also that properly sampled data of simultaneous far-ultraviolet images of auroral ovals obtained by the Hubble Space Telescope imaging spectrograph (HST-STIS) would have contained QP-40 oscillatory signatures. Based on our theoretical analysis, we offer several predictions that can be tested by further spacecraft and ground-based telescope observations.</p> <div class="credits"> <p class="dwt_author">Lou, Yu-Qing; Zheng, Chen</p> <p class="dwt_publisher"></p> <p class="publishDate">2003-09-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">208</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/11882471"> <span id="translatedtitle"><span class="hlt">NON-THERMAL</span> PLASMA TECHNOLOGY FOR DEGRADATION OF ORGANIC COMPOUNDS IN WASTEWATER CONTROL: A CRITICAL REVIEW</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary"><span class="hlt">Non-thermal</span> plasma is an emerging technique in environmental pollution control technology, produced by the high-voltage discharge processes and therefore a large amount of high energy electrons and active species are generated. The degradation of difficult-degraded organic pollutions will be greatly enhanced by the active species generated from <span class="hlt">non-thermal</span> plasma process. However, research on <span class="hlt">non-thermal</span> plasma technology on organic wastewater cleaning</p> <div class="credits"> <p class="dwt_author">Hsu-Hui Cheng; Shiao-Shing Chen; Yu-Chi Wu; Din-Lit Ho</p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">209</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/24246231"> <span id="translatedtitle">Does microwave sterilization of growth media involve any <span class="hlt">non-thermal</span> effect?</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">Fast reactions mediated by microwaves are often attributed by many to <span class="hlt">non-thermal</span> effect. We show here that rapid formation of Maillard reaction products during microwave sterilization of growth medium results from concentration effect and not any <span class="hlt">non-thermal</span> effect. This leads to an improved method for microwave sterilization of growth media. PMID:24246231</p> <div class="credits"> <p class="dwt_author">Bhattacharjee, Mrinal K; Delsol, Jodie K</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">210</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/36013063"> <span id="translatedtitle"><span class="hlt">Non-thermal</span> plasma technologies: New tools for bio-decontamination</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">Bacterial control and decontamination are crucial to industrial safety assessments. However, most recently developed materials are not compatible with standard heat sterilization treatments. Advanced oxidation processes, and particularly <span class="hlt">non-thermal</span> plasmas, are emerging and promising technologies for sanitation because they are both efficient and cheap. The applications of <span class="hlt">non-thermal</span> plasma to bacterial control remain poorly known for several reasons: this technique</p> <div class="credits"> <p class="dwt_author">M. Moreau; N. Orange; M. G. J. Feuilloley</p> <p class="dwt_publisher"></p> <p class="publishDate">2008-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">211</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.physics.sk/aps/pubs/2006/aps-2006-56-2-109.pdf"> <span id="translatedtitle"><span class="hlt">NON-THERMAL</span> PLASMA AT ATMOSPHERIC PRESSURE FOR OZONE GENERATION AND VOLATILE ORGANIC COMPOUNDS DECOMPOSITION1</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary"><span class="hlt">Non-thermal</span> plasma is usually referred to as plasma in which the temperature of electrons is higher than the temperature of ions. The key advantage of the <span class="hlt">non-thermal</span> plasma application for ozone generation and VOC decomposition is the îdirectedî energy consumption. In this case the energy delivered to the discharge is predominantly used for the generation of highly energetic electrons and</p> <div class="credits"> <p class="dwt_author">S. Pek; J. Khun</p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">212</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/servlets/purl/833295"> <span id="translatedtitle"><span class="hlt">Non-Thermal</span> Plasma System Development for CIDI Exhaust Aftertreatment</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">There is a need for an efficient, durable technology to reduce NOx emissions from oxidative exhaust streams such as those produced by compression-ignition, direct injection (CIDI) diesel or lean-burn gasoline engines. A partnership formed between the DOE Office of Advanced Automotive Technology, Pacific Northwest National Laboratory, Oak Ridge National Laboratory and the USCAR Low Emission Technologies Research and Development Partnership is evaluating the effectiveness of a <span class="hlt">non-thermal</span> plasma in conjunction with catalytic materials to mediate NOx and particulate emissions from diesel fueled light duty (CIDI) engines. Preliminary studies showed that plasma-catalyst systems could reduce up to 70% of NOx emissions at an equivalent cost of 3.5% of the input fuel in simulated diesel exhaust. These studies also showed that the type and concentration of hydrocarbon play a key role in both the plasma gas phase chemistry and the catalyst surface chemistry. More recently, plasma/catalyst systems have been evaluated for NOx reduction and particulate removal on a CIDI engine. Performance results for select plasma-catalyst systems for both simulated and actual CIDI exhaust will be presented. The effect of NOx and hydrocarbon concentration on plasma-catalyst performance will also be shown. SAE Paper SAE-2000-01-1601 {copyright} 2000 SAE International. This paper is published on this website with permission from SAE International. As a user of this website, you are permitted to view this paper on-line, download this pdf file and print one copy of this paper at no cost for your use only. The downloaded pdf file and printout of this SAE paper may not be copied, distributed or forwarded to others or for the use of others.</p> <div class="credits"> <p class="dwt_author">Balmer, M. Lou (Pacific Northwest National Laboratory (PNNL)); Tonkyn, Russell (Battelle Pacific Northwest Laboratories (BPNL)); Maupin, Gary; Yoon, Steven; Kolwaite, Ana (PNNL); Barlow, Stephen (BPNL); Domingo, Norberto; Storey, John M. (Oak Ridge National Laboratory); Hoard, John Wm. (Ford Research Laboratory); Howden, Ken (U.S. Dept. of Energy)</p> <p class="dwt_publisher"></p> <p class="publishDate">2000-04-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">213</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2008POBeo..84..405N"> <span id="translatedtitle">Modeling of <span class="hlt">non-thermal</span> plasma in flammable gas mixtures</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">An idea of using plasma-assisted methods of fuel ignition is based on non-equilibrium generation of chemically active species that speed up the combustion process. It is believed that gain in energy consumed for combustion acceleration by plasmas is due to the non-equilibrium nature of discharge plasma, which allows radicals to be produced in an above-equilibrium amount. Evidently, the size of the effect is strongly dependent on the initial temperature, pressure, and composition of the mixture. Of particular interest is comparison between thermal ignition of a fuel-air mixture and <span class="hlt">non-thermal</span> plasma initiation of the combustion. Mechanisms of thermal ignition in various fuel-air mixtures have been studied for years, and a number of different mechanisms are known providing an agreement with experiments at various conditions. The problem is -- how to conform thermal chemistry approach to essentially non-equilibrium plasma description. The electric discharge produces much above-equilibrium amounts of chemically active species: atoms, radicals and ions. The point is that despite excess concentrations of a number of species, total concentration of these species is far below concentrations of the initial gas mixture. Therefore, rate coefficients for reactions of these discharge produced species with other gas mixture components are well known quantities controlled by the translational temperature, which can be calculated from the energy balance equation taking into account numerous processes initiated by plasma. A numerical model was developed combining traditional approach of thermal combustion chemistry with advanced description of the plasma kinetics based on solution of electron Boltzmann equation. This approach allows us to describe self-consistently strongly non-equilibrium electric discharge in chemically unstable (ignited) gas. Equations of pseudo-one-dimensional gas dynamics were solved in parallel with a system of thermal chemistry equations, kinetic equations for charged particles (electrons, positive and negative ions), and with the electric circuit equation. The electric circuit comprises power supply, ballast resistor connected in series with the discharge and capacity. Rate coefficients for electron-assisted reactions were calculated from solving the two-term spherical harmonic expansion of the Boltzmann equation. Such an approach allows us to describe influence of thermal chemistry reactions (burning) on the discharge characteristics. Results of comparison between the discharge and thermal ignition effects for mixtures of hydrogen or ethylene with dry air will be reported. Effects of acceleration of ignition by discharge plasma will be analyzed. In particular, the role of singlet oxygen produced effectively in the discharge in ignition speeding up will be discussed.</p> <div class="credits"> <p class="dwt_author">Napartovich, A. P.; Kochetov, I. V.; Leonov, S. B.</p> <p class="dwt_publisher"></p> <p class="publishDate">2008-07-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">214</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ntis.gov/search/product.aspx?ABBR=ADA008271"> <span id="translatedtitle"><span class="hlt">Non-Thermal</span> Features of the Auroral Plasma Due to Precipitating Electrons.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ntis.gov/search/index.aspx">National Technical Information Service (NTIS)</a></p> <p class="result-summary">It is proposed that the non-linear plasma interactions which stabilize the instability between ambient and precipitating plasma electrons can account for several of the observed <span class="hlt">non-thermal</span> features of the auroral plasma. Comparison of measurements with t...</p> <div class="credits"> <p class="dwt_author">K. Papadopoulos T. Coffey</p> <p class="dwt_publisher"></p> <p class="publishDate">1973-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">215</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ntis.gov/search/product.aspx?ABBR=ADA425891"> <span id="translatedtitle"><span class="hlt">Non-Thermal</span> Plasma Decontamination Technology for Forward-Deployed Forces.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ntis.gov/search/index.aspx">National Technical Information Service (NTIS)</a></p> <p class="result-summary"><span class="hlt">Non-thermal</span> plasma processing is an emerging advanced oxidation technology for oxidation of hazardous microorganisms and compounds at low temperature. The plasma generated during an electrical discharge or when an energetic particle beam is injected into ...</p> <div class="credits"> <p class="dwt_author">C. Golkowski</p> <p class="dwt_publisher"></p> <p class="publishDate">2004-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">216</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/26248967"> <span id="translatedtitle"><span class="hlt">Non-thermal</span> plasma processing for environmental protection: decomposition of dilute VOCs in air</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary"><span class="hlt">Non-thermal</span> plasma processing is one of the most hopeful air-cleaning technologies to remove toxic gas contaminants in air. The historical background of the <span class="hlt">non-thermal</span> plasma related with the electrostatics is described and the fundamental experimental system including the reactor designs and their power supplies is introduced. Some experimental results suggested the high potential of the plasma processing to decompose those</p> <div class="credits"> <p class="dwt_author">T. Oda</p> <p class="dwt_publisher"></p> <p class="publishDate">2003-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">217</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2006CoTPh..45.1112D"> <span id="translatedtitle">Compressive and Rarefactive Waves in Dust Plasma with <span class="hlt">Non-thermal</span> Ions</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">The governing equation of the dust fluid with <span class="hlt">non-thermal</span> ions and variable dust charge on dust particles in hot dust plasmas is obtained. Both the compressive and rarefactive waves in this system are investigated. They can be determined by plasma parameters including the temperatures of dust fluid, ions and electrons, as well as the <span class="hlt">non-thermal</span> parameter of ions, and the number densities of the dust particles, the ions and the electrons, etc.</p> <div class="credits"> <p class="dwt_author">Duan, Wen-Shan; Wang, Hong-Yan; John, Parkes</p> <p class="dwt_publisher"></p> <p class="publishDate">2006-06-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">218</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2009GeoRL..3613202R"> <span id="translatedtitle">Emission of <span class="hlt">non-thermal</span> microwave radiation by a Martian dust storm</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">We report evidence for the emission of <span class="hlt">non-thermal</span> microwave radiation by a deep Martian dust storm. The observations were made using an innovative detector that can discriminate between radiation of thermal and <span class="hlt">non-thermal</span> origin by measuring the high order moments of its electric field strength. Measurements with this detector, installed in a 34 m radio telescope of the Deep Space Network (DSN), were made for about 5 hours a day over a dozen days between 22 May and 16 June 2006. <span class="hlt">Non-thermal</span> radiation was detected for a few hours only when a 35 km deep Martian dust storm was within the field of view of the radio telescope on 8 June 2006. The spectrum of the <span class="hlt">non-thermal</span> radiation has significant peaks around predicted values of the lowest three modes of the Martian Schumann Resonance (SR). The SR results from electromagnetic standing waves formed in the concentric spherical cavity between the Martian surface and its ionosphere and forced by large-scale electric discharge. Thus, the <span class="hlt">non-thermal</span> radiation was probably caused by electric discharge in the Martian dust storm.</p> <div class="credits"> <p class="dwt_author">Ruf, Christopher; Renno, Nilton O.; Kok, Jasper F.; Bandelier, Etienne; Sander, Michael J.; Gross, Steven; Skjerve, Lyle; Cantor, Bruce</p> <p class="dwt_publisher"></p> <p class="publishDate">2009-07-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">219</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/21371401"> <span id="translatedtitle">Anisotropic Transport of Electrons in a Novel FET Channel with Chains of InGaAs Nano-Islands Embedded along <span class="hlt">Quasi-Periodic</span> Multi-Atomic Steps on Vicinal (111)B GaAs</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">We have studied electron transport in n-AlGaAs/GaAs heterojunction FET channels, in which chains of InGaAs nano-islands are embedded along <span class="hlt">quasi-periodic</span> steps. By using two samples, conductance G{sub para}(V{sub g}) parallel to the steps and G{sub perp}(V{sub g}) perpendicular to them were measured at 80 K as functions of gate voltage V{sub g}. At sufficiently high V{sub g}, G{sub para} at 80 K is several times as high as G{sub perp}, which manifests the anisotropic two-dimensional transport of electrons. When V{sub g} is reduced to -0.7 V, G{sub perp} almost vanishes, while {sub Gpara} stays sizable unless V{sub g} is set below -0.8 V. These results indicate that 'inter-chain' barriers play stronger roles than 'intra-chain' barriers.</p> <div class="credits"> <p class="dwt_author">Akiyama, Y.; Kawazu, T. [National Institute for Materials Science, Tsukuba-shi, Ibaraki 305-0047 (Japan); IIS, University of Tokyo, Meguro-ku, Tokyo 153-8505 (Japan); Noda, T. [National Institute for Materials Science, Tsukuba-shi, Ibaraki 305-0047 (Japan); Sakaki, H. [National Institute for Materials Science, Tsukuba-shi, Ibaraki 305-0047 (Japan); IIS, University of Tokyo, Meguro-ku, Tokyo 153-8505 (Japan); Toyota Technological Institute, Tempaku-ku, Nagoya 468-8511 (Japan)</p> <p class="dwt_publisher"></p> <p class="publishDate">2010-01-04</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">220</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2004P%26SS...52..543K"> <span id="translatedtitle"><span class="hlt">Quasi-periodic</span> emissions (15- 80 min) from the poles of Jupiter as a principal source of the large-scale high-latitude magnetopause boundary layer of energetic particle</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">In this study, we concentrate on the examination of the <span class="hlt">quasi-periodic</span> behavior of 0.5- 1.6 MeV(˜40-400 keV) protons (electrons) and of relativistic (>16 MeV) electrons, observed at Jupiter by two different experiments onboard Ulysses, the HI-SCALE and COSPIN, respectively, within the large-scale south duskside magnetopause boundary layer (MPBL) of energetic particles, from ˜20:00 UT, day 41, to 12:00 UT, day 43. During those times, the observations confirm the transition of Ulysses to an important magnetospheric region with particle intensities comparable to the magnetodisk levels. A careful analysis of high time-resolution intensity, anisotropy and spectral measurements suggests the following: (1) The <span class="hlt">quasi-periodic</span> ˜40 min (QP-40) energetic electron (>˜40 keV) and proton (>˜0.5 MeV) emissions from the south pole were a characteristic phenomenon in the south duskside MPBL; an almost continuous QP 40-min variation has been confirmed in energetic electron observations. (2) When the QP-40 modulation was not evident in energetic particle intensities, it was still detectable in spectral and anisotropy observations. (3) The QP-40 emission is a principal, but not the only periodic, energetic electron and proton emission; other periodicities (˜15, ˜20, ˜30, ˜50, ˜60, ˜80 min) were also significant in energetic particle spectral and anisotropy observations. We infer that QP-40 emissions along with other periodic emissions (˜15, ˜20, ˜30, ˜50, ˜60, ˜80 min) were the principal source of the large-scale high-latitude MPBL of energetic particles during Ulysses outbound pass of Jupiter.</p> <div class="credits"> <p class="dwt_author">Karanikola, I.; Athanasiou, M.; Anagnostopoulos, G. C.; Pavlos, G. P.; Preka-Papadema, P.</p> <p class="dwt_publisher"></p> <p class="publishDate">2004-04-01</p> </div> </div> </div> </div> <div id="filter_results_form" class="filter_results_form floatContainer" style="visibility: visible;"> <div style="width:100%" id="PaginatedNavigation" class="paginatedNavigationElement"> <a id="FirstPageLink" onclick='return showDiv("page_1");' href="#" title="First Page"> <img id="FirstPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.first.18x20.png" alt="First Page" /></a> <a id="PreviousPageLink" onclick='return showDiv("page_10");' href="#" title="Previous Page"> <img id="PreviousPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.previous.18x20.png" alt="Previous Page" /></a> <span id="PageLinks" class="pageLinks"> <span> <a onClick='return showDiv("page_1");' href="#">1</a> <a onClick='return showDiv("page_2");' href="#">2</a> <a onClick='return showDiv("page_3");' href="#">3</a> <a onClick='return 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href="#">11</a> <a style="font-weight: bold;">12</a> <a onClick='return showDiv("page_13");' href="#">13</a> <a onClick='return showDiv("page_14");' href="#">14</a> <a onClick='return showDiv("page_15");' href="#">15</a> <a onClick='return showDiv("page_16");' href="#">16</a> <a onClick='return showDiv("page_17");' href="#">17</a> <a onClick='return showDiv("page_18");' href="#">18</a> <a onClick='return showDiv("page_19");' href="#">19</a> <a onClick='return showDiv("page_20");' href="#">20</a> <a onClick='return showDiv("page_21");' href="#">21</a> <a onClick='return showDiv("page_22");' href="#">22</a> <a onClick='return showDiv("page_23");' href="#">23</a> <a onClick='return showDiv("page_24");' href="#">24</a> <a onClick='return showDiv("page_25");' href="#">25</a> </span> </span> <a id="NextPageLink" onclick='return showDiv("page_13");' href="#" title="Next Page"> <img id="NextPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.next.18x20.png" alt="Next Page" /></a> <a id="LastPageLink" onclick='return showDiv("page_25.0");' href="#" title="Last Page"> <img id="LastPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.last.18x20.png" alt="Last Page" /></a> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">221</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/18775485"> <span id="translatedtitle"><span class="hlt">Non-thermal</span> plasma technologies: new tools for bio-decontamination.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">Bacterial control and decontamination are crucial to industrial safety assessments. However, most recently developed materials are not compatible with standard heat sterilization treatments. Advanced oxidation processes, and particularly <span class="hlt">non-thermal</span> plasmas, are emerging and promising technologies for sanitation because they are both efficient and cheap. The applications of <span class="hlt">non-thermal</span> plasma to bacterial control remain poorly known for several reasons: this technique was not developed for biological applications and most of the literature is in the fields of physics and chemistry. Moreover, the diversity of the devices and complexity of the plasmas made any general evaluation of the potential of the technique difficult. Finally, no experimental equipment for <span class="hlt">non-thermal</span> plasma sterilization is commercially available and reference articles for microbiologists are rare. The present review aims to give an overview of the principles of action and applications of plasma technologies in biodecontamination. PMID:18775485</p> <div class="credits"> <p class="dwt_author">Moreau, M; Orange, N; Feuilloley, M G J</p> <p class="dwt_publisher"></p> <p class="publishDate">2008-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">222</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/22016149"> <span id="translatedtitle">THE SWIFT BURST ALERT TELESCOPE PERSPECTIVE ON <span class="hlt">NON-THERMAL</span> EMISSION IN HIFLUGCS GALAXY CLUSTERS</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">The search for diffuse <span class="hlt">non-thermal</span>, inverse Compton (IC) emission from galaxy clusters at hard X-ray energies has been underway for many years, with most detections being either of low significance or controversial. In this work, we investigate 14-195 keV spectra from the Swift Burst Alert Telescope (BAT) all-sky survey for evidence of <span class="hlt">non-thermal</span> excess emission above the exponentially decreasing tail of thermal emission in the flux-limited HIFLUGCS sample. To account for the thermal contribution at BAT energies, XMM-Newton EPIC spectra are extracted from coincident spatial regions so that both thermal and <span class="hlt">non-thermal</span> spectral components can be determined simultaneously. We find marginally significant IC components in six clusters, though after closer inspection and consideration of systematic errors we are unable to claim a clear detection in any of them. The spectra of all clusters are also summed to enhance a cumulative <span class="hlt">non-thermal</span> signal not quite detectable in individual clusters. After constructing a model based on single-temperature fits to the XMM-Newton data alone, we see no significant excess emission above that predicted by the thermal model determined at soft energies. This result also holds for the summed spectra of various subgroups, except for the subsample of clusters with diffuse radio emission. For clusters hosting a diffuse radio halo, a relic, or a mini-halo, <span class="hlt">non-thermal</span> emission is initially detected at the {approx}5{sigma} confidence level-driven by clusters with mini-halos-but modeling and systematic uncertainties ultimately degrade this significance. In individual clusters, the <span class="hlt">non-thermal</span> pressure of relativistic electrons is limited to {approx}< 10% of the thermal electron pressure, with stricter limits for the more massive clusters, indicating that these electrons are likely not dynamically important in the central regions of clusters.</p> <div class="credits"> <p class="dwt_author">Wik, Daniel R.; Baumgartner, Wayne H.; Tueller, Jack; Okajima, Takashi [Astrophysics Science Division, NASA/Goddard Space Flight Center, Greenbelt, MD 20771 (United States); Sarazin, Craig L. [Department of Astronomy, University of Virginia, P.O. Box 400325, Charlottesville, VA 22904-4325 (United States); Zhang Yuying [Argelander-Institut fuer Astronomie, Universitaet Bonn, Auf dem Huegel 71, 53121 Bonn (Germany); Mushotzky, Richard F. [Department of Astronomy, University of Maryland, College Park, MD 20742 (United States); Clarke, Tracy E., E-mail: daniel.r.wik@nasa.gov [Naval Research Laboratory, 4555 Overlook Avenue SW, Code 7213, Washington, DC 20375 (United States)</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-03-20</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">223</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2012ApJ...748...67W"> <span id="translatedtitle">The Swift Burst Alert Telescope Perspective on <span class="hlt">Non-thermal</span> Emission in HIFLUGCS Galaxy Clusters</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">The search for diffuse <span class="hlt">non-thermal</span>, inverse Compton (IC) emission from galaxy clusters at hard X-ray energies has been underway for many years, with most detections being either of low significance or controversial. In this work, we investigate 14-195 keV spectra from the Swift Burst Alert Telescope (BAT) all-sky survey for evidence of <span class="hlt">non-thermal</span> excess emission above the exponentially decreasing tail of thermal emission in the flux-limited HIFLUGCS sample. To account for the thermal contribution at BAT energies, XMM-Newton EPIC spectra are extracted from coincident spatial regions so that both thermal and <span class="hlt">non-thermal</span> spectral components can be determined simultaneously. We find marginally significant IC components in six clusters, though after closer inspection and consideration of systematic errors we are unable to claim a clear detection in any of them. The spectra of all clusters are also summed to enhance a cumulative <span class="hlt">non-thermal</span> signal not quite detectable in individual clusters. After constructing a model based on single-temperature fits to the XMM-Newton data alone, we see no significant excess emission above that predicted by the thermal model determined at soft energies. This result also holds for the summed spectra of various subgroups, except for the subsample of clusters with diffuse radio emission. For clusters hosting a diffuse radio halo, a relic, or a mini-halo, <span class="hlt">non-thermal</span> emission is initially detected at the ~5? confidence level—driven by clusters with mini-halos—but modeling and systematic uncertainties ultimately degrade this significance. In individual clusters, the <span class="hlt">non-thermal</span> pressure of relativistic electrons is limited to <~ 10% of the thermal electron pressure, with stricter limits for the more massive clusters, indicating that these electrons are likely not dynamically important in the central regions of clusters.</p> <div class="credits"> <p class="dwt_author">Wik, Daniel R.; Sarazin, Craig L.; Zhang, Yu-Ying; Baumgartner, Wayne H.; Mushotzky, Richard F.; Tueller, Jack; Okajima, Takashi; Clarke, Tracy E.</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-03-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">224</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2010PhDT........28K"> <span id="translatedtitle">Mechanisms of interaction of <span class="hlt">non-thermal</span> plasma with living cells</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Thermal plasmas and lasers have been widely used in medicine to cut, ablate and cauterize tissues through heating; in contrast, <span class="hlt">non-thermal</span> plasma produces various highly active molecules and atoms without heat. As a result, its effects on living cells and tissues could be selective and tunable. This makes <span class="hlt">non-thermal</span> plasma very attractive for medical applications. However, despite several interesting demonstrations of <span class="hlt">non-thermal</span> plasma in blood coagulation and tissue sterilization, the biological and physical mechanisms of its interaction with living cells are still poorly understood impeding further development of <span class="hlt">non-thermal</span> plasma as a clinical tool. Although several possible mechanisms of interaction have been suggested, no systematic experimental work has been performed to verify these hypotheses. Using cells in culture, it is shown in this work that <span class="hlt">non-thermal</span> plasma created by dielectric barrier discharge (DBD) has dose-dependent effects ranging from increasing cell proliferation to inducing apoptosis which are consistent with the effects of oxidative stress. DNA damage is chosen as a marker to assess the effects of oxidative stress in a quantitative manner. It is demonstrated here that plasma induced DNA damage as well as other effects ranging from cell proliferation to apoptosis are indeed due to production of intracellular reactive oxygen species (ROS). We found that DNA damage is initiated primarily by plasma generated active neutral species which cannot be attributed to ozone alone. Moreover, it is found that extracellular media and its components play a critical role in the transfer of the <span class="hlt">non-thermal</span> plasma initiated oxidative stress into cells. Specifically, it is found that the peroxidation efficiency of amino acids is the sole predictor of the ability of the medium to transfer the oxidative stress induced by <span class="hlt">non-thermal</span> plasma. Phosphorylation of H2AX, a DNA damage marker, following plasma treatment is found to be ATR dependent and ATM independent, suggesting that <span class="hlt">non-thermal</span> plasma may induce formation of bulky lesions unlike ionizing radiation (IR) or H2O2 which primarily produce DNA double strand breaks. Moreover, it is found that the pathway by which plasma generated oxidative stress is transferred across cellular membranes does not involve lipid peroxidation by-products, although lipid peroxidation does occur.</p> <div class="credits"> <p class="dwt_author">Kalghatgi, Sameer Ulhas</p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">225</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ntis.gov/search/product.aspx?ABBR=ADA585933"> <span id="translatedtitle"><span class="hlt">Non-Thermal</span> High-Intensity Focused Ultrasound for Breast Cancer Therapy.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ntis.gov/search/index.aspx">National Technical Information Service (NTIS)</a></p> <p class="result-summary">Several in vitro studies have demonstrated the <span class="hlt">non-thermal</span> (< 42 deg C) cell killing effect of pulsed HIFU, which resembles high linear energy transfer (LET) radiation cell damage that is not not affected by the local biochemical environment and shows les...</p> <div class="credits"> <p class="dwt_author">C. M. Ma</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">226</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ntis.gov/search/product.aspx?ABBR=ADA568023"> <span id="translatedtitle"><span class="hlt">Non-thermal</span> High-intensity Focused Ultrasound for Breast Cancer Therapy.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ntis.gov/search/index.aspx">National Technical Information Service (NTIS)</a></p> <p class="result-summary">Several in vitro studies have demonstrated the <span class="hlt">non-thermal</span> (< 42C) cell killing effect of HIFU, which resembles high linear energy transfer (LET) radiation cell damage that is not affected by the local biochemical environment and shows less radiation resi...</p> <div class="credits"> <p class="dwt_author">C. M. Ma</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">227</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/51063907"> <span id="translatedtitle">Treatment of wastewater from paracetamol factory by using <span class="hlt">non-thermal</span> plasma and active carbon</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary"><span class="hlt">Non-thermal</span> plasma combined with activated carbon was developed to purify wastewater from paracetamol factory. The effect of discharge time, discharge voltage, initial pH value of wastewater, velocity of the air flow and whether adding activated carbon on the COD degradation and decolorization ratio were investigated. It was found that as discharge time prolonged, decolorization ratio decreased but the COD degradation</p> <div class="credits"> <p class="dwt_author">Ming-gong Chen; Fang Zhang; Can Cui; Xia Liao; Jing Chen; Jun-feng Rong; Dong-xu Yu</p> <p class="dwt_publisher"></p> <p class="publishDate">2011-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">228</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2014ApJ...787..123H"> <span id="translatedtitle">Energetic Electron Propagation in the Decay Phase of <span class="hlt">Non-thermal</span> Flare Emission</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">On the basis of the trap-plus-precipitation model, the peculiarities of <span class="hlt">non-thermal</span> emission in the decay phase of solar flares have been considered. The calculation formulas for the escape rate of trapped electrons into the loss cone in terms of time profiles of hard X-ray (HXR) and microwave (MW) emission have been obtained. It has been found that the evolution of the spectral indices of <span class="hlt">non-thermal</span> emission depend on the regimes of the pitch angle diffusion of trapped particles into the loss cone. The properties of <span class="hlt">non-thermal</span> electrons related to the HXR and MW emission of the solar flare on 2004 November 3 are studied with Nobeyama Radioheliograph, Nobeyama Radio Polarimeters, RHESSI, and Geostationary Operational Environmental Satellite observations. The spectral indices of <span class="hlt">non-thermal</span> electrons related to MW and HXR emission remained constant or decreased, while the MW escape rate as distinguished from that of the HXRs increased. This may be associated with different diffusion regimes of trapped electrons into the loss cone. New arguments in favor of an important role of the superstrong diffusion for high-energy electrons in flare coronal loops have been obtained.</p> <div class="credits"> <p class="dwt_author">Huang, Jing; Yan, Yihua; Tsap, Yuri T.</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-06-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">229</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://oaspub.epa.gov/eims/eimsapi.dispdetail?deid=18855"> <span id="translatedtitle">EXPERIMENTAL AND CFD STUDIES OF <span class="hlt">NON-THERMAL</span> PLASMAS FOR NOX CONTROL</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://oaspub.epa.gov/eims/query.page">EPA Science Inventory</a></p> <p class="result-summary"><span class="hlt">Non-thermal</span> plasmas (NTPs) represent a promising technology for the destruction of various toxic gases entrained in air streams. One challenging example of the need for hazardous gas control is the jet engine test cell (JETC) facility where very large amounts of NO(x)s are emitte...</p> <div class="credits"> <p class="dwt_author"></p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">230</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/48715476"> <span id="translatedtitle">Direct Nonoxidative Methane Conversion by <span class="hlt">Non-thermal</span> Plasma: Experimental Study</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">The direct non-oxidative conversion of methane to higher hydrocarbons in <span class="hlt">non-thermal</span> plasma, namely dielectric barrier discharge and corona discharge, has been investigated experimentally at atmospheric pressure. In dielectric barrier discharge, the methane is mainly converted to ethane and propane with small amounts of unsaturated and higher hydrocarbons. While in corona discharge, methane was activated mainly to acetylene with small amount</p> <div class="credits"> <p class="dwt_author">Yun Yang</p> <p class="dwt_publisher"></p> <p class="publishDate">2003-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">231</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/18596801"> <span id="translatedtitle">Mediation of the solar wind termination shock by <span class="hlt">non-thermal</span> ions.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">Broad regions on both sides of the solar wind termination shock are populated by high intensities of <span class="hlt">non-thermal</span> ions and electrons. The pre-shock particles in the solar wind have been measured by the spacecraft Voyager 1 (refs 1-5) and Voyager 2 (refs 3, 6). The post-shock particles in the heliosheath have also been measured by Voyager 1 (refs 3-5). It was not clear, however, what effect these particles might have on the physics of the shock transition until Voyager 2 crossed the shock on 31 August-1 September 2007 (refs 7-9). Unlike Voyager 1, Voyager 2 is making plasma measurements. Data from the plasma and magnetic field instruments on Voyager 2 indicate that <span class="hlt">non-thermal</span> ion distributions probably have key roles in mediating dynamical processes at the termination shock and in the heliosheath. Here we report that intensities of low-energy ions measured by Voyager 2 produce <span class="hlt">non-thermal</span> partial ion pressures in the heliosheath that are comparable to (or exceed) both the thermal plasma pressures and the scalar magnetic field pressures. We conclude that these ions are the >0.028 MeV portion of the <span class="hlt">non-thermal</span> ion distribution that determines the termination shock structure and the acceleration of which extracts a large fraction of bulk-flow kinetic energy from the incident solar wind. PMID:18596801</p> <div class="credits"> <p class="dwt_author">Decker, R B; Krimigis, S M; Roelof, E C; Hill, M E; Armstrong, T P; Gloeckler, G; Hamilton, D C; Lanzerotti, L J</p> <p class="dwt_publisher"></p> <p class="publishDate">2008-07-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">232</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://oaspub.epa.gov/eims/eimsapi.dispdetail?deid=29303"> <span id="translatedtitle">FIRST REPORT ON <span class="hlt">NON-THERMAL</span> PLASMA REACTOR SCALING CRITERIA AND OPTIMIZATION MODELS</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://oaspub.epa.gov/eims/query.page">EPA Science Inventory</a></p> <p class="result-summary">The purpose of SERDP project CP-1038 is to evaluate and develop <span class="hlt">non-thermal</span> plasma (NTP) reactor technology for DoD air emissions control applications. The primary focus is on oxides of nitrogen (NOx) and a secondary focus on hazardous air pollutants (HAPs), especially volatile o...</p> <div class="credits"> <p class="dwt_author"></p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">233</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/24749699"> <span id="translatedtitle">Control of multi-drug-resistant pathogens with <span class="hlt">non-thermal</span>-plasma-treated alginate wound dressing.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">Abstract Background: <span class="hlt">Non-thermal</span> dielectric-barrier discharge plasma (<span class="hlt">non-thermal</span> plasma) is being investigated for use in wound healing. Alginate gel, already in clinical use, is non-toxic but has no meaningful antimicrobial property. This study reports that a <span class="hlt">non-thermal</span>-plasma-treated alginate wound dressing has strong antimicrobial properties. Methods: Alginate gel was treated with <span class="hlt">non-thermal</span> plasma in room air and inoculated with bacterial pathogens. At 15?min after this, bacterial cell viability was determined by colony assay or 2,3-bis-(2-methoxy-4- nitro-5-sulfophenyl)-2H-tetrazolium-5-carboxanilide (XTT) assay. The anti-biofilm efficacy of the <span class="hlt">non-thermal</span>-plasma-treated alginate gel was investigated and the treated gel was tested against vascular endothelial cells for a cytotoxic effect. The proliferation and migration of bacterial cells before and after exposure to the treated gel were investigated with an in vitro wound testing assay. Scanning electron microscopy was used to observe changes in the gel surface associated with exposure to bacterial pathogens. The treated gel was tested against Acinetobacter baumannii, Escherichia coli, Staphylococcus aureus, S. epidermidis, Candida albicans, and C. glabrata as representative pathogens (at 10(6)-10(9) colony-forming units [CFU]/mL), and the thickness of a plasma-treated gel dressing and distance between a glass dielectric-barrier discharge plasma probe and the gel surface were kept constant. Results: <span class="hlt">Non-thermal</span>-plasma-treated alginate gel exhibited a strong biocidal property and inactivated all of the pathogens included in the study at counts of 10(8) CFU/mL and within 15?sec of treatment. The treated gel inactivated 10(9) CFU/mL of the organisms within 1?min, and 3 min of exposure to the treated gel inactivated pathogens embedded in biofilms. The plasma-treated gel showed no significant cytotoxicity, and endothelial cells exposed to the treated gel proliferated and migrated well across a wound area over a period of time. Dressings made with the treated gel retained their biocidal effects for about a month. Scanning electron microscopy showed no damage to the surfaces of treated gels, but damage to the bacterial pathogens on plasma exposure. Conclusion: A <span class="hlt">non-thermal</span>-plasma-treated alginate gel dressing has the clinical potential to decontaminate wounds, prevent surgical site infection, and promote wound healing. PMID:24749699</p> <div class="credits"> <p class="dwt_author">Poor, Alexander E; Ercan, Utku K; Yost, Adam; Brooks, Ari D; Joshi, Suresh G</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-06-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">234</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2011PhDT.......128L"> <span id="translatedtitle">The effects of <span class="hlt">non-thermal</span> plasmas on selected mammalian cells</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary"><span class="hlt">Non-thermal</span> plasma surface modifications have become indispensable processing steps in various industry and research sectors. Applications range from semiconductor processing to biotechnology and recently, plasma medicine. <span class="hlt">Non-thermal</span> plasma sources have the advantage that a number of electron-driven chemical reactions can be produced while maintaining the gas (heavy species) temperature low, thus enabling the treatment of temperature-sensitive surfaces such as polymers, tissues and live cells. In the fields of biology and medicine, <span class="hlt">non-thermal</span> plasmas have been primarily used for the deposition or modification of biocompatible polymers and for sterilization. Recently, <span class="hlt">non-thermal</span> plasmas have been used to treat tissues and cells. A new field of research has emerged, Plasma Medicine, which studies the effects of <span class="hlt">non-thermal</span> plasmas on cells and tissues for clinical applications. The Atmospheric Pressure Glow Discharge torch (APGD-t), a <span class="hlt">non-thermal</span> plasma source, built in our laboratory was used to study the effects of <span class="hlt">non-thermal</span> plasmas on mammalian cells. In its first application, we indirectly used the APGD-t to deposit a plasma-polymer on a glass surface and studied its effects on cultured cells. It was shown that the cells grew preferentially on the plasma-polymer, and their proliferation rate increased. The second application of the APGD-t was to further investigate previous observations of cell permeabilization obtained by plasma treatments and to apply <span class="hlt">non-thermal</span> plasmas to cell transfection. It was demonstrated that the APGD-t is able to locally transfect adherent cells. We estimated the diameter of the pores created to be below 10 nm and that the pores remain open for less than 5 seconds. However, while investigating the mechanisms involved in cell transfection we observed that the use of higher gas flows in the negative controls (using the APGD-t but with the plasma turned off) also resulted in cell transfection. To further study this phenomena, we built a simple transfection device consisting of a straight glass capillary tube and a plastic support. Using three different gases and five different capillary diameters, we were able to relate the transfection efficiency to the dynamic pressure of the gas exiting the capillary tube. Finally, even though transfection of cells seem to depend more on the mechanical forces exerted by the gas flow than on the effects of the plasma, other applications of <span class="hlt">non-thermal</span> plasma in the field of medicine are in development. However, published studies have focused on only the positive effects of <span class="hlt">non-thermal</span> plasmas, neglecting the potentially induced adverse effects. Therefore, we studied if damage could be caused in cells following an indirect (APGD-t) or a direct (parallel electrodes DBD) plasma treatment. We found that a low power direct plasma treatment caused oxidative stress in HeLa cells. Both plasma sources were shown to produce DNA double-strand breaks but no lipid peroxidation. Also, the sequencing of plasma-treated naked plasmid DNA introduced in electrocompetent bacteria showed no evidence of mutations.</p> <div class="credits"> <p class="dwt_author">Leduc, Mathieu</p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">235</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2009AGUFMSH21B1516R"> <span id="translatedtitle">The Importance of <span class="hlt">Non-Thermal</span> Pressures in the Heliosheath: Towards New Methods of Analysis</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">The in-situ plasma measurements when Voyager 2 crossed the termination shock into the heliosheath revealed that only ~20% of the downstream pressure resided in the thermal ion population at energies << 1 keV. The LECP ion measurements > 30 keV at both VGRs 1 and 2 implied a partial pressure ?P~0.02pPa that accounted for another ~15% of the total pressure. Adding in the missing 70% of the <span class="hlt">non-thermal</span> pressure, the total <span class="hlt">non-thermal</span> pressure at the VGRs must be P~0.12pPa. Consensus estimates of the local interstellar magnetic field (ISMF) are near B~0.25nT which gives a hydrostatic magnetic pressure B2/2?0~0.25pPa. Cassini/INCA all-sky images of 5-44keV ENAs from the heliosheath [Krimigis et al., this session] show that neither VGR1 nor VGR2 is in the direction of maximum ENA emission. Consequently, it is possible that the pressure of <span class="hlt">non-thermal</span> protons in the heliosheath is comparable to the hydrostatic pressure of the interstellar magnetic field (ISMF) that confines the heliosheath. An immediate corollary is that we will not understand the physics of the heliosheath until we find ways of quantitatively describing the dynamics of pressures produced by <span class="hlt">non-thermal</span> ion populations. Present MHD theories and simulations simply do not capture these essential dynamical processes. We point out that the magnetospheric communities studying the dynamics of <span class="hlt">non-thermal</span> ion injections (with plasma beta>1) at Earth and Saturn revealed by ENA imaging have been making significant progress in a quite similar problem. We offer some possible approaches for the quantitative analysis of the heliosheath, based on the magnetospheric experience.</p> <div class="credits"> <p class="dwt_author">Roelof, E. C.; Gruntman, M.; Krimigis, S. M.; Mitchell, D. G.; McComas, D. J.; Funsten, H. O.</p> <p class="dwt_publisher"></p> <p class="publishDate">2009-12-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">236</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2004AIPC..714..383T"> <span id="translatedtitle">Unified Model of <span class="hlt">Quasi-Periodic</span> Oscillations</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">We present a new theoretical framework for interpreting observed spectral/temporal characteristics of accreting neutron star and black hole systems as gravity wave (g-mode oscillations). This model successfully incorporates features of earlier models (published by the present authors and colleagues over the last several years) into a more general scheme that reduces in one limit to a classic treatment by Chandrasekhar, placing this paradigm in the tradition of his analysis. It goes beyond his treatment in the inclusion of radial dependence, the incorporation of MHD, and the application to X-ray timing phenomenology. The conceptual picture that goes with this idea is one in which the problem of disk accretion onto a (symmetrical) black hole is the starting point; accretion in geometries where symmetries are broken by magnetic fields is treated with extensions or perturbations to that case. Primary emphasis is on understanding QPO features and power spectrum breaks. Pairs or groups of QPOs that evolve in correlated ways are treated as splittings of eigenfrequencies in a fluid dynamics analysis rather than, say, as beat phenomena. One particular QPO is identified with the Kepler (gravitational) frequency and the other QPOs are related to that one. Because the Kepler frequency is Newtonian and not a General Relativistic effect, the entire treatment is Newtonian, but this helps explain how certain relationships appear to extend over ~ six orders of magnitude in frequency, linking white dwarfs, neutron stars, and black holes in a single comprehensive picture. The explanatory range of the theoretical framework is considerable: it addresses the magnetic field strength and configuration near the compact object, the extension of the Keplerian disk near the central object (and the location of the transition between Keplerian and non Keplerian flow), the presence of advection flow along with disk accretion and the conditions for shock formation in the accretion flow. Successes of earlier treatments, for example fitting the correlated drifts of as many as six persistent power density spectrum features (QPOs or breaks) with minimal parametrization are retained in the new unified scheme. Presented calculations are aimed at (i) extending the explanatory range of the model, (ii) working out details and consequences of the new framework that unifies it with Chandrasekhar's analysis, (iii) making it explicitly an MHD model and not simply hydrodynamics, and (iv) validating it with test. The goal is to have a theoretical synthesis of the existing QPO phenomenology that will serve as a starting point for future X-ray timing observations.</p> <div class="credits"> <p class="dwt_author">Titarchuk, Lev; Wood, Kent S.</p> <p class="dwt_publisher"></p> <p class="publishDate">2004-07-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">237</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/18730625"> <span id="translatedtitle"><span class="hlt">Quasi-periodic</span> distributed feedback laser</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">Although lasers have found numerous applications, their design is often still based on the concept of a gain medium within a mirror cavity. Exceptions to this are distributed feedback lasers, in which feedback develops along a periodic structure, or random lasers, which do not require any form of cavity. Random lasers have very rich emission spectra, but are difficult to</p> <div class="credits"> <p class="dwt_author">Lukas Mahler; Alessandro Tredicucci; Fabio Beltram; Christoph Walther; Jérôme Faist; Harvey E. Beere; David A. Ritchie; Diederik S. Wiersma</p> <p class="dwt_publisher"></p> <p class="publishDate">2010-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">238</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ntis.gov/search/product.aspx?ABBR=PB84216704"> <span id="translatedtitle">Non Linear Oscillators with <span class="hlt">Quasi</span> <span class="hlt">Periodic</span> Forcing.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ntis.gov/search/index.aspx">National Technical Information Service (NTIS)</a></p> <p class="result-summary">The paper is organized as follows. In this first chapter we present a more precise setting of the problem and a formulation of the results. To this purpose the author briefly considers the linear case and develop the standard contraction agreement, essent...</p> <div class="credits"> <p class="dwt_author">B. L. J. Braaksma H. W. Broer</p> <p class="dwt_publisher"></p> <p class="publishDate">1983-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">239</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2013MNRAS.435.3494W"> <span id="translatedtitle">Constraints on kilohertz <span class="hlt">quasi-periodic</span> oscillation models and stellar equations of state from SAX J1808.4-3658, Cyg X-2 and 4U 1820-30</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">We test the relativistic precession model (RPM) and the magnetohydrodynamics Alfvén wave oscillation model (AWOM) for the kilohertz (kHz) <span class="hlt">quasi-periodic</span> oscillations (QPOs) from sources with measured neutron star (NS) masses and twin kHz QPO frequencies. For the RPM, the derived NS masses of Cyg X-2, SAX J1808.4-3658 and 4U 1820-30 are 1.96 ± 0.10, 2.83 ± 0.04 and 1.85 ± 0.02 M?, respectively. These are, respectively, ˜30, 100 and 40 per cent higher than the measured results 1.5 ± 0.3, <1.4 and 1.29^{+0.19}_{-0.07} M?. For the AWOM, where the free parameter of the model is the density of the star, we infer the NS radii to be around 10-20 km for the above three sources. Based on this, we can infer the matter compositions inside the NSs with the help of the equations of state. In particular, for SAX J1808.4-3658, the AWOM shows a lower mass density for its NS than those of the other known kHz QPO sources, with a radius range of 17-20 km, which excludes the strange quark matter inside its star.</p> <div class="credits"> <p class="dwt_author">Wang, D. H.; Chen, L.; Zhang, C. M.; Lei, Y. J.; Qu, J. L.</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-11-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">240</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2004HEAD....8.1713Y"> <span id="translatedtitle">Photon-Energy Dependence of the Phase of <span class="hlt">Quasi-Periodic</span> Oscillations in Black Holes and Neutron Stars and the Implications for Models of Their X-Ray Emission</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Using a new method to determine the relative phases of <span class="hlt">quasi-periodic</span> oscillations (QPOs) at low and high photon energies, we find that the 6 Hz oscillations of the QPOs in the black hole X-ray binary XTE J1550-564 and in the 6 Hz normal branch oscillation (NBO) in the neutron star LMXB Sco X-1 exhibit similar trends. In both oscillations, the waveforms shift to later times with increasing photon energy up to about 6--8 keV. Above this energy the trend reverses and the waveforms shift to earlier times with increasing photon energy, eventually leading the waveforms observed at low photon energies. This behavior rules out the possibility that Compton up/down scattering mechanism is the only mechanism responsible for generating the phase shifts. We discuss the implications for models of QPO X-ray spectra and the origin of spectral variability in these X-ray sources. This research was supported in part by NASA grant NAG 5-12030, NSF grant AST 0098399, and the funds of the Fortner Endowed Chair at Illinois. WY thanks M. van der Klis for stimulating comments and the support of NWO grant 614.051.002 at the University of Amsterdam where this study was initiated.</p> <div class="credits"> <p class="dwt_author">Yu, W.; Lamb, F. K.</p> <p class="dwt_publisher"></p> <p class="publishDate">2004-08-01</p> </div> </div> </div> </div> <div id="filter_results_form" class="filter_results_form floatContainer" style="visibility: visible;"> <div style="width:100%" id="PaginatedNavigation" class="paginatedNavigationElement"> <a id="FirstPageLink" onclick='return showDiv("page_1");' href="#" title="First Page"> <img id="FirstPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.first.18x20.png" alt="First Page" /></a> <a id="PreviousPageLink" onclick='return showDiv("page_11");' href="#" title="Previous Page"> <img id="PreviousPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.previous.18x20.png" alt="Previous Page" /></a> <span id="PageLinks" class="pageLinks"> <span> <a onClick='return showDiv("page_1");' href="#">1</a> <a onClick='return showDiv("page_2");' href="#">2</a> <a onClick='return showDiv("page_3");' href="#">3</a> <a onClick='return showDiv("page_4");' 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onclick='return showDiv("page_25.0");' href="#" title="Last Page"> <img id="LastPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.last.18x20.png" alt="Last Page" /></a> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">241</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2012Icar..221..682Y"> <span id="translatedtitle">Mars exospheric thermal and <span class="hlt">non-thermal</span> components: Seasonal and local variations</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">A model of the martian exosphere is built for average solar conditions. A Chamberlain's approach (Chamberlain, J.W. [1963]. Planet. Space Sci. 11, 901) is used to describe the O, CO, CO2, and O2 thermal exospheric components. The average thermal oxygen density at 300 km in altitude varies by about one order of magnitude with seasons. A Monte-Carlo test particle simulation is also developed in order to estimate the <span class="hlt">non-thermal</span> oxygen component of the exosphere. The seasonal variation of the <span class="hlt">non-thermal</span> oxygen average density is much less than the thermal component but displays clear seasonal variations of its spatial distribution. The neutral oxygen atomic escaping flux varies from 2.9 to 5.3 × 1025 s-1 in good agreement with Valeille et al. (Valeille, A., Combi, M.R., Bougher, S.W., Tenishev, V., Nagy, A.F. [2009a]. J. Geophys. Res. (Planets) 114, 11006; Valeille, A., Tenishev, V., Bougher, S.W., Combi, M.R., Nagy, A.F. [2009b]. J. Geophys. Res. (Planets) 114, 11005). Mars's oxygen exosphere is thermal below 600 km and <span class="hlt">non-thermal</span> above 700 km at all seasons. The typical scale height is ˜45 km for thermal O and ˜500 km for the <span class="hlt">non-thermal</span> oxygen density. The total photoionization rate above 300 km corresponds to a CO2+/O total production ratio between 0.004 and 0.02. When compared to the composition of the escaping flux measured by ASPERA-3/Mars Express, this suggests that ions formed below 300 km should significantly contribute to the escaping ion flux and/or that a significant part of the newly O+ ions reimpacts Mars. The simulated oxygen density profile is also compared to the recent observed profile by Alice/Rosetta (Feldman, P.D. et al. [2011]. Icarus 214, 394-399). Although the scale height of our simulated <span class="hlt">non-thermal</span> oxygen exosphere and the transition from thermal to <span class="hlt">non-thermal</span> dominated exospheres are slightly higher than suggested by Feldman et al. (Feldman, P.D. et al. [2011]. Icarus 214, 394-399), a good agreement is found when taking into account the uncertainties of Alice/Rosetta observations.</p> <div class="credits"> <p class="dwt_author">Yagi, M.; Leblanc, F.; Chaufray, J. Y.; Gonzalez-Galindo, F.; Hess, S.; Modolo, R.</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-11-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">242</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2009AIPC.1121..114Z"> <span id="translatedtitle">Spectral Line <span class="hlt">Non-thermal</span> Broadening and MHD Waves in the Solar Corona</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">The rapid temperature rise from the solar surface (6000 K) up to the corona (1 MK) and acceleration of solar wind particles still are unresolved problems in solar physics. The energy source for the coronal heating and the wind acceleration probably lies in the solar photosphere. MHD waves are believed to carry the photospheric energy into the corona. Recent observations from space based telescopes made significant progress in understanding the process of MHD wave propagation from the solar surface towards the corona. Some of MHD wave modes have been observed through intensity variations and Doppler shift oscillations in spectral lines. Another powerful mechanism is to detect the waves through the <span class="hlt">non-thermal</span> broadening of spectral lines. The lecture gives the basic points of wave induced effects in solar coronal spectral lines and recent progress in wave observations through spectral line <span class="hlt">non-thermal</span> broadening.</p> <div class="credits"> <p class="dwt_author">Zaqarashvili, T. V.</p> <p class="dwt_publisher"></p> <p class="publishDate">2009-04-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">243</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2008cosp...37.2695S"> <span id="translatedtitle">Small amplitude solitary structures in multicomponent dusty plasma containing <span class="hlt">non-thermal</span> electrons</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">There has been a rapidly growing interest in the physics of dusty plasma not only because dust is an omnipresent ingredient of our universe, but also because of its vital role in understanding different collective processes in astrophysical and space environments. With the observations that negatively as well as positively charged dusty particles are present in different regions of space such as Jupiter's magnetosphere, upper mesosphere, planetary magnetosphere, interplanetary space etc., it is interesting to investigate the problems in such type of plasma system. In present investigation we have considered that the constituents of dusty plasmas are <span class="hlt">non-thermal</span> electrons, ions, negative as well as positive charged dust particles. We have derived the KdV equation using reductive perturbation method to study the small amplitude solitary potential structures. It has been observed that there is a significant variation of amplitude and width of solitary potentials with the <span class="hlt">non-thermal</span> parameter and other parameters.</p> <div class="credits"> <p class="dwt_author">Singh Saini, Nareshpal</p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">244</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2014AIPC.1588..191C"> <span id="translatedtitle">Study of <span class="hlt">non-thermal</span> plasma jet with dielectric barrier configuration in nitrogen and argon</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Dielectric barrier discharge (DBD) is advantageous in generating <span class="hlt">non-thermal</span> plasma at atmospheric pressure, as it avoids transition to thermal arc and dispenses with costly vacuum system. It has found useful applications in treating heat-sensitive materials such as plastics and living tissue. In this work, the discharge formed between the Pyrex glass layer and the ground electrode is extruded through a nozzle to form the <span class="hlt">non-thermal</span> plasma jet. The DBD characteristics were investigated in terms of charge transferred and mean power dissipated per cycle when operated in nitrogen and argon at various flow rates and applied voltages. These characteristics were then correlated to the dimension of the plasma jet. The mean power dissipated in the DBD was below 7 W giving an efficiency of 17 %. The length of the plasma jet was greatly limited to below 1 cm due to the configuration of the DBD system and nozzle.</p> <div class="credits"> <p class="dwt_author">Choo, C. Y.; Chin, O. H.</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-03-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">245</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/50916841"> <span id="translatedtitle">Bond strength evaluation on dental structures after <span class="hlt">non-thermal</span> plasma treatment</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">Summary form only given. This study aims to evaluate the potential of atmospheric pressure <span class="hlt">non-thermal</span> plasma technology (NPT) to enhance the adhesive bond strength on normative dentin substrates. Two different microplasma jets were used in our experiments, a direct-current driven microhollow cathode discharge jet operated in air and a rf-driven jet operated in Ar. Other gas mixtures, e.g. He\\/O2 are</p> <div class="credits"> <p class="dwt_author">N. R. F. A. Silva; L. Martins; P. G. Coelho; V. P. Thompson; Weidong Zhu; K. H. Becker</p> <p class="dwt_publisher"></p> <p class="publishDate">2010-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">246</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=20120012018&hterms=distribution&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D70%26Ntt%3Ddistribution"> <span id="translatedtitle">Determination of <span class="hlt">Non-Thermal</span> Velocity Distributions from SERTS Linewidth Observations</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary"><span class="hlt">Non-thermal</span> velocities obtained from the measurement of coronal Extreme Ultraviolet (EUV) linewidths have been consistently observed in solar EUV spectral observations and have been theorized to result fro m many plausible scenarios including wave motions, turbulence, or magnetic reconnection. Constraining these velocities can provide a physical limit for the available energy resulting from unresolved motions in the corona. We statistically determine a series of <span class="hlt">non-thermal</span> velocity distributions from linewidth measurements of 390 emission lines from a wide array of elements and ionization states observed during the Solar Extreme Ultraviolet Research Telescope and Spectrograph 1991-1997 flights covering the spectral range 174-418 A and a temperature range from 80,000 K to 12.6 MK. This sample includes 248 lines from active regions, 101 lines from quiet-Sun regions, and 41 lines were observed from plasma off the solar limb. We find a strongly peaked distribution corresponding to a <span class="hlt">non-thermal</span> velocity of 19-22 km/s in all three of the quiet-Sun, active region, and off-limb distributions. For the possibility of Alfven wave resonance heating, we find thai velocities in the core of these distributions do not provide sufficient energy, given typical densities and magnetic field strengths for the coronal plasma, to overcome the estimated coronal energy losses required to maintain the corona at the typical temperatures working as the sole mechanism. We find that at perfect efficiency 50%-60% of the needed energy flux can be produced from the <span class="hlt">non-thermal</span> velocities measured.</p> <div class="credits"> <p class="dwt_author">Coyner, Aaron J.; Davila, Joseph M.</p> <p class="dwt_publisher"></p> <p class="publishDate">2011-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">247</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3052910"> <span id="translatedtitle">Near-Infrared Irradiation <span class="hlt">Non-thermally</span> Affects Subcutaneous Adipocytes and Bones</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p class="result-summary">Objective: We previously reported that near-infrared irradiation simulating solar near-infrared with pre- and parallel-irradiational cooling can penetrate the skin and <span class="hlt">non-thermally</span> affects dermis, superficial muscles, and so forth. To clarify the possible effect of NIR irradiation on other subcutaneous tissues, we evaluated how near-infrared <span class="hlt">non-thermally</span> affects subcutaneous adipocytes and bones in rats. Methods: The central back tissues of rats were irradiated with a specialized near-infrared device that simulates solar radiation. The total energy emitted was equivalent to approximately 8.75 hours of sunbathing in North America. Histological evaluation was performed on subcutaneous adipocytes and the spinous process of the near-infrared-irradiated rat and compared with non-irradiated controls. Results: Subcutaneous and bone marrow adipocytes, CD34-positive hematopoietic stem cells in bone marrow, and the cortical bone mass were all significantly increased, whereas the bone marrow cell number was significantly decreased following near-infrared irradiation. Apoptotic cells were detected in the bone marrow at postirradiation days 7 and 30 but were not detected at day 60 or in the controls. Bone marrow cell numbers recovered gradually, whereas the increase in subcutaneous and bone marrow adipocytes, CD34-positive hematopoietic stem cells in bone marrow, and cortical bone mass remained elevated even at day 180. Conclusions: Near-infrared irradiation that simulated solar radiation <span class="hlt">non-thermally</span> affected subcutaneous adipocytes and bones in rats. It induced putative, <span class="hlt">non-thermal</span> damage of bone marrow, which was mediated by apoptosis. However, it increased subcutaneous and bone marrow adipocytes, CD34-positive hematopoietic stem cells in bone marrow, and cortical bone mass.</p> <div class="credits"> <p class="dwt_author">Tanaka, Yohei; Matsuo, Kiyoshi; Yuzuriha, Shunsuke</p> <p class="dwt_publisher"></p> <p class="publishDate">2011-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">248</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.mecheng.osu.edu/netl/files/netl/netl/PSST_paper_ESCAMPIG_2008_published.pdf"> <span id="translatedtitle">Plasma assisted ignition and high-speed flow control: <span class="hlt">non-thermal</span> and thermal effects</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">The paper reviews recent progress in two rapidly developing engineering applications of plasmas, plasma assisted combustion and plasma assisted high-speed flow control. Experimental and kinetic modeling results demonstrate the key role of <span class="hlt">non-thermal</span> plasma chemistry in hydrocarbon ignition by uniform, repetitively pulsed, nanosecond pulse duration, low-temperature plasmas. Ignition delay time in premixed ethylene-air flows excited by the plasma has been</p> <div class="credits"> <p class="dwt_author">I. V. Adamovich; I. Choi; N. Jiang; J.-H. Kim; S. Keshav; W. R. Lempert; E. Mintusov; M. Nishihara; M. Samimy; M. Uddi</p> <p class="dwt_publisher"></p> <p class="publishDate">2009-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">249</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/servlets/purl/6708775"> <span id="translatedtitle">SOLCOST - Version 3. 0. Solar energy design program for <span class="hlt">non-thermal</span> specialists</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">The SOLCOST solar energy design program is a public domain computerized design tool intended for use by <span class="hlt">non-thermal</span> specialists to size solar systems with a methodology based on life cycle cost. An overview of SOLCOST capabilities and options is presented. A detailed guide to the SOLCOST input parameters is included. Sample problems showing typical imput decks and resulting SOLCOST output sheets are given. Details of different parts of the analysis are appended. (MHR)</p> <div class="credits"> <p class="dwt_author">Not Available</p> <p class="dwt_publisher"></p> <p class="publishDate">1980-05-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">250</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/12454466"> <span id="translatedtitle">The symbiotic star CH Cygni - I. <span class="hlt">Non-thermal</span> bipolar jets</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">Very Large Array surface brightness and spectral index maps of the evolving extended emission of the triple symbiotic star CH Cygni are presented. These are derived from observations at 4.8, 8.4 and 14GHz between 1985 and 1999. The maps are dominated by thermal emission around the central bright peak of the nebula, but we also find unambiguous <span class="hlt">non-thermal</span> emission associated</p> <div class="credits"> <p class="dwt_author">M. M. Crocker; R. J. Davis; S. P. S. Eyres; M. F. Bode; A. R. Taylor; A. Skopal; H. T. Kenny</p> <p class="dwt_publisher"></p> <p class="publishDate">2001-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">251</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/40437900"> <span id="translatedtitle">Surface modification and characterizations of basalt fibers with <span class="hlt">non-thermal</span> plasma</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">Atmospheric-pressure <span class="hlt">non-thermal</span> plasmas have been increasingly promoted for polymer surface modification. In this paper, atmospheric-pressure plasmas of oxygen, argon, hydrogen and mixture gases of nitrogen and hydrogen were used to surface modification of basalt fibers in order to illuminate their chemical durability, surface active groups and roughness etc. The plasma-induced surface changes on morphologies and active groups were characterized by</p> <div class="credits"> <p class="dwt_author">G. J. Wang; Y. W. Liu; Y. J. Guo; Z. X. Zhang; M. X. Xu; Z. X. Yang</p> <p class="dwt_publisher"></p> <p class="publishDate">2007-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">252</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/22113484"> <span id="translatedtitle">Dust-acoustic solitary waves in dusty plasmas with <span class="hlt">non-thermal</span> ions</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">Most studies on dusty plasmas have assumed that electrons and ions follow Maxwellian distributions. However, in the presence of energetic ions, the distribution of ions tends to be non-Maxwellian. It is shown here that the existence of <span class="hlt">non-thermal</span> ions would increase the phase velocity of a dust-acoustic wave. It is also found that the change in the phase velocity profoundly affects the characteristics of a dust-acoustic solitary wave.</p> <div class="credits"> <p class="dwt_author">Asgari, H.; Muniandy, S. V.; Wong, C. S. [Plasma Technology Research Center, Department of Physics, University of Malaya, 50603 Kuala Lumpur (Malaysia)</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-02-15</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">253</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=20110010267&hterms=HEV&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D10%26Ntt%3DHEV"> <span id="translatedtitle">The Swift BAT Perspective on <span class="hlt">Non-Thermal</span> Emission in HIFLUGCS Galaxy Clusters</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">The search for diffuse <span class="hlt">non-thermal</span>, inverse Compton (IC) emission from galaxy clusters at hard X-ray energies has been underway for many years, with most detections being either of low significance or controversial. Until recently, comprehensive surveys of hard X-ray emission from clusters were not possible; instead, individually proposed-for. long observations would be collated from the archive. With the advent of the Swift BAT all sky survey, any c1u,;ter's emission above 14 keV can be probed with nearly uniform sensitivity. which is comparable to that of RXTE, Beppo-SAX, and Suzaku with the 58-month version of the survey. In this work. we search for <span class="hlt">non-thermal</span> excess emission above the exponentially decreasing, high energy thermal emission in the flux-limited HIFLUGCS sample. The BAT emission from many of the detected clusters is marginally extended; we are able to extract the total flux for these clusters using fiducial models for their spatial extent. To account for thermal emission at BAT energies, XMM-Newton EPIC spectra are extracted from coincident spatial regions so that both the thermal and <span class="hlt">non-thermal</span> spectral components can be determined simultaneou,;ly in joint fits. We find marginally significant IC components in 6 clusters, though after closer inspection and consideration of systematic errors we are unable to claim a clear detection in any of them. The spectra of all clusters are also summed to enhance a cumulative <span class="hlt">non-thermal</span> signal not quite detectable in individual clusters. After constructing a model based on single temperature</p> <div class="credits"> <p class="dwt_author">Wik, Daniel R.</p> <p class="dwt_publisher"></p> <p class="publishDate">2011-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">254</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2013ApJ...770...26S"> <span id="translatedtitle">Ubiquitous <span class="hlt">Non-thermals</span> in Astrophysical Plasmas: Restating the Difficulty of Maintaining Maxwellians</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">This paper outlines the rather narrow conditions on a radiatively decoupled plasma where a Maxwell-Boltzmann (MB) distribution can be assumed with confidence. The complementary <span class="hlt">non-thermal</span> distribution with non-perturbative kurtosis is argued to have a much broader purview than has previously been accepted. These conditions are expressed in terms of the electron Knudsen number, Ke , the ratio of the electron mean free path to the scale length of electron pressure. Rather generally, f(v < v 2(Ke )) will be Gaussian, so that MB atomic or wave particle effects controlled by speeds v < v 2 ? w(15/8Ke )1/4 will remain defensible, where w is the most probable speed. The sufficient condition for Spitzer-Braginskii plasma fluid closure at the energy equation requires globally Ke (s) <= 0.01; this global condition pertains to the maximum value of Ke along the arc length s of the magnetic field (to its extremities) provided that contiguous plasma remains uncoupled from the radiation field. The <span class="hlt">non-thermal</span> regime Ke > 0.01 is common in all main-sequence stellar atmospheres above approximately 0.05 stellar radii from the surface. The entire solar corona and wind are included in this regime where <span class="hlt">non-thermal</span> distributions with kurtosis are shown to be ubiquitous, heat flux is not well modeled by Spitzer-Braginskii closure, and fluid modeling is qualitative at best.</p> <div class="credits"> <p class="dwt_author">Scudder, J. D.; Karimabadi, H.</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-06-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">255</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2012ASPC..455..199R"> <span id="translatedtitle">The Effects of Including <span class="hlt">Non-Thermal</span> Particles in Flare Loop Models</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">In this work, we use HyLoop (Winter et al. 2011), a loop model that can incorporate the effects of both MHD and <span class="hlt">non-thermal</span> particle populations, to simulate soft X-ray emissions in various situations. First of all, we test the effect of acceleration location on the emission in several XRT filters by simulating a series of post flare loops with different injection points for the <span class="hlt">non-thermal</span> particle beams. We use an injection distribution peaked at the loop apex to represent a direct acceleration model, and an injection distribution peaked at the footpoints to represent the Alfvén wave interaction model. We find that footpoint injection leads to several early peaks in the apex-to-footpoint emission ratio. Second, we model a loop with cusp-shaped geometry based on the eruption model developed byLin & Forbes (2000) and Reeves & Forbes (2005a), and find that early in the flare, emission in the loop footpoints is much brighter in the XRT filters if <span class="hlt">non-thermal</span> particles are included in the calculation. Finally, we employ a multi-loop flare model to simulate thermal emission and compare with a previous model where a semi-circular geometry was used (Reeves et al. 2007). We compare the Geostationary Operational Environmental Satellite (GOES) emission from the two models and find that the cusp-shaped geometry leads to a smaller GOES class flare.</p> <div class="credits"> <p class="dwt_author">Reeves, K. K.; Winter, H. D.; Larson, N. L.</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-05-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">256</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2010AAS...21640710C"> <span id="translatedtitle">Determination Of <span class="hlt">Non-thermal</span> Velocity Distributions From Spatially-averaged EUV Spectra Observed With SERTS And Hinode/EIS</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Unresolved <span class="hlt">non-thermal</span> broadenings have been reported in observations of solar EUV spectra for decades. These unresolved broadenings are generally attributed to <span class="hlt">non-thermal</span> motions within coronal plasma loops and have been shown to provide a limitation on the maximum available energy in the coronal plasma to facilitate coronal heating. Therefore, determining an average <span class="hlt">non-thermal</span> velocity component of the broadening in observed EUV line profiles provides a significant observational constraint for all coronal heating models to address. We have analyzed spatially-averaged spectra from both the Solar EUV Research Telescope and Spectrograph (SERTS) over the EUV bandpass from 170-420 angstroms in a variety of solar conditions, from quiet sun to active region to off-limb data. For each instrument, we construct a <span class="hlt">non-thermal</span> velocity, <Vnth2>, distributions for active region and quiet sun emission lines respectively. We then fit each distribution with a Gaussian to determine the typical unresolved <span class="hlt">non-thermal</span> velocities observed in both quiet sun and active region distributions. Ideally, if no <span class="hlt">non-thermal</span> component exists the distributions would all peak at zero, but in the case of the SERTS observations, we find the distributions peak at velocities between 21-25 km/s regardless of solar activity. Building off of the SERTS analysis, we create similar distributions using spatially-averaged line profiles from Hinode/EIS observations to use the increased spectral resolution of EIS to refine the <span class="hlt">non-thermal</span> velocity constraints determined with SERTS.</p> <div class="credits"> <p class="dwt_author">Coyner, Aaron J.; Davila, J. M.</p> <p class="dwt_publisher"></p> <p class="publishDate">2010-05-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">257</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/22127161"> <span id="translatedtitle">UBIQUITOUS <span class="hlt">NON-THERMALS</span> IN ASTROPHYSICAL PLASMAS: RESTATING THE DIFFICULTY OF MAINTAINING MAXWELLIANS</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">This paper outlines the rather narrow conditions on a radiatively decoupled plasma where a Maxwell-Boltzmann (MB) distribution can be assumed with confidence. The complementary <span class="hlt">non-thermal</span> distribution with non-perturbative kurtosis is argued to have a much broader purview than has previously been accepted. These conditions are expressed in terms of the electron Knudsen number, K{sub e} , the ratio of the electron mean free path to the scale length of electron pressure. Rather generally, f(v < v{sub 2}(K{sub e} )) will be Gaussian, so that MB atomic or wave particle effects controlled by speeds v < v{sub 2} {identical_to} w(15/8K{sub e} ){sup 1/4} will remain defensible, where w is the most probable speed. The sufficient condition for Spitzer-Braginskii plasma fluid closure at the energy equation requires globally K{sub e} (s) {<=} 0.01; this global condition pertains to the maximum value of K{sub e} along the arc length s of the magnetic field (to its extremities) provided that contiguous plasma remains uncoupled from the radiation field. The <span class="hlt">non-thermal</span> regime K{sub e} > 0.01 is common in all main-sequence stellar atmospheres above approximately 0.05 stellar radii from the surface. The entire solar corona and wind are included in this regime where <span class="hlt">non-thermal</span> distributions with kurtosis are shown to be ubiquitous, heat flux is not well modeled by Spitzer-Braginskii closure, and fluid modeling is qualitative at best.</p> <div class="credits"> <p class="dwt_author">Scudder, J. D. [Department of Physics and Astronomy, University of Iowa, Iowa City, IA 54420 (United States); Karimabadi, H., E-mail: jack-scudder@uiowa.edu [SciberQuest, Del Mar, CA 92014 (United States)</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-06-10</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">258</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2010cosp...38.3049B"> <span id="translatedtitle">Thermal and <span class="hlt">non-thermal</span> seed populations and their contribution to coronal shock acceleration</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Charged particle acceleration in coronal and interplanetary CME-driven shocks is currently considered the primary source of large solar energetic particle (SEP) intensities. In large SEP events, the particles accelerated at the shock generate Alfvénic turbulence in the ambient medium, which facilitates particle trapping and repeated shock crossings, thus bootstrapping the acceleration process. In order to study this process, we have developed a Monte Carlo simulation method, where particles are traced in prescribed large-scale electromagnetic fields utilizing the guiding center approximation. In our simulations, particles are scattered in the turbulence according to quasilinear theory, with the scattering amplitude directly proportional to the intensity of Alfvén waves at gyro-resonant wavenumbers. The Alfvén waves are traced simultaneously with the particles, so that the wave field is propagated outwards from the Sun using WKB propagation supplemented with a phenomenological wavenumber diffusion term and a growth rate computed from the net flux of the accelerated particles. In this work, we study how the thermal and the <span class="hlt">non-thermal</span> portions of the acceleration seed population participate in the acceleration process. We model the seed particle population by using a kappa distribution, in order to mimic a thermal bulk plasma supplemented by a <span class="hlt">non-thermal</span> high-energy tail. We will study the contribution of the thermal and <span class="hlt">non-thermal</span> populations to the wave generation, and their participation in the accelerated particle populations, in different phases of the evolution of the SEP event. With this model, we can estimate the requirements for the source population to produce observed solar events.</p> <div class="credits"> <p class="dwt_author">Battarbee, Markus; Vainio, Rami; Laitinen, Timo</p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">259</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3268344"> <span id="translatedtitle"><span class="hlt">Non-thermal</span> Plasma Induces Apoptosis in Melanoma Cells via Production of Intracellular Reactive Oxygen Species</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p class="result-summary"><span class="hlt">Non-thermal</span> atmospheric pressure dielectric barrier discharge (DBD) plasma may provide a novel approach to treat malignancies via induction of apoptosis. The purpose of this study was to evaluate the potential of DBD plasma to induce apoptosis in melanoma cells. Melanoma cells were exposed to plasma at doses that did not induce necrosis, and cell viability and apoptotic activity were evaluated by Trypan blue exclusion test, Annexin-V/PI staining, caspase-3 cleavage, and TUNEL® analysis. Trypan blue staining revealed that <span class="hlt">non-thermal</span> plasma treatment significantly decreased the viability of cells in a dose-dependent manner 3 and 24 h after plasma treatment. Annexin-V/PI staining revealed a significant increase in apoptosis in plasma-treated cells at 24, 48, and 72 h post-treatment (p<0.001). Caspase-3 cleavage was observed 48 h post-plasma treatment at a dose of 15 J/cm2. TUNEL® analysis of plasma-treated cells demonstrated an increase in apoptosis at 48 and 72 h post-treatment (p<0.001) at a dose of 15 J/cm2. Pre-treatment with N-acetyl-L-cysteine (NAC), an intracellular reactive oxygen species (ROS) scavenger, significantly decreased apoptosis in plasma-treated cells at 5 and 15 J/cm2. Plasma treatment induces apoptosis in melanoma cells through a pathway that appears to be dependent on production of intracellular ROS. DBD plasma production of intracellular ROS leads to dose-dependent DNA damage in melanoma cells, detected by ?-H2AX, which was completely abrogated by pre-treating cells with ROS scavenger, NAC. Plasma-induced DNA damage in turn may lead to the observed plasma-induced apoptosis. Since plasma is <span class="hlt">non-thermal</span>, it may be used to selectively treat malignancies.</p> <div class="credits"> <p class="dwt_author">Sensenig, Rachel; Kalghatgi, Sameer; Cerchar, Ekaterina; Fridman, Gregory; Shereshevsky, Alexey; Torabi, Behzad; Arjunan, Krishna Priya; Podolsky, Erica; Fridman, Alexander; Friedman, Gary; Azizkhan-Clifford, Jane; Brooks, Ari D.</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">260</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2013A%26A...551A..37M"> <span id="translatedtitle">Particle acceleration and <span class="hlt">non-thermal</span> emission during the V407 Cygni nova outburst</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Context. On March 2010, the symbiotic binary V407 Cyg erupted as a result of a nova explosion. The event gave rise to a two-week long burst of ? 100 MeV ?-rays detected by Fermi/LAT, a unique observation testifying to particle acceleration in the system. Aims: The outburst can be considered a scaled-down supernova, with short dynamical time scale, and thus can constitute a test case for theories of the origin of Galactic cosmic rays. We aim at determining the properties of the accelerated particles and identifying the origin of the high-energy radiation. Methods: We developed a model for diffusive shock acceleration and <span class="hlt">non-thermal</span> emission in V407 Cyg, complemented by an evaluation of the thermal emission from the shocked plasma. We considered both leptonic and hadronic contributions to the <span class="hlt">non-thermal</span> processes, and investigated the effect of many binary and nova parameters. Results: The ?-ray emission is mostly of leptonic origin and arises predominantly from inverse-Compton scattering of the nova light. Matching the light curve requires gas accumulation in the vicinity of the white dwarf, as a consequence of wind accretion, while the spectrum imposes particle scattering close to the Bohm limit in the upstream equipartition magnetic field. The nova accelerated protons (respectively electrons) with energies up to ?300 GeV (respectively ?20 GeV), for a total <span class="hlt">non-thermal</span> energy ?10 erg after two weeks, representing ?10% of the initial nova kinetic energy. The electron-to-proton ratio at injection is 6%. Conclusions: The V407 Cyg eruption can be understood from the same principles that are invoked for particle acceleration in supernova remnants, although without the need for strong magnetic field amplification. The population of novae in symbiotic systems is a negligible source of Galactic cosmic rays, and most likely not a class of TeV-emitters.</p> <div class="credits"> <p class="dwt_author">Martin, P.; Dubus, G.</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-03-01</p> </div> </div> </div> </div> <div id="filter_results_form" class="filter_results_form floatContainer" style="visibility: visible;"> <div style="width:100%" id="PaginatedNavigation" class="paginatedNavigationElement"> <a id="FirstPageLink" onclick='return showDiv("page_1");' href="#" title="First Page"> <img id="FirstPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.first.18x20.png" alt="First Page" /></a> <a id="PreviousPageLink" onclick='return showDiv("page_12");' href="#" title="Previous Page"> <img id="PreviousPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.previous.18x20.png" alt="Previous Page" /></a> <span id="PageLinks" class="pageLinks"> <span> <a 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showDiv("page_15");' href="#" title="Next Page"> <img id="NextPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.next.18x20.png" alt="Next Page" /></a> <a id="LastPageLink" onclick='return showDiv("page_25.0");' href="#" title="Last Page"> <img id="LastPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.last.18x20.png" alt="Last Page" /></a> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">261</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2010PhDT.......342B"> <span id="translatedtitle">Magnetic fields in galaxy clusters: Faraday rotation and <span class="hlt">non</span> <span class="hlt">thermal</span> emission</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">In this thesis we study the magnetic field in galaxy clusters and their connection with thermal and <span class="hlt">non-thermal</span> phenomena in the Intra Cluster Medium. These topics are investigated through the analysis of the polarization properties of sources located behind and inside galaxy clusters as well as through MHD cosmological simulation. To this aim we have obtained observations at the Very Large Array (VLA) radio telescope (New Mexico USA) and we have investigated the magnetic field properties through different methods. We used the numerical code Faraday to interpret our results. We also used the brand new implementation within the Gadget3 code to investigate the properties of massive simulated galaxy clusters.</p> <div class="credits"> <p class="dwt_author">Bonafede, Annalisa</p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">262</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/15016925"> <span id="translatedtitle">Lean NOx Reduction in Two Stages: <span class="hlt">Non-thermal</span> Plasma Followed by Heterogeneous Catalysis</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">We present data in this paper showing that <span class="hlt">non-thermal</span> plasma in combination with heterogeneous catalysis is a promising technique for the treatment of NOx in diesel exhaust. Using a commonly available zeolite catalyst, sodium Y, to treat synthetic diesel exhaust we report approximately 50% chemical reduction of NOx over a broad, representative temperature range. We have measured the overall efficiency as a function of the temperature and hydrocarbon concentration. The direct detection of N2 and N2O when the background gas is replaced by helium confirms that true chemical reduction is occurring.</p> <div class="credits"> <p class="dwt_author">Tonkyn, Russell G.; Yoon, Ilsop S.; Barlow, Stephan E.; Panov, Alexander G.; Kolwaite, A; Balmer, Mari LOU.</p> <p class="dwt_publisher"></p> <p class="publishDate">2000-10-16</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">263</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/doepatents/biblio/972295"> <span id="translatedtitle">Field-enhanced electrodes for additive-injection <span class="hlt">non-thermal</span> plasma (NTP) processor</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/doepatents">DOEpatents</a></p> <p class="result-summary">The present invention comprises a field enhanced electrode package for use in a <span class="hlt">non-thermal</span> plasma processor. The field enhanced electrode package includes a high voltage electrode and a field-enhancing electrode with a dielectric material layer disposed in-between the high voltage electrode and the field-enhancing electrode. The field-enhancing electrode features at least one raised section that includes at least one injection hole that allows plasma discharge streamers to occur primarily within an injected additive gas.</p> <div class="credits"> <p class="dwt_author">Rosocha, Louis A. (Los Alamos, NM); Ferreri, Vincent (Westminster, CO); Kim, Yongho (Los Alamos, NM)</p> <p class="dwt_publisher"></p> <p class="publishDate">2009-04-21</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">264</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2002JPlPh..67..199R"> <span id="translatedtitle">Arbitrary-amplitude solitary kinetic Alfvén waves in a <span class="hlt">non-thermal</span> plasma</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">An exact Sagdeev equation for arbitrary-amplitude solitary kinetic Alfvén waves in a <span class="hlt">non-thermal</span> plasma is derived. For small [beta][prime prime or minute], the proportion of fast electrons, an analytical expression for the exact pseudopotential V ([phi]) is obtained. For several values of [beta][prime prime or minute], the Sagdeev potential V ([phi]) has been calculated by integrating the Sagdeev equation. It is found that, depending on the values of [beta][prime prime or minute], both hump and dip solitons exist.</p> <div class="credits"> <p class="dwt_author">Roychoudhury, Rajkumar</p> <p class="dwt_publisher"></p> <p class="publishDate">2002-04-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">265</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/servlets/purl/900188"> <span id="translatedtitle">Removal of Elemental Mercury from a Gas Stream Facilitated by a <span class="hlt">Non-Thermal</span> Plasma Device</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">Mercury generated from anthropogenic sources presents a difficult environmental problem. In comparison to other toxic metals, mercury has a low vaporization temperature. Mercury and mercury compounds are highly toxic, and organic forms such as methyl mercury can be bio-accumulated. Exposure pathways include inhalation and transport to surface waters. Mercury poisoning can result in both acute and chronic effects. Most commonly, chronic exposure to mercury vapor affects the central nervous system and brain, resulting in neurological damage. The CRE technology employs a series of <span class="hlt">non-thermal</span>, plasma-jet devices to provide a method for elemental mercury removal from a gas phase by targeting relevant chemical reactions. The technology couples the known chemistry of converting elemental mercury to ionic compounds by mercury-chlorine-oxygen reactions with the generation of highly reactive species in a <span class="hlt">non-thermal</span>, atmospheric, plasma device. The generation of highly reactive metastable species in a <span class="hlt">non-thermal</span> plasma device is well known. The introduction of plasma using a jet-injection device provides a means to contact highly reactive species with elemental mercury in a manner to overcome the kinetic and mass-transfer limitations encountered by previous researchers. To demonstrate this technology, WRI has constructed a plasma test facility that includes plasma reactors capable of using up to four plasma jets, flow control instrumentation, an integrated control panel to operate the facility, a mercury generation system that employs a temperature controlled oven and permeation tube, combustible and mercury gas analyzers, and a ductless fume hood designed to capture fugitive mercury emissions. Continental Research and Engineering (CR&E) and Western Research Institute (WRI) successfully demonstrated that <span class="hlt">non-thermal</span> plasma containing oxygen and chlorine-oxygen reagents could completely convert elemental mercury to an ionic form. These results demonstrate potential the application of this technology for removing elemental mercury from flue gas streams generated by utility boilers. On an absolute basis, the quantity of reagent required to accomplish the oxidation was small. For example, complete oxidation of mercury was accomplished using a 1% volume fraction of oxygen in a nitrogen stream. Overall, the tests with mercury validated the most useful aspect of the CR&E technology: Providing a method for elemental mercury removal from a gas phase by employing a specific plasma reagent to either increase reaction kinetics or promote reactions that would not have occurred under normal circumstances.</p> <div class="credits"> <p class="dwt_author">Charles Mones</p> <p class="dwt_publisher"></p> <p class="publishDate">2006-12-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">266</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2014JAP...115v3304F"> <span id="translatedtitle">Stabilization of a lean premixed flame using <span class="hlt">non-thermal</span> plasma</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">This study experimentally investigates the effect of <span class="hlt">non-thermal</span> plasma (NTP) on the stabilization of a lean premixed methane/air flame. The equivalence ratio of the methane/air mixture for the lean blowout limit (?CH4?0.81) decreases to 0.79 when the fuel is strongly exposed to NTP. Both the flame temperature and the luminescence intensity of C2, CH, and OH radicals increase with increasing applied voltage, resulting in an increase in flame intensity. This allows the lean blowout limit of the methane/air mixture to be extended.</p> <div class="credits"> <p class="dwt_author">Fukuda, Daisuke; Shinjo, Ryosuke; Okamoto, Toshiya; Gotoda, Hiroshi</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-06-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">267</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/22140151"> <span id="translatedtitle">ON THE NATURE OF THE mHz X-RAY <span class="hlt">QUASI-PERIODIC</span> OSCILLATIONS FROM ULTRALUMINOUS X-RAY SOURCE M82 X-1: SEARCH FOR TIMING-SPECTRAL CORRELATIONS</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">Using all the archival XMM-Newton X-ray (3-10 keV) observations of the ultraluminous X-ray source (ULX) M82 X-1, we searched for a correlation between its variable mHz <span class="hlt">quasi-periodic</span> oscillation (QPO) frequency and its hardness ratio (5-10 keV/3-5 keV), an indicator of the energy spectral power-law index. When stellar-mass black holes (StMBHs) exhibit type-C low-frequency QPOs ({approx}0.2-15 Hz), the centroid frequency of the QPO is known to correlate with the energy spectral index. The detection of such a correlation would strengthen the identification of M82 X-1's mHz QPOs as type-C and enable a more reliable mass estimate by scaling its QPO frequencies to those of type-C QPOs in StMBHs of known mass. We resolved the count rates and the hardness ratios of M82 X-1 and a nearby bright ULX (source 5/X42.3+59) through surface brightness modeling. We detected QPOs in the frequency range of 36-210 mHz during which M82 X-1's hardness ratio varied from 0.42 to 0.47. Our primary results are (1) that we do not detect any correlation between the mHz QPO frequency and the hardness ratio (a substitute for the energy spectral power-law index) and (2) similar to some accreting X-ray binaries, we find that M82 X-1's mHz QPO frequency increases with its X-ray count rate (Pearson's correlation coefficient = +0.97). The apparent lack of a correlation between the QPO centroid frequency and the hardness ratio poses a challenge to the earlier claims that the mHz QPOs of M82 X-1 are the analogs of the type-C low-frequency QPOs of StMBHs. On the other hand, it is possible that the observed relation between the hardness ratio and the QPO frequency represents the saturated portion of the correlation seen in type-C QPOs of StMBHs-in which case M82 X-1's mHz QPOs can still be analogous to type-C QPOs.</p> <div class="credits"> <p class="dwt_author">Pasham, Dheeraj R. [Astronomy Department, University of Maryland, College Park, MD 20742 (United States); Strohmayer, Tod E., E-mail: dheeraj@astro.umd.edu, E-mail: tod.strohmayer@nasa.gov [Astrophysics Science Division, NASA's Goddard Space Flight Center, Greenbelt, MD 20771 (United States)</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-07-10</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">268</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3491894"> <span id="translatedtitle"><span class="hlt">Non-thermal</span> Plasma Causes p53-Dependent Apoptosis in Human Colon Carcinoma Cells</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p class="result-summary"><span class="hlt">Non-thermal</span> plasma (NTP) consists of a huge amount of biologically active particles, whereas its temperature is close to ambient. This combination allows one to use NTP as a perspective tool for solving different biomedical tasks, including antitumor therapy. The treatment of tumor cells with NTP caused dose-dependent effects, such as growth arrest and apoptosis. However, while the outcome of NTP treatment has been established, the molecular mechanisms of the interaction between NTP and eukaryotic cells have not been thoroughly studied thus far. In this work, the mechanisms and the type of death of human colon carcinoma HCT 116 cells upon application of <span class="hlt">non-thermal</span> argon plasma were studied. The effect of NTP on the major stress-activated protein p53 was investigated. The results demonstrate that the viability of HCT116 cells upon plasma treatment is dependent on the functional p53 protein. NTP treatment caused an increase in the intracellular concentration of p53 and the induction of the p53-controlled regulon. The p53-dependent accumulation of active proapoptotic caspase-3 was shown in NTP-treated cells. The study was the first to demonstrate that treatment of human colon carcinoma cells with NTP results in p53-dependent apoptosis. The results obtained contribute to our understanding of the applicability of NTP in antitumor therapy.</p> <div class="credits"> <p class="dwt_author">Tuhvatulin, A.I.; Sysolyatina, E.V.; Scheblyakov, D.V.; Logunov, D.Yu.; Vasiliev, M.M.; Yurova, M.A.; Danilova, M.A.; Petrov, O.F.; Naroditsky, B.S.; Morfill, G.E.; Grigoriev, A.I.; Fortov, V.E.; Gintsburg, A.L.; Ermolaeva, S.A.</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">269</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/22717524"> <span id="translatedtitle">Evaluation of thermal and <span class="hlt">non-thermal</span> effects of UHF RFID exposure on biological drugs.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">The Radio Frequency Identification (RFID) technology promises to improve several processes in the healthcare scenario, especially those related to traceability of people and things. Unfortunately, there are still some barriers limiting the large-scale deployment of these innovative technologies in the healthcare field. Among these, the evaluation of potential thermal and <span class="hlt">non-thermal</span> effects due to the exposure of biopharmaceutical products to electromagnetic fields is very challenging, but still slightly investigated. This paper aims to setup a controlled RF exposure environment, in order to reproduce a worst-case exposure of pharmaceutical products to the electromagnetic fields generated by the UHF RFID devices placed along the supply chain. Radiated powers several times higher than recommended by current normative limits were applied (10 W and 20 W). The electric field strength at the exposed sample location, used in tests, was as high as 100 V/m. <span class="hlt">Non-thermal</span> effects were evaluated by chromatography techniques and in vitro assays. The results obtained for a particular case study, the ActrapidTM human insulin preparation, showed temperature increases lower than 0.5 °C and no significant changes in the structure and performance of the considered drug. PMID:22717524</p> <div class="credits"> <p class="dwt_author">Calcagnini, Giovanni; Censi, Federica; Maffia, Michele; Mainetti, Luca; Mattei, Eugenio; Patrono, Luigi; Urso, Emanuela</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-11-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">270</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2008cihw.conf..187R"> <span id="translatedtitle">Clumping effects on <span class="hlt">non-thermal</span> particle spectra in massive star systems</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Observational evidence exists that winds of massive stars are clumped. Many massive star systems are known as <span class="hlt">non-thermal</span> particle production sites, as indicated by their synchrotron emission in the radio band. As a consequence they are also considered as candidate sites for <span class="hlt">non-thermal</span> high-energy photon production up to gamma-ray energies. The present work considers the effects of wind clumpiness expected on the emitting relativistic particle spectrum in colliding wind systems, built up from the pool of thermal wind particles through diffusive particle acceleration, and taking into account inverse Compton and synchrotron losses. In comparison to a homogeneous wind, a clumpy wind causes flux variations of the emitting particle spectrum when the clump enters the wind collision region. It is found that the spectral features associated with this variability moves temporally from low to high energy bands with the time shift between any two spectral bands being dependent on clump size, filling factor, and the energy-dependence of particle energy gains and losses.</p> <div class="credits"> <p class="dwt_author">Reimer, A.</p> <p class="dwt_publisher"></p> <p class="publishDate">2008-04-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">271</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/20167347"> <span id="translatedtitle">Degradation of volatile organic compounds in a <span class="hlt">non-thermal</span> plasma air purifier.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">The degradation of volatile organic compounds in a commercially available <span class="hlt">non-thermal</span> plasma based air purifying system was investigated. Several studies exist that interrogate the degradation of VOCs in closed air systems using a <span class="hlt">non-thermal</span> plasma combined with a heterogeneous catalyst. For the first time, however, our study was performed under realistic conditions (normal indoor air, 297.5K and 12.5 g m(-3) water content) on an open system, in the absence of an auxiliary catalyst, and using standard operating air flow rates (up to 320 L min(-1)). Cyclohexene, benzene, toluene, ethylbenzene and the xylene isomers were nebulized and guided through the plasma air purifier. The degradation products were trapped by activated charcoal tubes or silica gel tubes, and analyzed using gas chromatography mass spectrometry. Degradation efficiencies of 11+/-1.6% for cyclohexene, <2% for benzene, 11+/-2.4% for toluene, 3+/-1% for ethylbenzene, 1+/-1% for sigma-xylene, and 3+/-0.4% for m-/rho-xylene were found. A fairly wide range of degradation products could be identified. On both trapping media, various oxidized species such as alcohols, aldehydes, ketones and one epoxide were observed. The formation of adipaldehyde from nebulized cyclohexene clearly indicates an ozonolysis reaction. Other degradation products observed suggests reactions with OH radicals. We propose that mostly ozone and OH radicals are responsible for the degradation of organic molecules in the plasma air purifier. PMID:20167347</p> <div class="credits"> <p class="dwt_author">Schmid, Stefan; Jecklin, Matthias C; Zenobi, Renato</p> <p class="dwt_publisher"></p> <p class="publishDate">2010-03-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">272</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/servlets/purl/10158017"> <span id="translatedtitle">Preradiation studies for <span class="hlt">non-thermal</span> Z-pinch wire load experiments on Saturn</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">The implosion dynamics of compact wire arrays on Saturn are explored as a function of wire mass m, wire length {ell}, wire radii R, and radial power-flow feed geometry using the ZORK code. Electron losses and the likelihood of arcing in the radial feed adjacent the wire load are analyzed using the TWOQUICK and CYLTRAN codes. The physical characteristics of the implosion and subsequent thermal radiation production are estimated using the LASNEX code in one dimension. These analyses show that compact tungsten wire arrays with parameters suggested by D. Mosher and with a 21-nH vacuum feed geometry satisfy the empirical scaling criterion I/(M/{ell}) {approximately} 2 MA/(mg/cm) of Mosher for optimizing <span class="hlt">non-thermal</span> radiation from z pinches, generate low electron losses in the radial feeds, and generate electric fields at the insulator stack below the Charlie Martin flashover limit thereby permitting full power to be delivered to the load. Under such conditions, peak currents of {approximately}5 MA can be delivered to wire loads {approximately}20 ns before the driving voltage reverses at the insulator stack, potentially allowing the m = 0 instability to develop with the subsequent emission of <span class="hlt">non-thermal</span> radiation as predicted by the Mosher model.</p> <div class="credits"> <p class="dwt_author">Sanford, T.W.L.; Humphreys, D.R.; Poukey, J.W.; Marder, B.M.; Halbleib, J.A.; Crow, J.T.; Spielman, R.B. [Sandia National Labs., Albuquerque, NM (United States); Mock, R.C. [Ktech Corp., Albuquerque, NM (United States)</p> <p class="dwt_publisher"></p> <p class="publishDate">1994-06-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">273</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/1034230"> <span id="translatedtitle">Thermal and <span class="hlt">Non-thermal</span> Physiochemical Processes in Nanoscale Films of Amorphous Solid Water</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">Amorphous solid water (ASW) is a metastable form of water created by vapor deposition onto a cold substrate (typically less than 130 K). Since this unusual form of water only exists on earth in laboratories with highly specialized equipment, it is fair to ask why there is any interest in studying this esoteric material. Much of the scientific interest involves using ASW as a model system to explore the physical and reactive properties of liquid water and aqueous solutions. Other researchers are interested in ASW because it is believed to be the predominate form of water in the extreme cold temperatures found in many astrophysical and planetary environments. In addition, ASW is a convenient model system for studying the stability of metastable systems (glasses) and the properties of highly porous materials. A fundamental understanding of such properties has applications in a diverse range of disciplines including cryobiology, food science, pharmaceuticals, astrophysics and nuclear waste storage among others.There exist several excellent reviews on the properties of ASW and supercooled liquid water and a new comprehensive review is beyond the scope of this Account. Instead, we focus on our research over the past 15 years using molecular beams and surface science techniques to probe the thermal and <span class="hlt">non</span> <span class="hlt">thermal</span> properties of nanoscale films of ASW. We use molecular beams to precisely control the deposition conditions (flux, incident, energy, incident angle) to create compositionally-tailored, nanoscale films of ASW at low temperatures. To study the transport properties (viscosity, diffusivity), the amorphous films can be heated above their glass transition temperatures, Tg, at which time they transform into deeply supercooled liquids prior to crystallization. The advantage of this approach is that at temperatures near Tg the viscosity is approximately 15 orders of magnitude larger than a normal liquid, and therefore the crystallization kinetics are dramatically slowed, increasing the time available for experiments. For example, near Tg, on a typical laboratory time scale (e.g. {approx}1000 s), a water molecule moves less than a molecular distance. For this reason, nanoscale films help to probe the behavior and reactions of supercooled liquid at these low temperatures. ASW films can be used for investigating the <span class="hlt">non-thermal</span> reactions relevant to radiolysis. In this account we will present a survey of our research on the thermal and <span class="hlt">non</span> <span class="hlt">thermal</span> properties of ASW using this approach.</p> <div class="credits"> <p class="dwt_author">Smith, R. Scott; Petrik, Nikolay G.; Kimmel, Gregory A.; Kay, Bruce D.</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-01-17</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">274</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2009PSST...18c4018A"> <span id="translatedtitle">Plasma assisted ignition and high-speed flow control: <span class="hlt">non-thermal</span> and thermal effects</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">The paper reviews recent progress in two rapidly developing engineering applications of plasmas, plasma assisted combustion and plasma assisted high-speed flow control. Experimental and kinetic modeling results demonstrate the key role of <span class="hlt">non-thermal</span> plasma chemistry in hydrocarbon ignition by uniform, repetitively pulsed, nanosecond pulse duration, low-temperature plasmas. Ignition delay time in premixed ethylene-air flows excited by the plasma has been measured in a wide range of pulse repetition rates and equivalence ratios and compared with kinetic modeling calculations, showing good agreement. Comparing ignition delay time predicted by the model for plasma assisted ignition and for ignition by equilibrium heating demonstrated that chain reactions of radicals generated by the plasma reduce ignition time by up to two orders of magnitude and ignition temperature by up to 300 K. These results provide additional evidence of the <span class="hlt">non-thermal</span> nature of low-temperature plasma assisted ignition. Experiments and flow modeling show that the dominant mechanism of high-speed plasma flow control is thermal, due to heating of the flow by the plasma. Development and characterization of pulsed dc and pulsed RF localized arc filament plasma actuator arrays for control of high-speed atmospheric pressure jet flows are discussed. Actuator power is quite low, ~10 W at 10% duty cycle. Plasma emission spectra show that a greater fraction of the pulsed RF discharge power goes to heat the flow (up to 2500 °C), while a significant fraction of the pulsed dc discharge power is spent on electrode and wall heating, resulting in their erosion. Rapid localized heating of the flow by the pulsed arc filaments, at a rate of ~1000 K/10 µs, results in the formation of strong compression/shock waves, detected by schlieren imaging. Effect of flow forcing by repetitively pulsed RF actuators is demonstrated in a M = 1.3 axisymmetric jet. These two case studies provide illustrative examples of isolating <span class="hlt">non-thermal</span> (non-equilibrium plasma chemistry) and thermal (Joule heating) effects in plasmas and adapting them to develop efficient large-volume plasma igniters and high-speed flow actuators.</p> <div class="credits"> <p class="dwt_author">Adamovich, I. V.; Choi, I.; Jiang, N.; Kim, J.-H.; Keshav, S.; Lempert, W. R.; Mintusov, E.; Nishihara, M.; Samimy, M.; Uddi, M.</p> <p class="dwt_publisher"></p> <p class="publishDate">2009-08-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">275</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2010ChPhL..27h9701Y"> <span id="translatedtitle">Multiband <span class="hlt">Non-Thermal</span> Radiation from the Crab Nebula and the Pulsar Wind Nebula in MSH 15-52</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">We study the multiband <span class="hlt">non-thermal</span> emission from two pulsar wind nebulae (PWNe), the Crab nebula and the PWN in MSH 15-52. Both of them have been recently detected by the Fermi large area telescope (LAT) and powered by central gamma-ray pulsars. Motivated by the Fermi LAT results, we use a simplified time-dependent injection model to study the <span class="hlt">non-thermal</span> emission from radio to very high energy gamma-ray radiation from these two sources. In this model, the relativistic electrons are accelerated in pulsar magnetosphere and at pulsar wind termination shocks and can be described by a broken power law. Those high energy particles evolve with time and produce <span class="hlt">non-thermal</span> emission through synchrotron radiation and inverse Compton scattering of soft photons. For Crab nebula, using the GeV emission from 100 MeV to 10 GeV given by Fermi LAT, we can constrain the maximum energy of the electrons and other parameters. The <span class="hlt">non-thermal</span> emission can be well explained by this model. We also use this model to explain the <span class="hlt">non-thermal</span> emission from the PWN in MSH 15-52.</p> <div class="credits"> <p class="dwt_author">Yu, Huan; Jiang, Ze-Jun</p> <p class="dwt_publisher"></p> <p class="publishDate">2010-08-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">276</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2013PhDT.......149R"> <span id="translatedtitle"><span class="hlt">Non-thermal</span> effects of 94 GHz radiation on bacterial metabolism</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Bacillus subtilis, Escherichia coli, Staphylococcus aureus, and Klebsiella pneumoniae were used to investigate the <span class="hlt">non-thermal</span> effects of terahertz (THz) radiation exposure on bacterial cells. The THz source used was a 94 GHz (0.94 THz) Millitech Gunn Diode Oscillator with a power density of 1.3 mW/cm2. The cultures were placed in the middle sixty wells of two 96-well microplates, one serving as the experimental plate and one serving as a control. The experimental plate was placed on the radiation source for either two, eighteen, or twenty-four hours and the metabolism of the cells was measured in a spectrophotometer using the tetrazolium dye XTT. The results showed no consistent significant differences in either the growth rates or the metabolism of any of the bacterial species at this frequency and power density.</p> <div class="credits"> <p class="dwt_author">Raitt, Brittany J.</p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">277</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2012EL.....9730001T"> <span id="translatedtitle">Generalized elastic model: Thermal vs. <span class="hlt">non-thermal</span> initial conditions —Universal scaling, roughening, ageing and ergodicity</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">We study correlation properties of the generalized elastic model which accounts for the dynamics of polymers, membranes, surfaces and fluctuating interfaces, among others. We develop a theoretical framework which leads to the emergence of universal scaling laws for systems starting from thermal (equilibrium) or <span class="hlt">non-thermal</span> (non-equilibrium) initial conditions. Our analysis incorporates and broadens previous results such as observables' double scaling regimes, (super)roughening and anomalous diffusion, and furnishes a new scaling behavior for correlation functions at small times (long distances). We discuss ageing and ergodic properties of the generalized elastic model in non-equilibrium conditions, providing a comparison with the situation occurring in continuous time random walk. Our analysis also allows to assess which observable is able to distinguish whether the system is in or far from equilibrium conditions in an experimental set-up.</p> <div class="credits"> <p class="dwt_author">Taloni, A.; Chechkin, A.; Klafter, J.</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-02-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">278</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3812656"> <span id="translatedtitle">The Effect of Blood Flow on Magnetic Resonance Imaging of <span class="hlt">Non</span> <span class="hlt">Thermal</span> Irreversible Electroporation</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p class="result-summary">To generate an understanding of the physiological significance of MR images of <span class="hlt">Non-Thermal</span> Irreversible Electroporation (NTIRE) we compared the following MR imaging sequences: T1W, T2W, PD, GE, and T2 SPAIR acquired after NTIRE treatment in a rodent liver model. The parameters that were studied included the presence or absence of a Gd-based contrast agent, and in vivo and ex-vivo NTIRE treatments in the same liver. NTIRE is a new minimally invasive tissue ablation modality in which pulsed electric fields cause molecularly selective cell death while, the extracellular matrix and large blood vessels remain patent. This attribute of NTIRE is of major clinical importance as it allows treatment of undesirable tissues near critical blood vessels. The presented study results suggest that MR images acquired following NTIRE treatment are all directly related to the unique pattern of blood flow after NTIRE treatment and are not produced in the absence of blood flow.</p> <div class="credits"> <p class="dwt_author">Hjouj, Mohammad; Lavee, Jacob; Last, David; Guez, David; Daniels, Dianne; Sharabi, Shirley; Rubinsky, Boris; Mardor, Yael</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">279</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2011APS..GECQR1008M"> <span id="translatedtitle">Disinfection of Staphylococcus Aureus by pulsed <span class="hlt">non-thermal</span> atmospheric plasma jet</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">The aim of this paper was to study the effect of low-temperature atmospheric plasma jet on non-pathogenic bacteria's colonies. In this regard, Germicidal effect of time and distance of ICP He and He/N2 plasma jet on Staphylococcus Aureus were reported. The gas discharges were generated by a 40 KHz high voltage power supply which led to the inductively coupled plasma. The results showed that He/N2 enhance the sterilization time in comparison of He plasma. To the best of our knowledge this is the first study which has compared the effect of sterilization of ICP Helium and Helium-Nitrogen plasma in listed conditions. Also, the distance dependence showed that the germicidal effect was not linear the distance of electrode and sample. The protein leakage test and SEM of bacteria morphology confirmed the sterilization effect of <span class="hlt">non-thermal</span> atmospheric pressure plasma jet.</p> <div class="credits"> <p class="dwt_author">Mirpour, Shahriar; Ghoranneviss, Mahmood; Shahgoli, Farhad</p> <p class="dwt_publisher"></p> <p class="publishDate">2011-11-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">280</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2013PhDT.......183L"> <span id="translatedtitle"><span class="hlt">Non-thermal</span> emission in astrophysical environments: From pulsars to supernova remnants</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">The study of electromagnetic radiation from distant astrophysical objects provides essential data in understanding physics of these sources. In particular, <span class="hlt">non-thermal</span> radiation provides great insight into the properties of local environments, particle populations, and emission mechanisms, knowledge which otherwise would remain untapped. Throughout the projects conducted for this dissertation, we modeled certain aspects of observed <span class="hlt">non-thermal</span> emission from three classes of sources: radio pulsars, pulsar wind nebulae, and supernova remnants. Orbital variation in the double pulsar system PSR J0737-3039A/B can be used to probe the details of the magnetospheric structure of pulsar B. Strongly magnetized wind from pulsar A distorts the magnetosphere of pulsar B in a way similar to the solar wind's distortion of the Earth's magnetosphere. Using the two complimentary models of pulsar B's magnetosphere, adapted from the Earth's magnetosphere models by Dungey and Tsyganenko, we determine the precise location of the coherent radio emission generation region in pulsar B's magnetosphere. This analysis is complemented by modeling the observed evolution of the pulse profiles of B due to geodetic precession. The emission region is located at about 3750 stellar radii and has a horseshoe-like shape centered on the polar magnetic field lines. The best fit angular parameters of the emission region indicate that radio emission is generated on the field lines which, according to the theoretical models, originate close to the poles and carry the maximum current. When considered together, not only do the results of the two models converge, they can explain why the modulation of B's radio emission at A's period is observed only within a certain orbital phase region. We discuss the implications of these results for pulsar magnetospheric models and mechanisms of coherent radio emission generation. We also developed a spatially-resolved, analytic model for the high-energy <span class="hlt">non-thermal</span> emission from pulsar wind nebulae (PWNe). Theoretically, synchrotron cooling should cause a gradual change in particle spectrum downstream. This effect is indeed observed in the X-ray spectra of The Crab Nebula , 3C 58, and G21.5.0.9. However, current theoretical models of PWNe that only account for the bulk motion in the pulsar outflow overestimate the steepening of the resulted emission spectrum. This implies that there is an additional mechanism of particle transport which would supply energetic particles to the outer layers of the PWN. Our model solves the lack of high-energy electrons in the outer regions of the nebula by taking the diffusion of particles into account. The resulting multi-wavelength spectra exhibits multiple breaks, which is in agreement with observations. Thin <span class="hlt">non-thermal</span> X-ray filaments are often seen near shock fronts in young supernova remnants (SNRs), often spatially coincident with the high energy gamma-ray emission. The formation of such discrete features is likely influenced by the combined effects of radiative cooling, advection, and diffusion. Spatially-resolved spectral studies of the filaments may, therefore, provide significant insights into the relative importance of main physical processes involved in young SNRs. Using 1 Ms Chandra observation of Cassiopeia A, we perform advection-diffusion modeling of synchrotron emission of filaments to measure the magnetic field, shock obliquity, the diffusion strength and the plasma turbulence level.</p> <div class="credits"> <p class="dwt_author">Lomiashvili, David</p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div id="filter_results_form" class="filter_results_form floatContainer" style="visibility: visible;"> <div style="width:100%" id="PaginatedNavigation" class="paginatedNavigationElement"> <a id="FirstPageLink" onclick='return showDiv("page_1");' href="#" title="First Page"> <img id="FirstPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.first.18x20.png" alt="First Page" /></a> <a id="PreviousPageLink" onclick='return showDiv("page_13");' href="#" title="Previous Page"> <img id="PreviousPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.previous.18x20.png" 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showDiv("page_25");' href="#">25</a> </span> </span> <a id="NextPageLink" onclick='return showDiv("page_16");' href="#" title="Next Page"> <img id="NextPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.next.18x20.png" alt="Next Page" /></a> <a id="LastPageLink" onclick='return showDiv("page_25.0");' href="#" title="Last Page"> <img id="LastPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.last.18x20.png" alt="Last Page" /></a> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">281</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2013NatSR...3E3088H"> <span id="translatedtitle">The Effect of Blood Flow on Magnetic Resonance Imaging of <span class="hlt">Non</span> <span class="hlt">Thermal</span> Irreversible Electroporation</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">To generate an understanding of the physiological significance of MR images of <span class="hlt">Non-Thermal</span> Irreversible Electroporation (NTIRE) we compared the following MR imaging sequences: T1W, T2W, PD, GE, and T2 SPAIR acquired after NTIRE treatment in a rodent liver model. The parameters that were studied included the presence or absence of a Gd-based contrast agent, and in vivo and ex-vivo NTIRE treatments in the same liver. NTIRE is a new minimally invasive tissue ablation modality in which pulsed electric fields cause molecularly selective cell death while, the extracellular matrix and large blood vessels remain patent. This attribute of NTIRE is of major clinical importance as it allows treatment of undesirable tissues near critical blood vessels. The presented study results suggest that MR images acquired following NTIRE treatment are all directly related to the unique pattern of blood flow after NTIRE treatment and are not produced in the absence of blood flow.</p> <div class="credits"> <p class="dwt_author">Hjouj, Mohammad; Lavee, Jacob; Last, David; Guez, David; Daniels, Dianne; Sharabi, Shirley; Rubinsky, Boris; Mardor, Yael</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-10-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">282</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/23513444"> <span id="translatedtitle">Decomposition of trifluoromethane in a dielectric barrier discharge <span class="hlt">non-thermal</span> plasma reactor.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">The decomposition of trifluoromethane (CHF3) was carried out using <span class="hlt">non-thermal</span> plasma generated in a dielectric barrier discharge (DBD) reactor. The effects of reactor temperature, electric power, initial concentration and oxygen content were examined. The DBD reactor was able to completely destroy CHF3 with alumina beads as a packing material. The decomposition efficiency increased with increasing electric power and reactor temperature. The destruction of CHF3 gradually increased with the addition of O2 up to 2%, but further increase in the oxygen content led to a decrease in the decomposition efficiency. The degradation pathways were explained with the identified by-products. The main by-products from CHF3 were found to be COF2, CF4, CO2 and CO although the COF2 and CF4 disappeared when the plasma were combined with alumina catalyst. PMID:23513444</p> <div class="credits"> <p class="dwt_author">Gandhi, M Sanjeeva; Mok, Y S</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">283</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2013PlST...15..439L"> <span id="translatedtitle">Sterilization of Staphylococcus Aureus by an Atmospheric <span class="hlt">Non-Thermal</span> Plasma Jet</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">An atmospheric <span class="hlt">non-thermal</span> plasma jet was developed for sterilizing the Staphylococcus aureus (S. aureus). The plasma jet was generated by dielectric barrier discharge (DBD), which was characterized by electrical and optical diagnostics. The survival curves of the bacteria showed that the plasma jet could effectively inactivate 106 cells of S. aureus within 120 seconds and the sterilizing efficiency depended critically on the discharge parameter of the applied voltage. It was further confirmed by scanning electron microscopy (SEM) that the cell morphology was seriously damaged by the plasma treatment. The plasma sterilization mechanism of S. aureus was attributed to the active species of OH, N2+ and O, which were generated abundantly in the plasma jet and characterized by OES. Our findings suggest a convenient and low-cost way for sterilization and inactivation of bacteria.</p> <div class="credits"> <p class="dwt_author">Liu, Xiaohu; Hong, Feng; Guo, Ying; Zhang, Jing; Shi, Jianjun</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-05-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">284</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2012APS..GECAM1009L"> <span id="translatedtitle">Control of the Proliferation of Mammalian Cells by the <span class="hlt">Non-Thermal</span> Atmospheric Pressure Plasmas</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Recent development of the atmospheric pressure plasmas (APPs) reported dramatic achievement on the applications to sterilization, wound healing, blood coagulation, and so on. These effects are coming from the abundant electrons, various ions, radicals, and neutral atoms which cause specific interactions with cells. However, the application of APPs to human cells has been mainly focused on cell death, but not so much on cell proliferation. In this study, the effects of a <span class="hlt">non-thermal</span> dielectric barrier discharge (DBD) were investigated for three different human cell lines. It was observed that the exposure of APP to human adipose-derived stem cells (ASC) and the primary lung fibroblast IMR-90 cells induced increased cell proliferation in a specific condition. On the other hand, the same exposure of APP to HeLa cells dramatically decreased their viability. These observations suggest that different types of human cells differentially respond to the exposure of APP.</p> <div class="credits"> <p class="dwt_author">Lee, Hae June; Ha, Chang Seung; Ma, Yonghao; Lee, Jungyeol; Song, Kiwon</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-10-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">285</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/23954717"> <span id="translatedtitle">Removal of dimethyl sulfide by the combination of <span class="hlt">non-thermal</span> plasma and biological process.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">A bench scale system integrated with a <span class="hlt">non-thermal</span> plasma (NTP) and a biotricking filtration (BTF) unit for the treatment of gases containing dimethyl sulfide (DMS) was investigated. DMS removal efficiency in the integrated system was up to 96%. Bacterial communities in the BTF were assessed by PCR-DGGE, which play the dominant role in the biological processes of metabolism, sulfur oxidation, sulfate-reducing and carbon oxidation. The addition of ozone from NTP made microbial community in BTF more complicated and active for DMS removal. The NTP oxidize DMS to simple compounds such as methanol and carbonyl sulfide; the intermediate organic products and DMS are further oxidized to sulfate, carbon dioxide, water vapors by biological degradation. These results show that NTP-BTF is achievable and open new possibilities for applying the integrated with NTP and BTF to odour gas treatment. PMID:23954717</p> <div class="credits"> <p class="dwt_author">Wei, Z S; Li, H Q; He, J C; Ye, Q H; Huang, Q R; Luo, Y W</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-10-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">286</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/22113399"> <span id="translatedtitle">Dust-acoustic shock formation in dusty plasmas with <span class="hlt">non-thermal</span> ions</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">In this study, the nonlinear Burgers equation in the presence of the dust charge fluctuation is derived and the shock-like solution is determined. It is well known that in order to have a monotonic or oscillatory shock wave, a source of dissipation is needed. By using the experimental data reported in the laboratory observation of self-excited dust-acoustic shock waves [Heinrich et al., Phys. Rev. Lett. 103, 115002 (2009)], it is shown that dust charge fluctuation can be considered as a candidate for the source of dissipation needed for the dust-acoustic shock formation. By examining the effects of <span class="hlt">non-thermal</span> ions on dust-acoustic shock's characteristics, a possible theoretical explanation for the discrepancies observed between theory and experiment is proposed.</p> <div class="credits"> <p class="dwt_author">Asgari, H.; Muniandy, S. V.; Wong, C. S. [Plasma Technology Research Center, Department of Physics, University of Malaya, 50603 Kuala Lumpur (Malaysia)</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-01-15</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">287</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3432087"> <span id="translatedtitle">Eradication of Pseudomonas aeruginosa Biofilms by Atmospheric Pressure <span class="hlt">Non-Thermal</span> Plasma</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p class="result-summary">Bacteria exist, in most environments, as complex, organised communities of sessile cells embedded within a matrix of self-produced, hydrated extracellular polymeric substances known as biofilms. Bacterial biofilms represent a ubiquitous and predominant cause of both chronic infections and infections associated with the use of indwelling medical devices such as catheters and prostheses. Such infections typically exhibit significantly enhanced tolerance to antimicrobial, biocidal and immunological challenge. This renders them difficult, sometimes impossible, to treat using conventional chemotherapeutic agents. Effective alternative approaches for prevention and eradication of biofilm associated chronic and device-associated infections are therefore urgently required. Atmospheric pressure <span class="hlt">non-thermal</span> plasmas are gaining increasing attention as a potential approach for the eradication and control of bacterial infection and contamination. To date, however, the majority of studies have been conducted with reference to planktonic bacteria and rather less attention has been directed towards bacteria in the biofilm mode of growth. In this study, the activity of a kilohertz-driven atmospheric pressure <span class="hlt">non-thermal</span> plasma jet, operated in a helium oxygen mixture, against Pseudomonas aeruginosa in vitro biofilms was evaluated. Pseudomonas aeruginosa biofilms exhibit marked susceptibility to exposure of the plasma jet effluent, following even relatively short (?10?s s) exposure times. Manipulation of plasma operating conditions, for example, plasma operating frequency, had a significant effect on the bacterial inactivation rate. Survival curves exhibit a rapid decline in the number of surviving cells in the first 60 seconds followed by slower rate of cell number reduction. Excellent anti-biofilm activity of the plasma jet was also demonstrated by both confocal scanning laser microscopy and metabolism of the tetrazolium salt, XTT, a measure of bactericidal activity.</p> <div class="credits"> <p class="dwt_author">Alkawareek, Mahmoud Y.; Algwari, Qais Th.; Laverty, Garry; Gorman, Sean P.; Graham, William G.; O'Connell, Deborah; Gilmore, Brendan F.</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">288</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/22952948"> <span id="translatedtitle">Eradication of Pseudomonas aeruginosa biofilms by atmospheric pressure <span class="hlt">non-thermal</span> plasma.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">Bacteria exist, in most environments, as complex, organised communities of sessile cells embedded within a matrix of self-produced, hydrated extracellular polymeric substances known as biofilms. Bacterial biofilms represent a ubiquitous and predominant cause of both chronic infections and infections associated with the use of indwelling medical devices such as catheters and prostheses. Such infections typically exhibit significantly enhanced tolerance to antimicrobial, biocidal and immunological challenge. This renders them difficult, sometimes impossible, to treat using conventional chemotherapeutic agents. Effective alternative approaches for prevention and eradication of biofilm associated chronic and device-associated infections are therefore urgently required. Atmospheric pressure <span class="hlt">non-thermal</span> plasmas are gaining increasing attention as a potential approach for the eradication and control of bacterial infection and contamination. To date, however, the majority of studies have been conducted with reference to planktonic bacteria and rather less attention has been directed towards bacteria in the biofilm mode of growth. In this study, the activity of a kilohertz-driven atmospheric pressure <span class="hlt">non-thermal</span> plasma jet, operated in a helium oxygen mixture, against Pseudomonas aeruginosa in vitro biofilms was evaluated. Pseudomonas aeruginosa biofilms exhibit marked susceptibility to exposure of the plasma jet effluent, following even relatively short (? 10's s) exposure times. Manipulation of plasma operating conditions, for example, plasma operating frequency, had a significant effect on the bacterial inactivation rate. Survival curves exhibit a rapid decline in the number of surviving cells in the first 60 seconds followed by slower rate of cell number reduction. Excellent anti-biofilm activity of the plasma jet was also demonstrated by both confocal scanning laser microscopy and metabolism of the tetrazolium salt, XTT, a measure of bactericidal activity. PMID:22952948</p> <div class="credits"> <p class="dwt_author">Alkawareek, Mahmoud Y; Algwari, Qais Th; Laverty, Garry; Gorman, Sean P; Graham, William G; O'Connell, Deborah; Gilmore, Brendan F</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">289</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/19910483"> <span id="translatedtitle">Killing of adherent oral microbes by a <span class="hlt">non-thermal</span> atmospheric plasma jet.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">Atmospheric plasma jets are being intensively studied with respect to potential applications in medicine. The aim of this in vitro study was to test a microwave-powered <span class="hlt">non-thermal</span> atmospheric plasma jet for its antimicrobial efficacy against adherent oral micro-organisms. Agar plates and dentin slices were inoculated with 6 log(10) c.f.u. cm(-2) of Lactobacillus casei, Streptococcus mutans and Candida albicans, with Escherichia coli as a control. Areas of 1 cm(2) on the agar plates or the complete dentin slices were irradiated with a helium plasma jet for 0.3, 0.6 or 0.9 s mm(-2), respectively. The agar plates were incubated at 37 degrees C, and dentin slices were vortexed in liquid media and suspensions were placed on agar plates. The killing efficacy of the plasma jet was assessed by counting the number of c.f.u. on the irradiated areas of the agar plates, as well as by determination of the number of c.f.u. recovered from dentin slices. A microbe-killing effect was found on the irradiated parts of the agar plates for L. casei, S. mutans, C. albicans and E. coli. The plasma-jet treatment reduced the c.f.u. by 3-4 log(10) intervals on the dentin slices in comparison to recovery rates from untreated controls. The microbe-killing effect was correlated with increasing irradiation times. Thus, <span class="hlt">non-thermal</span> atmospheric plasma jets could be used for the disinfection of dental surfaces. PMID:19910483</p> <div class="credits"> <p class="dwt_author">Rupf, Stefan; Lehmann, Antje; Hannig, Matthias; Schäfer, Barbara; Schubert, Andreas; Feldmann, Uwe; Schindler, Axel</p> <p class="dwt_publisher"></p> <p class="publishDate">2010-02-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">290</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=20070022510&hterms=Black+Holes&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D60%26Ntt%3D%2522Black%2BHoles%2522"> <span id="translatedtitle">Gamma-ray Spectral Characteristics of Thermal and <span class="hlt">Non-thermal</span> Emission from Three Black Holes</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">Cygnus X-1 and the gamma-ray transients GROJ0422+32 and GROJ1719-24 displayed similar spectral properties when they underwent transitions between the high and low gamma-ray (30 keV to few MeV) intensity states. When these sources were in the high (gamma)-ray intensity state ((gamma)2, for Cygnus X-l), their spectra featured two components: a Comptonized shape below 200-300 keV with a soft power-law tail (photon index >= 3) that extended to 1 MeV or beyond. When the sources were in the low-intensity state ((gamma)0, for Cygnus X-l), the Comptonized spectral shape below 200 keV typically vanished and the entire spectrum from 30 keV to 1 MeV can be characterized by a single power law with a relatively harder photon index 2-2.7. Consequently the high- and low-intensity gamma-ray spectra intersect, generally in the 400 KeV - 1 MeV range, in contrast to the spectral pivoting seen previously at lower (10 keV) energies. The presence of the power-law component in both the high- and low-intensity gammaray spectra strongly suggests that the <span class="hlt">non-thermal</span> process is likely to be at work in both the high and the low-intensity situations. We have suggested a possible scenario (Ling & Wheaton, 2003), by combining the ADAF model of Esin et al. (1998) with a separate jet region that produces the <span class="hlt">non-thermal</span> gamma-ray emission, and which explains the state transitions. Such a scenario will be discussed in the context of the observational evidence, summarized above, from the database produced by EBOP, JPL's BATSE earth occultation analysis system.</p> <div class="credits"> <p class="dwt_author">Ling, James C.; Wheaton, William A.</p> <p class="dwt_publisher"></p> <p class="publishDate">2004-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">291</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2011AdSpR..48.1578E"> <span id="translatedtitle">Solitary, explosive and periodic solutions for electron acoustic solitary waves with <span class="hlt">non-thermal</span> hot ions</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">A theoretical investigation has been made for electron acoustic waves propagating in a system of unmagnetized collisionless plasma consists of a cold electron fluid and ions with two different temperatures in which the hot ions obey the <span class="hlt">non-thermal</span> distribution. The reductive perturbation method has been employed to derive the Korteweg-de Vries equation for small but finite amplitude electrostatic waves. It is found that the presence of the energetic population of <span class="hlt">non-thermal</span> hot ions ?, initial normalized equilibrium density of low temperature ions ? and the ratio of temperatures of low temperature ions to high temperature ions ? do not only significantly modify the basic properties of solitary structure, but also change the polarity of the solitary profiles. At the critical hot ions density, the KdV equation is not appropriate for describing the system. Hence, a new set of stretched coordinates is considered to derive the modified KdV equation. In the vicinity of the critical hot ions density, neither KdV nor modified KdV equation is appropriate for describing the electron acoustic waves. Therefore, a further modified KdV equation is derived. An algebraic method with computerized symbolic computation, which greatly exceeds the applicability of the existing tanh, extended tanh methods in obtaining a series of exact solutions of the various KdV-type equations, is used here. Numerical studies have been reveals different solutions e.g., bell-shaped solitary pulses, singular solitary "blowup" solutions, Jacobi elliptic doubly periodic wave, Weierstrass elliptic doubly periodic type solutions, in addition to explosive pulses. The results of the present investigation may be applicable to some plasma environments, such as Earth's magnetotail region.</p> <div class="credits"> <p class="dwt_author">Elwakil, S. A.; Abulwafa, E. M.; El-Shewy, E. K.; Abd-El-Hamid, H. M.</p> <p class="dwt_publisher"></p> <p class="publishDate">2011-11-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">292</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/21304887"> <span id="translatedtitle"><span class="hlt">Non</span> <span class="hlt">Thermal</span> Emission from Clusters of Galaxies: the Importance of a Joint LOFAR/Simbol-X View</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">Deep radio observations of galaxy clusters have revealed the existence of diffuse radio sources ('halos' and 'relics') related to the presence of relativistic electrons and weak magnetic fields in the intracluster volume. I will outline our current knowledge about the presence and properties of this <span class="hlt">non-thermal</span> cluster component. Despite the recent progress made in observational and theoretical studies of the <span class="hlt">non-thermal</span> emission in galaxy clusters, a number of open questions about its origin and its effects on the thermo-dynamical evolution of galaxy clusters need to be answered. I will show the importance of combining galaxy cluster observations by new-generation instruments such as LOFAR and Simbol-X. A deeper knowledge of the <span class="hlt">non-thermal</span> cluster component, together with statistical studies of radio halos and relics, will allow to test the current cluster formation scenario and to better constrain the physics of large scale structure evolution.</p> <div class="credits"> <p class="dwt_author">Ferrari, C. [UNSA, CNRS UMR 6202 Cassiopee, Observatoire de la Cote d'Azur, Nice (France)</p> <p class="dwt_publisher"></p> <p class="publishDate">2009-05-11</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">293</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2009EPJD...54..153P"> <span id="translatedtitle">Electrohydrodynamic flow in a wire-plate <span class="hlt">non-thermal</span> plasma reactor measured by 3D PIV method</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">This work was aimed at measurements of the electrohydrodynamic (EHD) secondary flow in a <span class="hlt">non-thermal</span> plasma reactor using three-dimensional particle image velocimetry (3D PIV) method. The wide-type <span class="hlt">non-thermal</span> plasma reactor used in this work was an acrylic box with a wire discharge electrode and two plate collecting electrodes. The positive DC voltage was applied to the wire electrode through a 10 M? resistor. The collecting electrodes were grounded. The voltage applied to the wire electrode was 28 kV. Air flow seeded with a cigarette smoke was blown along the reactor duct with an average velocity of 0.6 m/s. The 3D PIV velocity fields measurements were carried out in four parallel planes stretched along the reactor duct, perpendicularly to the wire electrode and plate electrodes. The measured flow velocity fields illustrate complex nature of the EHD induced secondary flow in the <span class="hlt">non-thermal</span> plasma reactor.</p> <div class="credits"> <p class="dwt_author">Podlinski, J.; Niewulis, A.; Mizeraczyk, J.</p> <p class="dwt_publisher"></p> <p class="publishDate">2009-08-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">294</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=2590178"> <span id="translatedtitle"><span class="hlt">Non-thermal</span> influences on the control of skin blood flow have minimal effects on heat transfer during exercise.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p class="result-summary">During exercise, circulatory reflexes ensure that the cardiac output is sufficiently elevated to meet the oxygen delivery requirements of the contracting skeletal muscles and the heat delivery requirements of the body to the skin. The latter requirements are met by increasing skin blood flow. These increases are largely driven by elevations in the body temperatures, although <span class="hlt">non-thermal</span> effects on the control of skin blood flow occur in certain conditions. These effects are largely the consequence of high and/or low baroreflex stimulation. Even in the face of such <span class="hlt">non-thermal</span> effects, which occur during exercise in the heat, the body's requirements for heat transfer from core to skin are largely met by the increased skin blood flow. Thus, <span class="hlt">non-thermal</span> effects on the control of skin blood flow are relatively unimportant in the body's overall regulatory response to exercise.</p> <div class="credits"> <p class="dwt_author">Nadel, E. R.</p> <p class="dwt_publisher"></p> <p class="publishDate">1986-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">295</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2014HEAD...1410607N"> <span id="translatedtitle">Hot Flow Model for Low Luminosity AGNs and Black Hole Binaries: the Role and Origin of <span class="hlt">Non-thermal</span> Electrons</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Optically thin, two-temperature accretion flows are widely considered as a relevant accretion mode below ~0.01 LEdd in AGNs as well as in X-ray binaries. We study spectral formation in such flows using a refined model with a fully general relativistic description of both the radiative (leptonic and hadronic) and hydrodynamic processes, and with an exact treatment of global Comptonization. We point out that basic properties of two-temperature flows determine the relative strengths of the synchrotron radiation of thermal electrons and <span class="hlt">non-thermal</span> electrons from charged-pion decay, in a manner consistent with observations. In AGNs, the <span class="hlt">non-thermal</span> synchrotron dominates the seed photon input down to ~10-5 LEdd and it allows to explain the X-ray spectral index–Eddington ratio relation as well as the cut-off energies measured in the best-studied AGNs; the (standard) model with the thermal synchrotron being the main source of seed photons does not agree with these observations. For stellar-mass black holes, <span class="hlt">non-thermal</span> electrons from hadronic processes become important only above ~0.01 LEdd (and may be relevant for the <span class="hlt">non-thermal</span> tails observed in luminous hard states of Cyg X-1 and GX 339-4) and we find that the thermal synchrotron provides a sufficient seed photon flux to explain observations of black hole transients below ~0.01 LEdd. We also note that <span class="hlt">non-thermal</span> acceleration processes in hot flows are constrained by comparisons of the predicted gamma-ray fluxes (from neutral pion decay) with Fermi-LAT upper limits. For NGC 4151, it limits the energy content in the <span class="hlt">non-thermal</span> component of proton distribution to at most 1 per cent.</p> <div class="credits"> <p class="dwt_author">Niedzwiecki, Andrzej; Xie, Fu-Guo; Stepnik, Agnieszka</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-08-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">296</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4078877"> <span id="translatedtitle"><span class="hlt">Non-thermal</span>, pulsed electric field cell ablation: A novel tool for regenerative medicine and scarless skin regeneration</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p class="result-summary">High voltage, short pulsed electric fields (PEF) is a <span class="hlt">non-thermal</span> ablation method, in which defined PEF irreversibly destabilize cell membranes, while preserving other tissue components such as the extracellular matrix (ECM). In the present report, we show that PEF ablated rat skin retains its microvascular blood supply and ECM structure. Complete regeneration of epidermis, hair follicles, sebaceous glands, and the panniculus carnosusis observed two months after the ablation. Our results clearly indicate that <span class="hlt">non-thermal</span> PEF has the potential to be a powerful and novel tool for scarless tissue regeneration.</p> <div class="credits"> <p class="dwt_author">Golberg, Alexander; Broelsch, G. Felix; Bohr, Stefan; Mihm, Martin C.; Austen, William G.; Albadawi, Hassan; Watkins, Michael T.; Yarmush, Martin L.</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">297</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/1644249"> <span id="translatedtitle">Removal of volatile organic compounds from air streams and industrial flue gases by <span class="hlt">non-thermal</span> plasma technology</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">Gaseous pollution control technologies for acid gases (NOx , SOx, etc.), volatile organic compounds (VOC), greenhouse gases, ozone layer depleting substance (ODS), etc., have been commercialized based on catalysis, incineration and adsorption methods. However, <span class="hlt">non-thermal</span> plasma techniques based on electron beams and corona discharges become significant due to advantages such as lower cost, higher removal efficiency, smaller space volume, etc.</p> <div class="credits"> <p class="dwt_author">Kuniko Urashima; Jen-Shih Chang</p> <p class="dwt_publisher"></p> <p class="publishDate">2000-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">298</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/23820168"> <span id="translatedtitle">Pathology of <span class="hlt">non-thermal</span> irreversible electroporation (N-TIRE)-induced ablation of the canine brain.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">This study describes the neuropathologic features of normal canine brain ablated with <span class="hlt">non-thermal</span> irreversible electroporation (N-TIRE). The parietal cerebral cortices of four dogs were treated with N-TIRE using a dose-escalation protocol with an additional dog receiving sham treatment. Animals were allowed to recover following N-TIRE ablation and the effects of treatment were monitored with clinical and magnetic resonance imaging examinations. Brains were subjected to histopathologic and ultrastructural assessment along with Bcl-2, caspase-3, and caspase-9 immunohistochemical staining following sacrifice 72 h post-treatment. Adverse clinical effects of N-TIRE were only observed in the dog treated at the upper energy tier. MRI and neuropathologic examinations indicated that N-TIRE ablation resulted in focal regions of severe cytoarchitectural and blood-brain-barrier disruption. Lesion size correlated to the intensity of the applied electrical field. N-TIRE-induced lesions were characterized by parenchymal necrosis and hemorrhage; however, large blood vessels were preserved. A transition zone containing parenchymal edema, perivascular inflammatory cuffs, and reactive gliosis was interspersed between the necrotic focus and normal neuropil. Apoptotic labeling indices were not different between the N-TIRE-treated and control brains. This study identified N-TIRE pulse parameters that can be used to safely create circumscribed foci of brain necrosis while selectively preserving major vascular structures. PMID:23820168</p> <div class="credits"> <p class="dwt_author">Rossmeisl, John H; Garcia, Paulo A; Roberston, John L; Ellis, Thomas L; Davalos, Rafael V</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">299</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/24139886"> <span id="translatedtitle">Potential cellular targets and antibacterial efficacy of atmospheric pressure <span class="hlt">non-thermal</span> plasma.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">Atmospheric pressure <span class="hlt">non-thermal</span> plasma (APNTP) has been gaining increasing interest as a new alternative antibacterial approach. Although this approach has demonstrated promising antibacterial activity, its exact mechanism of action remains unclear. Mechanistic elucidation of the antimicrobial activity will facilitate development and rational optimisation of this approach for potential medical applications. In this study, the antibacterial efficacy of an in-house-built APNTP jet was evaluated alongside an investigation of the interactions between APNTP and major cellular components in order to identify the potential cellular targets involved in plasma-mediated bacterial destruction mechanisms. The investigated plasma jet exhibited excellent, rapid antibacterial activity against a selected panel of clinically significant bacterial species including Bacillus cereus, meticillin-resistant Staphylococcus aureus (MRSA), Escherichia coli and Pseudomonas aeruginosa, all of which were completely inactivated within 2 min of plasma exposure. Plasma-mediated damaging effects were observed, to varying degrees, on all of the investigated cellular components including DNA, a model protein enzyme, and lipid membrane integrity and permeability. The antibacterial efficacy of APNTP appears to involve a multiple-target mechanism, which potentially reduces the likelihood of emergence of microbial resistance towards this promising antimicrobial approach. However, cellular membrane damage and resulting permeability perturbation was found to be the most likely rate-determining step in this mechanism. PMID:24139886</p> <div class="credits"> <p class="dwt_author">Alkawareek, Mahmoud Y; Gorman, Sean P; Graham, William G; Gilmore, Brendan F</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-02-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">300</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2014AAS...22315411Z"> <span id="translatedtitle">Evidence for <span class="hlt">non-thermal</span> radio emission from a classical nova - V1723 Aql</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">The outburst of classical nova V1723 Aql was observed on September 11, 2012. The long term radio observations so far show that it exhibits double-bump radio light curves and partially optically thin spectra. The first bump doesn't follow the classical Hubble Flow Mode which depicts the evolution of thick sphercially expanding thermal ejecta. The brightness temperature varies with time and frequencies(1e7 K at 1.38 GHz, 1e5 K at 36.53 GHz, around the first maximum). We examine whether the first bump can be explained by the model of a shock-heated thin shell lying above the main ejecta. The modified model with linear temperature gradient ( r^q, q=0,+/-1) and steep density profile (? ~ r^{-p},p=2,9) in the shell fails to explain the first bump light curves and flat spectra. The late-time observation day 800) implies a spectrum of f? ~ ?^{-0.65} (40 GHz>?>10 GHz) which strongly indicates the existance of <span class="hlt">non-thermal</span> (synchrotron) emission.</p> <div class="credits"> <p class="dwt_author">Zheng, Yong; Sokoloski, J. L.; Rupen, M. P.; Weston, J.; Chomiuk, L.; Mioduszewski, A. J.; Mukai, K.; Krauss, M. I.; Roy, N.; Nelson, T.</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-01-01</p> </div> </div> </div> </div> <div id="filter_results_form" class="filter_results_form floatContainer" style="visibility: visible;"> <div style="width:100%" id="PaginatedNavigation" class="paginatedNavigationElement"> <a id="FirstPageLink" onclick='return showDiv("page_1");' href="#" title="First Page"> <img id="FirstPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.first.18x20.png" alt="First Page" /></a> <a id="PreviousPageLink" onclick='return showDiv("page_14");' href="#" title="Previous Page"> <img id="PreviousPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.previous.18x20.png" alt="Previous Page" /></a> <span id="PageLinks" class="pageLinks"> <span> <a onClick='return showDiv("page_1");' href="#">1</a> <a onClick='return showDiv("page_2");' href="#">2</a> <a onClick='return showDiv("page_3");' href="#">3</a> <a onClick='return 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href="#">11</a> <a onClick='return showDiv("page_12");' href="#">12</a> <a onClick='return showDiv("page_13");' href="#">13</a> <a onClick='return showDiv("page_14");' href="#">14</a> <a onClick='return showDiv("page_15");' href="#">15</a> <a style="font-weight: bold;">16</a> <a onClick='return showDiv("page_17");' href="#">17</a> <a onClick='return showDiv("page_18");' href="#">18</a> <a onClick='return showDiv("page_19");' href="#">19</a> <a onClick='return showDiv("page_20");' href="#">20</a> <a onClick='return showDiv("page_21");' href="#">21</a> <a onClick='return showDiv("page_22");' href="#">22</a> <a onClick='return showDiv("page_23");' href="#">23</a> <a onClick='return showDiv("page_24");' href="#">24</a> <a onClick='return showDiv("page_25");' href="#">25</a> </span> </span> <a id="NextPageLink" onclick='return showDiv("page_17");' href="#" title="Next Page"> <img id="NextPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.next.18x20.png" alt="Next Page" /></a> <a id="LastPageLink" onclick='return showDiv("page_25.0");' href="#" title="Last Page"> <img id="LastPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.last.18x20.png" alt="Last Page" /></a> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">301</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/15917826"> <span id="translatedtitle">Ultrafast <span class="hlt">non-thermal</span> control of magnetization by instantaneous photomagnetic pulses.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">The demand for ever-increasing density of information storage and speed of manipulation has triggered an intense search for ways to control the magnetization of a medium by means other than magnetic fields. Recent experiments on laser-induced demagnetization and spin reorientation use ultrafast lasers as a means to manipulate magnetization, accessing timescales of a picosecond or less. However, in all these cases the observed magnetic excitation is the result of optical absorption followed by a rapid temperature increase. This thermal origin of spin excitation considerably limits potential applications because the repetition frequency is limited by the cooling time. Here we demonstrate that circularly polarized femtosecond laser pulses can be used to <span class="hlt">non-thermally</span> excite and coherently control the spin dynamics in magnets by way of the inverse Faraday effect. Such a photomagnetic interaction is instantaneous and is limited in time by the pulse width (approximately 200 fs in our experiment). Our finding thus reveals an alternative mechanism of ultrafast coherent spin control, and offers prospects for applications of ultrafast lasers in magnetic devices. PMID:15917826</p> <div class="credits"> <p class="dwt_author">Kimel, A V; Kirilyuk, A; Usachev, P A; Pisarev, R V; Balbashov, A M; Rasing, Th</p> <p class="dwt_publisher"></p> <p class="publishDate">2005-06-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">302</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/24041772"> <span id="translatedtitle">Conversion of carbon disulfide in air by <span class="hlt">non-thermal</span> plasma.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">Carbon disulfide (CS2), a typical odorous organic sulfur compound, has adverse effects on human health and is a potential threat to the environment. In the present study, CS2 conversion in air by <span class="hlt">non-thermal</span> plasma (NTP) was systematically investigated using a link tooth wheel-cylinder plasma reactor energized by a DC power supply. The results show that corona discharge is effective in removing CS2. The CS2 conversion increases with the increase of specific input energy (SIE). Both short-living (e.g. O, OH radicals) and long-living species contribute to the CS2 conversion, but the short-living species play a more important role. Both gaseous and solid products are formed during the conversion of CS2. Gaseous products mainly include CO, CO2, OCS, SO2, SO3 and H2SO4. The yields of CO and CO2 increase, the yields of OCS and SO2 follow bell curves while the sum yield of SO3 and H2SO4 remains constant as SIE increases. The solid products, consisting of CO3(2-), SO4(2-) and possible polymeric sulfur, deposit on the inner wall and electrodes of the plasma reactor. PMID:24041772</p> <div class="credits"> <p class="dwt_author">Yan, Xiao; Sun, Yifei; Zhu, Tianle; Fan, Xing</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-10-15</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">303</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2011PMB....56..951G"> <span id="translatedtitle">In vivo <span class="hlt">non-thermal</span> irreversible electroporation impact on rat liver galvanic apparent internal resistance</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary"><span class="hlt">Non-thermal</span> irreversible electroporation (NTIRE) is a biophysical phenomenon which involves application of electric field pulses to cells or tissues, causing certain rearrangements in the membrane structure leading to cell death. The treated tissue ac impedance changes induced by electroporation were shown to be the indicators for NTIRE efficiency. In a previous study we characterized in vitro tissue galvanic apparent internal resistance (GAIR) changes due to NTIRE. Here we describe an in vivo study in which we monitored the GAIR changes of a rat liver treated by NTIRE. Electrical pulses were delivered through the same Zn/Cu electrodes by which GAIR was measured. GAIR was measured before and for 3 h after the treatment at 15 min intervals. The results were compared to the established ac bioimpedance measurement method. A decrease of 33% was measured immediately after the NTIRE treatment and a 40% decrease was measured after 3 h in GAIR values; in the same time 40% and 47% decrease respectively were measured by ac bioimpedance analyses. The temperature increase due to the NTIRE was only 0.5 °C. The results open the way for an inexpensive, self-powered in vivo real-time NTIRE effectiveness measurement.</p> <div class="credits"> <p class="dwt_author">Golberg, A.; Laufer, S.; Rabinowitch, H. D.; Rubinsky, B.</p> <p class="dwt_publisher"></p> <p class="publishDate">2011-02-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">304</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2012APS..GECAM1012R"> <span id="translatedtitle">Antitumor action of <span class="hlt">non</span> <span class="hlt">thermal</span> plasma sources, DBD and Plasma Gun, alone or in combined protocols</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">The presentation deals with the assessment on two <span class="hlt">non</span> <span class="hlt">thermal</span> plasma sources developed and optimized for oncology applications. The first plasma source is a floating-electrode dielectric barrier discharge powered at a few hundreds of Hz which deliver air-plasma directly on the surface of cell culture medium in dishes or on the skin or organs of mice bearing cancer tumors. The second plasma source, so called Plasma Gun, is a plasma jet source triggered in noble gas, transferred in high aspect ratio and flexible capillaries, on targeting cells or tumors after plasma transfer in air through the ``plasma plume'' generated at the capillary outlet. In vitro evidence for massive cancer cell destruction and in vivo tumor activity and growth rate reductions have been measured with both plasma sources. DNA damages, cell cycle arrests and apoptosis induction were also demonstrated following the application of any of the two plasma source both in vitro and in vivo. The comparison of plasma treatment with state of the art chemotherapeutic alternatives has been performed and last but not least the benefit of combined protocols involving plasma and chemotherapeutic treatments has been evidenced for mice bearing orthotopic pancreas cancer and is under evaluation for the colon tumors.</p> <div class="credits"> <p class="dwt_author">Robert, Eric; Brullé, Laura; Vandamme, Marc; Riès, Delphine; Le Pape, Alain; Pouvesle, Jean-Michel</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-10-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">305</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/20839022"> <span id="translatedtitle">Augmented survival of Neisseria gonorrhoeae within biofilms: exposure to atmospheric pressure <span class="hlt">non-thermal</span> plasmas.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">Bacteria embedded within biofilms present a challenge to surface decontamination by conventional means. Atmospheric pressure <span class="hlt">non-thermal</span> plasma processes have emerged as a promising approach to overcoming this problem. We used atmospheric pressure non-equilibrium plasmas (APNPs) to assess planktonic versus biofilm-resident bacterial (Neisseria gonorrhoeae) susceptibility to treatment. The decontamination efficiency of the process was evaluated against bacteria embedded within a biofilm, as well as planktonic cells placed on a glass surface. Bacterial survival was assessed using a combination of colony forming unit (CFU) ability and vital staining with a combination of SYTO9 plus propidium iodide. Both methods revealed an increased resistance of biofilm-resident bacteria compared with planktonic cells, after a 20-min exposure to the APNPs. Transmission electron microscopy revealed disruption and damage to the cell wall, resulting in the release of cytoplasmic compounds, alterations in morphology, and a decrease in cell volume, indicating that APNPs may affect the cell wall. Present results show that biofilm-resident bacteria demonstrate augmented survival when exposed to APNP treatment and therefore that decontamination procedures should take into account this survival when evaluating surface decontamination measures. PMID:20839022</p> <div class="credits"> <p class="dwt_author">Xu, L; Tu, Y; Yu, Y; Tan, M; Li, J; Chen, H</p> <p class="dwt_publisher"></p> <p class="publishDate">2011-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">306</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/22215418"> <span id="translatedtitle">EVIDENCE OF <span class="hlt">NON-THERMAL</span> X-RAY EMISSION FROM HH 80</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">Protostellar jets appear at all stages of star formation when the accretion process is still at work. Jets travel at velocities of hundreds of km s{sup –1}, creating strong shocks when interacting with the interstellar medium. Several cases of jets have been detected in X-rays, typically showing soft emission. For the first time, we report evidence of hard X-ray emission possibly related to <span class="hlt">non-thermal</span> processes not explained by previous models of the post-shock emission predicted in the jet/ambient interaction scenario. HH 80 is located at the south head of the jet associated with the massive protostar IRAS 18162-2048. It shows soft and hard X-ray emission in regions that are spatially separated, with the soft X-ray emission region situated behind the region of hard X-ray emission. We propose a scenario for HH 80 where soft X-ray emission is associated with thermal processes from the interaction of the jet with denser ambient matter and hard X-ray emission is produced by synchrotron radiation at the front shock.</p> <div class="credits"> <p class="dwt_author">López-Santiago, J. [Instituto de Matemática Interdisciplinar, S. D. Astronomía y Geodesia, Facultad de Ciencias Matemáticas, Universidad Complutense de Madrid, E-28040 Madrid (Spain)] [Instituto de Matemática Interdisciplinar, S. D. Astronomía y Geodesia, Facultad de Ciencias Matemáticas, Universidad Complutense de Madrid, E-28040 Madrid (Spain); Peri, C. S.; Benaglia, P. [Instituto Argentino de Radioastronomía (IAR), CCT La Plata (CONICET), C.C.5, 1894 Villa Elisa, Buenos Aires (Argentina)] [Instituto Argentino de Radioastronomía (IAR), CCT La Plata (CONICET), C.C.5, 1894 Villa Elisa, Buenos Aires (Argentina); Bonito, R. [Dipartimento di Fisica e Chimica, Università di Palermo, Piazza del Parlamento 1, I-90134 Palermo (Italy)] [Dipartimento di Fisica e Chimica, Università di Palermo, Piazza del Parlamento 1, I-90134 Palermo (Italy); Miceli, M. [INAF-Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, I-90134 Palermo (Italy)] [INAF-Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, I-90134 Palermo (Italy); Albacete-Colombo, J. F. [Universidad Nacional del COMAHUE, Monseñor Esandi y Ayacucho, 8500 Viedma, Río Negro (Argentina)] [Universidad Nacional del COMAHUE, Monseñor Esandi y Ayacucho, 8500 Viedma, Río Negro (Argentina); De Castro, E. [Dpto. de Astrofísica y CC. de la Atmósfera, Universidad Complutense de Madrid, E-28040 Madrid (Spain)] [Dpto. de Astrofísica y CC. de la Atmósfera, Universidad Complutense de Madrid, E-28040 Madrid (Spain)</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-10-20</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">307</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/servlets/purl/16711"> <span id="translatedtitle">Direct chemical oxidation: a <span class="hlt">non-thermal</span> technology for the destruction of organic wastes</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">Direct Chemical Oxidation (DCO) is a <span class="hlt">non-thermal</span>, ambient pressure, aqueous-based technology for the oxidative destruction of the organic components of hazardous or mixed waste streams. The process has been developed for applications in waste treatment and chemical demilitarization and decontamination at LLNL since 1992, and is applicable to the destruction of virtually all solid or liquid organics, including: chlorosolvents, oils and greases, detergents, organic-contaminated soils or sludges, explosives, chemical and biological warfare agents, and PCB's. [1-15] The process normally operates at 80-100 C, a heating requirement which increases the difficulty of surface decontamination of large objects or, for example, treatment of a wide area contaminated soil site. The driver for DCO work in FY98 was thus to investigate the use of catalysts to demonstrate the effectiveness of the technology for organics destruction at temperatures closer to ambient. In addition, DCO is at a sufficiently mature stage of development that technology transfer to a commercial entity was a logical next step, and was thus included in FY98 tasks.</p> <div class="credits"> <p class="dwt_author">Balazs, G.B.; Cooper, J. F.; Lewis, P. R.; Adamson, M. G.</p> <p class="dwt_publisher"></p> <p class="publishDate">1998-02-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">308</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2013JAP...114j4701S"> <span id="translatedtitle"><span class="hlt">Non-thermal</span> mechanism of weak microwave fields influence on neurons</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">A <span class="hlt">non-thermal</span> mechanism of weak microwave field impact on a nerve fiber is proposed. It is shown that in the range of about 30-300 GHz, there are strongly pronounced resonances associated with the excitation of ultrasonic vibrations in the membrane as a result of interaction with electromagnetic radiation. The viscous dissipation limits the resonances and results in their broadening. These forced vibrations create acoustic pressure, which may lead to the redistribution of the protein transmembrane channels, and thus changing the threshold of the action potential excitation in the axons of the neural network. The influence of the electromagnetic microwave radiation on various specific areas of myelin nerve fibers was analyzed: the nodes of Ranvier, and the initial segment--the area between the neuron hillock and the first part of the axon covered with the myelin layer. It was shown that the initial segment is the most sensitive area of the myelined neurons from which the action potential normally starts.</p> <div class="credits"> <p class="dwt_author">Shneider, M. N.; Pekker, M.</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-09-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">309</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/22092062"> <span id="translatedtitle">SUZAKU OBSERVATIONS OF THE <span class="hlt">NON-THERMAL</span> SUPERNOVA REMNANT HESS J1731-347</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">A detailed analysis of the <span class="hlt">non-thermal</span> X-ray emission from the northwestern and southern parts of the supernova remnant (SNR) HESS J1731-347 with Suzaku is presented. The shell portions covered by the observations emit hard and lineless X-rays. The spectrum can be reproduced by a simple absorbed power-law model with a photon index {Gamma} of 1.8-2.7 and an absorption column density N{sub H} of (1.0-2.1) Multiplication-Sign 10{sup 22} cm{sup -2}. These quantities change significantly from region to region; the northwestern part of the SNR has the hardest and most absorbed spectrum. The western part of the X-ray shell has a smaller curvature than the northwestern and southern shell segments. A comparison of the X-ray morphology to the very high energy gamma-ray and radio images was performed. The efficiency of the electron acceleration and the emission mechanism in each portion of the shell are discussed. Thermal X-ray emission from the SNR was searched for but could not be detected at a significant level.</p> <div class="credits"> <p class="dwt_author">Bamba, Aya; Yamazaki, Ryo [Department of Physics and Mathematics, Aoyama Gakuin University, 5-10-1 Fuchinobe, Chuo-ku, Sagamihara, Kanagawa 252-5258 (Japan); Puehlhofer, Gerd; Klochkov, Dmitry [Institut fuer Astronomie und Astrophysik, Universitaet Tuebingen, Sand 1, D-72076 Tuebingen (Germany); Acero, Fabio [Laboratoire Univers et Particules de Montpellier, Universite Montpellier 2, CNRS/IN2P3, CC 72, Place Eugene Bataillon, F-34095 Montpellier (France); Tian Wenwu [National Astronomical Observatories, CAS, Beijing 100012 (China); Li Zhiyuan [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States); Horns, Dieter [Institut fuer Experimentalphysik, Universitaet Hamburg, Luruper Chaussee 149, D-22761 Hamburg (Germany); Kosack, Karl [CEA Saclay, DSM/IRFU, F-91191 Gif-sur-Yvette (France); Komin, Nukri [Laboratoire d'Annecy-le-Vieux de Physique des Particules, Universite de Savoie, CNRS/IN2P3, F-74941 Annecy-le-Vieux (France)</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-09-10</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">310</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2013MNRAS.429L..70O"> <span id="translatedtitle"><span class="hlt">Non-thermal</span> emission from pulsar-wind nebulae in starburst galaxies</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">The recently detected ?-ray emission from starburst galaxies is most commonly considered to be diffuse emission arising from strong interactions of accelerated cosmic rays. Mannheim, Elsässer & Tibolla, however, have argued that a population of individual pulsar-wind nebulae (PWNe) could be responsible for the detected TeV emission. Here, we show that the starburst environment plays a critical role in the TeV emission from starburst PWN, and perform the first detailed calculations for this scenario. Our approach is based on the measured star formation rates in the starburst nuclei of NGC 253 and M82, assumed pulsar birth periods and a simple model for the injection of <span class="hlt">non-thermal</span> particles. The two-zone model applied here takes into account the high far-infrared radiation field and different densities and magnetic fields in the PWN and the starburst regions, as well as particle escape. We confirm that PWN can make a significant contribution to the TeV fluxes, provided that the injection spectrum of particles is rather hard and that the average pulsar birth period is rather short (˜35 ms). The PWN contribution should lead to a distinct spectral feature which can be probed by future instruments such as Cherenkov Telescope Array.</p> <div class="credits"> <p class="dwt_author">Ohm, S.; Hinton, J. A.</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-02-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">311</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/23735483"> <span id="translatedtitle">Impact of <span class="hlt">non-thermal</span> plasma treatment on MAPK signaling pathways of human immune cell lines.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">In the field of wound healing research <span class="hlt">non-thermal</span> plasma (NTP) increasingly draws attention. Next to its intensely studied antibacterial effects, some studies already showed stimulating effects on eukaryotic cells. This promises a unique potential in healing of chronic wounds, where effective therapies are urgently needed. Immune cells do play an important part in the process of wound healing and their reaction to NTP treatment has yet been rarely examined. Here, we studied the impact of NTP treatment using the kinpen on apoptotic and proliferative cell signaling pathways of two human immune cell lines, the CD4(+)T helper cell line Jurkat and the monocyte cell line THP-1. Depending on NTP treatment time the number of apoptotic cells increased in both investigated cell types according to a caspase 3 assay. Western blot analysis pointed out that plasma treatment activated pro-apoptotic signaling proteins like p38 mitogen-activated protein kinase (p38 MAPK) and c-Jun N-terminal kinase 1 and 2 (JNK 1/2) in both cell types. Stronger signals were detected in Jurkat cells at comparable plasma treatment times. Intriguingly, exposure of Jurkat and THP-1 cells to plasma also activated the pro-proliferative signaling molecules extracellular signal-regulated kinase 1/2 (ERK 1/2) and MAPK/ERK kinase 1 and 2 (MEK 1/2). In contrast to Jurkat cells, the anti-apoptotic heat shock protein 27 (HSP27) was activated in THP-1 cells after plasma treatment, indicating a possible mechanism how THP-1 cells may reduce programmed cell death. In conclusion, several signaling cascades were activated in the examined immune cell lines after NTP treatment and in THP-1 monocytes a possible defense mechanism against plasma impacts could be revealed. Therefore, plasma might be a treatment option for wound healing. PMID:23735483</p> <div class="credits"> <p class="dwt_author">Bundscherer, Lena; Wende, Kristian; Ottmüller, Katja; Barton, Annemarie; Schmidt, Anke; Bekeschus, Sander; Hasse, Sybille; Weltmann, Klaus-Dieter; Masur, Kai; Lindequist, Ulrike</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-10-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">312</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/23668811"> <span id="translatedtitle"><span class="hlt">Non-thermal</span> plasma treatment is associated with changes in transcriptome of human epithelial skin cells.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary"><span class="hlt">Non-thermal</span> atmospheric pressure plasma has recently gained attention in the field of biomedical and clinical applications. In the area of plasma medicine research, one promising approach is to promote wound healing by stimulation of cells involved. To understand basic molecular and cellular mechanisms triggered by plasma treatment, we investigated biological effects of an argon plasma jet kinpen on human epithelial skin cells. For assessment of transcriptome changes cell culture medium was plasma treated and applied to the HaCaT keratinocyte cell culture (indirect treatment). Consequently, whole-genome microarrays were used to analyze this interaction in detail and identified a statistically significant modification of 3,274 genes including 1,828 up- and 1,446 downregulated genes. Particularly, cells after indirect plasma treatment are characterized by differential expression of a considerable number of genes involved in the response to stress. In this regard, we found a plasma-dependent regulation of oxidative stress answer and increased expression of enzymes of the antioxidative defense system (e.g. 91 oxidoreductases). Our results demonstrate that plasma not only induces cell reactions of stress-sensing but also of proliferative nature. Consistent with gene expression changes as well as Ingenuity Pathway Analysis prediction, we propose that stimulating doses of plasma may protect epithelial skin cells in wound healing by promoting proliferation and differentiation. In conclusion, gene expression profiling may become an important tool in identifying plasma-related changes of gene expression. Our results underline the enormous clinical potential of plasma as a biomedical tool for stimulation of epithelial skin cells. PMID:23668811</p> <div class="credits"> <p class="dwt_author">Schmidt, Anke; Wende, Kristian; Bekeschus, Sander; Bundscherer, Lena; Barton, Annemarie; Ottmüller, Katja; Weltmann, Klaus-Dieter; Masur, Kai</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-08-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">313</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2003AGUFM.P51B0451G"> <span id="translatedtitle"><span class="hlt">Non-thermal</span> production of molecular oxygen on the surface of Europa</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">The signature of condensed O2 has been reported in optical reflectance measurements of the Jovian moon Ganymede, and a tenuous oxygen atmosphere has been observed surrounding Europa. The surfaces of these moons contain large amounts of water ice, and it is thought that O2 is formed by sputtering of ice by energetic particles from the Jovian magnetosphere. Knowledge of how O2 is produced in low-temperature ice is crucial for accurate theoretical and experimental simulations of the surfaces and atmospheres of icy solar system bodies. However, the role of electronic excitations and the mechanistic details are poorly understood. This talk will present an overview of the <span class="hlt">non-thermal</span> processes involved in the production and build up of oxygen and related species in icy surfaces like that of Europa. Discussion will include laboratory measurements of the electron energy threshold, flux and fluence dependence, temperature dependence, and cross-section for O2 production during low-energy (5-100 eV) electron bombardment of thin (~40 bilayer) amorphous and crystalline D2O ice films in vacuum that are suitable surrogates of the conditions found on Europa. Comparison of the fluence dependence with kinetic models shows that O2 is formed by direct excitation and dissociation of a stable precursor molecule, and not by diffusion and chemical recombination of radicals. The O2 yield is also strongly dependent on the temperature of the ice, is different for crystalline and amorphous ice films, and shows structure indicative of bulk structural transitions. We also report a previously unobserved hysteresis with temperature cycling. The results point to a novel explanation of thermal effects in ice sputtering, based on a temperature dependence of the dissociative excited state lifetime of water.</p> <div class="credits"> <p class="dwt_author">Grieves, G.; Orlando, T.; Sieger, M.; Johnson, R. E.</p> <p class="dwt_publisher"></p> <p class="publishDate">2003-12-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">314</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/60078274"> <span id="translatedtitle">NOVEL COMPOSITE HYDROGEN-PERMEABLE MEMBRANES FOR <span class="hlt">NON-THERMAL</span> PLASMA REACTORS FOR THE DECOMPOSITION OF HYDROGEN SULFIDE</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">The goal of this experimental project is to design and fabricate a reactor and membrane test cell to dissociate hydrogen sulfide (HâS) in a <span class="hlt">non-thermal</span> plasma and recover hydrogen (Hâ) through a superpermeable multi-layer membrane. Superpermeability of hydrogen atoms (H) has been reported by some researchers using membranes made of Group V transition metals (niobium, tantalum, vanadium, and their alloys),</p> <div class="credits"> <p class="dwt_author">Morris D. Argyle; John F. Ackerman; Suresh Muknahallipatna; Jerry C. Hamann; Stanislaw Legowski; Ji-Jun Zhang; Guibing Zhao; Robyn J. Alcanzare; Linna Wang; Ovid A. Plumb</p> <p class="dwt_publisher"></p> <p class="publishDate">2004-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">315</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/58728866"> <span id="translatedtitle">Studies on a <span class="hlt">non-thermal</span> pulsed corona plasma between two parallel-plate electrodes in water</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">A <span class="hlt">non-thermal</span> plasma generated between two parallel-plate electrodes submerged in water was studied in this work. The surface of one of the stainless-steel electrodes (the cathode) was coated with a ceramic layer of Al2O3. This reactor cell was connected to a water cycle and the discharge was carried out in a closed loop and therefore an equilibrium was established during</p> <div class="credits"> <p class="dwt_author">M M Sein; Z Bin Nasir; U Telgheder; T C Schmidt</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">316</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/50586217"> <span id="translatedtitle">Comparison of Direct and Indirect Effects of <span class="hlt">Non-Thermal</span> Atmospheric Pressure Plasma on Bacteria and Mechanisms of Such Interaction</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">Summary form only given. <span class="hlt">Non-thermal</span> plasmas are already well-known for their sterilization ability; however, the mechanisms of this sterilization are under debate. Short and long-living active species and radicals produced by plasma, ultraviolet (UV) radiation in VUV and UVC bands, local thermal effects of micro-discharges, and bombardment by charged particles are all listed as potential candidates for sterilization of various</p> <div class="credits"> <p class="dwt_author">G. Fridman; A. Fridman; A. Gutsol; V. Vasilets; G. Friedman</p> <p class="dwt_publisher"></p> <p class="publishDate">2007-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">317</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/21579989"> <span id="translatedtitle">THE <span class="hlt">NON-THERMAL</span>, TIME-VARIABLE RADIO EMISSION FROM Cyg OB2 no. 5: A WIND-COLLISION REGION</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">The radio emission from the well-studied massive stellar system Cyg OB2 no. 5 is known to fluctuate with a period of 6.7 years between a low-flux state, when the emission is entirely of free-free origin, and a high-flux state, when an additional <span class="hlt">non-thermal</span> component (of hitherto unknown nature) appears. In this paper, we demonstrate that the radio flux of that <span class="hlt">non-thermal</span> component is steady on timescales of hours and that its morphology is arc-like. This shows that the <span class="hlt">non-thermal</span> emission results from the collision between the strong wind driven by the known contact binary in the system and that of an unseen companion on a somewhat eccentric orbit with a 6.7 year period and a 5-10 mas semimajor axis. Together with the previously reported wind-collision region located about 0.''8 to the northeast of the contact binary, so far Cyg OB2 no. 5 appears to be the only multiple system known to harbor two radio-imaged wind-collision regions.</p> <div class="credits"> <p class="dwt_author">Ortiz-Leon, Gisela N.; Loinard, Laurent; RodrIguez, Luis F.; Dzib, Sergio A. [Centro de Radiostronomia y Astrofisica, Universidad Nacional Autonoma de Mexico, Morelia 58089 (Mexico); Mioduszewski, Amy J., E-mail: g.ortiz@crya.unam.mx [National Radio Astronomy Observatory, 1003 Lopezville Road, Socorro, NM 87801 (United States)</p> <p class="dwt_publisher"></p> <p class="publishDate">2011-08-10</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">318</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2012pbdm.book..445K"> <span id="translatedtitle">Decontamination of Bacillus subtilis Spores in a Sealed Package Using a <span class="hlt">Non-thermal</span> Plasma System</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">The safety of packaged food and medical devices is a major concern to consumers and government officials. Recent inventions (PK-1 and PK-2) based on the principles of <span class="hlt">non-thermal</span>, atmospheric plasma has shown significant reduction in bacterial contamination inside a sealed package. The objective of this study was to evaluate the PK-1 and PK-2 systems in the reduction of Bacillus subtilis spores using packages containing air or modified atmosphere (MA) gas (65% O2/30% CO2/5% N2). The experimental design consisted of the following parameters: (1) two voltage conditions: 13.5 kV with 1.0 cm electrode gap (PK-1) and 80 kV with 4.5 cm electrode gap (PK-2), (2) two treatment conditions: inside and outside the field of ionization, (3) PK-1 and PK-2 optimized treatment times: 300 and 120 s, respectively, and (4) two package gas types: air and modified atmosphere (MA) gas (65% O2/30% CO2/5% N2). Measurements included: (1) bacterial reductions of Bacillus subtilis var. niger (B. atrophaeus), (2) ozone, nitrous oxides (NOx), and carbon monoxide concentrations, and (3) relative humidity. Bacillus subtilis (1.7 × 106/strip) were loaded into sterile uncovered petri dishes and treated with ionization generated in packages using air or MA gas blend. Samples were treated for 300 s (PK-1) or 120 s (PK-2) and stored at room ­temperature for 24 h. Results documented relative humidity (RH) ranged from 20% to 30%. After 300 s of PK-1 treatment (13.5 kV/44 W/1.0 cm gap), ozone concentrations were 6,000 ppm (air) and 7,500 ppm (MA). After 120 s of PK-2 treatment (80 kV/150 W/4.5 cm), ozone concentrations were 7,500 ppm (air) and 12,000 ppm (MA). Ozone and NOx concentrations were non-detect (ND) after 24 h. PK-1 carbon monoxide levels were <20 ppm (air) and <100 ppm (MA) after 24 h. The PK-2 carbon monoxide levels were <20 ppm (air) and <400 ppm (MA) after 24 h. Treatments showed reductions in spores of greater than 6 log10 after 24 h. Reductions were maintained without additional re-growth at 72 h. These results indicate that the PK-1 and PK-2 systems have the capacity to reduce Bacillus subtilis spores in an in-package ionization process.</p> <div class="credits"> <p class="dwt_author">Keener, Kevin M.; Jensen, J. L.; Valdramidis, V. P.; Byrne, E.; Connolly, J.; Mosnier, J. P.; Cullen, P. J.</p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">319</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3494719"> <span id="translatedtitle">Laser schlieren deflectometry for temperature analysis of filamentary <span class="hlt">non-thermal</span> atmospheric pressure plasma</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p class="result-summary">The heat convection generated by micro filaments of a self-organized <span class="hlt">non-thermal</span> atmospheric pressure plasma jet in Ar is characterized by employing laser schlieren deflectometry (LSD). It is demonstrated as a proof of principle, that the spatial and temporal changes of the refractive index n in the optical beam path related to the neutral gas temperature of the plasma jet can be monitored and evaluated simultaneously. The refraction of a laser beam in a high gradient field of n(r) with cylindrical symmetry is given for a general real refraction index profile. However, the usually applied Abel approach represents an ill-posed problem and in particular for this plasma configuration. A simple analytical model is proposed in order to minimize the statistical error. Based on that, the temperature profile, specifically the absolute temperature in the filament core, the FWHM, and the frequencies of the collective filament dynamics are obtained for non-stationary conditions. For a gas temperature of 700 K inside the filament, the presented model predicts maximum deflection angles of the laser beam of 0.3 mrad which is in accordance to the experimental results obtained with LSD. Furthermore, the experimentally obtained FWHM of the temperature profile produced by the filament at the end of capillary is (1.5 ± 0.2) mm, which is about 10 times wider than the visual radius of the filament. The obtained maximum temperature in the effluent is (450 ± 30) K and is in consistence with results of other techniques. The study demonstrates that LSD represents a useful low-cost method for monitoring the spatiotemporal behaviour of microdischarges and allows to uncover their dynamic characteristics, e.g., the temperature profile even for challenging diagnostic conditions such as moving thin discharge filaments. The method is not restricted to the miniaturized and self-organized plasma studied here. Instead, it can be readily applied to other configurations that produce measurable gradients of refractive index by local gas heating and opens new diagnostics prospects particularly for microplasmas.</p> <div class="credits"> <p class="dwt_author">Schafer, J.; Foest, R.; Reuter, S.; Kewitz, T.; Sperka, J.; Weltmann, K.-D.</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">320</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2012hcxa.confE..77W"> <span id="translatedtitle">Thermal and <span class="hlt">non-thermal</span> X-ray processes in the Galactic Centre</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Recent observations have demonstrated that a diverse range of processes contribute to the extended X-ray emission observed from the central 100pc of our Galaxy. The region to the north-east of Sgr A* is characterized by bright knots of 6.4-keV iron-line emission arising from the X-ray fluorescence of dense molecular material. The variability of this emission establishes X-ray illumination as the excitation mechanism and links the line emission directly to an associated <span class="hlt">non-thermal</span> continuum arising from the Thomson scattering of the incident X- ray photons. The Galactic Centre SMBH (Sgr A*) is the most likely origin of the X-ray flux and, in fact, the X-ray fluorescence provides a crude record of the outburst activity of Sgr A* over the past 150 years. Strong He-like and H-like iron-K line emission at 6.7 and 6.9 keV indicative of a very hot (~7 keV) thermal component is evident throughout the Galactic Centre. Recent work suggests the bulk of this emission can be explained in terms of the integrated emission of low-luminosity point sources (eg CVs). It now seems unlikely that the region is pervaded by a truly diffuse and highly energetic ultra-hot thermal plasma. Thermal emission at kT ~ 0.8 keV, traced by He-like Sulphur (2.4 keV) and Argon (3.1 keV) lines, is strongly concentrated in the same north-eastern region. This component most likely originates in multiple supernova explosions, although it is difficult to identify individual remnants within the region of enhanced surface brightness. For a few localized regions the He-like Fe/S ratio suggests a temperature closer to ~1.5 keV. Intriguingly one such X-ray hot-spot is spatially coincident with the so-called Radio Arc region, a site of cosmic-ray particle acceleration. Various aspects of the above picture will be reviewed in this talk.</p> <div class="credits"> <p class="dwt_author">Warwick, Bob; Heard, Victoria; Capelli, Renzo</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-09-01</p> </div> </div> </div> </div> <div id="filter_results_form" class="filter_results_form floatContainer" style="visibility: visible;"> <div style="width:100%" id="PaginatedNavigation" class="paginatedNavigationElement"> <a id="FirstPageLink" onclick='return showDiv("page_1");' href="#" title="First Page"> <img id="FirstPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.first.18x20.png" alt="First Page" /></a> <a id="PreviousPageLink" onclick='return showDiv("page_15");' href="#" title="Previous Page"> <img id="PreviousPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.previous.18x20.png" alt="Previous Page" /></a> <span id="PageLinks" class="pageLinks"> <span> <a onClick='return showDiv("page_1");' href="#">1</a> 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title="Next Page"> <img id="NextPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.next.18x20.png" alt="Next Page" /></a> <a id="LastPageLink" onclick='return showDiv("page_25.0");' href="#" title="Last Page"> <img id="LastPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.last.18x20.png" alt="Last Page" /></a> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">321</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/22093785"> <span id="translatedtitle">Laser schlieren deflectometry for temperature analysis of filamentary <span class="hlt">non-thermal</span> atmospheric pressure plasma</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">The heat convection generated by micro filaments of a self-organized <span class="hlt">non-thermal</span> atmospheric pressure plasma jet in Ar is characterized by employing laser schlieren deflectometry (LSD). It is demonstrated as a proof of principle, that the spatial and temporal changes of the refractive index n in the optical beam path related to the neutral gas temperature of the plasma jet can be monitored and evaluated simultaneously. The refraction of a laser beam in a high gradient field of n(r) with cylindrical symmetry is given for a general real refraction index profile. However, the usually applied Abel approach represents an ill-posed problem and in particular for this plasma configuration. A simple analytical model is proposed in order to minimize the statistical error. Based on that, the temperature profile, specifically the absolute temperature in the filament core, the FWHM, and the frequencies of the collective filament dynamics are obtained for non-stationary conditions. For a gas temperature of 700 K inside the filament, the presented model predicts maximum deflection angles of the laser beam of 0.3 mrad which is in accordance to the experimental results obtained with LSD. Furthermore, the experimentally obtained FWHM of the temperature profile produced by the filament at the end of capillary is (1.5 {+-} 0.2) mm, which is about 10 times wider than the visual radius of the filament. The obtained maximum temperature in the effluent is (450 {+-} 30) K and is in consistence with results of other techniques. The study demonstrates that LSD represents a useful low-cost method for monitoring the spatiotemporal behaviour of microdischarges and allows to uncover their dynamic characteristics, e.g., the temperature profile even for challenging diagnostic conditions such as moving thin discharge filaments. The method is not restricted to the miniaturized and self-organized plasma studied here. Instead, it can be readily applied to other configurations that produce measurable gradients of refractive index by local gas heating and opens new diagnostics prospects particularly for microplasmas.</p> <div class="credits"> <p class="dwt_author">Schaefer, J.; Foest, R.; Reuter, S.; Weltmann, K.-D. [INP Greifswald, Felix-Hausdorff-Str. 2, 17489 Greifswald (Germany); Kewitz, T. [Institute of Experimental and Applied Physics, University Kiel, 24098 Kiel (Germany); Sperka, J. [Department of Physical Electronics, Masaryk University, 61137 Brno (Czech Republic)</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-10-15</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">322</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/23126765"> <span id="translatedtitle">Laser schlieren deflectometry for temperature analysis of filamentary <span class="hlt">non-thermal</span> atmospheric pressure plasma.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">The heat convection generated by micro filaments of a self-organized <span class="hlt">non-thermal</span> atmospheric pressure plasma jet in Ar is characterized by employing laser schlieren deflectometry (LSD). It is demonstrated as a proof of principle, that the spatial and temporal changes of the refractive index n in the optical beam path related to the neutral gas temperature of the plasma jet can be monitored and evaluated simultaneously. The refraction of a laser beam in a high gradient field of n(r) with cylindrical symmetry is given for a general real refraction index profile. However, the usually applied Abel approach represents an ill-posed problem and in particular for this plasma configuration. A simple analytical model is proposed in order to minimize the statistical error. Based on that, the temperature profile, specifically the absolute temperature in the filament core, the FWHM, and the frequencies of the collective filament dynamics are obtained for non-stationary conditions. For a gas temperature of 700 K inside the filament, the presented model predicts maximum deflection angles of the laser beam of 0.3 mrad which is in accordance to the experimental results obtained with LSD. Furthermore, the experimentally obtained FWHM of the temperature profile produced by the filament at the end of capillary is (1.5 ± 0.2) mm, which is about 10 times wider than the visual radius of the filament. The obtained maximum temperature in the effluent is (450 ± 30) K and is in consistence with results of other techniques. The study demonstrates that LSD represents a useful low-cost method for monitoring the spatiotemporal behaviour of microdischarges and allows to uncover their dynamic characteristics, e.g., the temperature profile even for challenging diagnostic conditions such as moving thin discharge filaments. The method is not restricted to the miniaturized and self-organized plasma studied here. Instead, it can be readily applied to other configurations that produce measurable gradients of refractive index by local gas heating and opens new diagnostics prospects particularly for microplasmas. PMID:23126765</p> <div class="credits"> <p class="dwt_author">Schäfer, J; Foest, R; Reuter, S; Kewitz, T; Šperka, J; Weltmann, K-D</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-10-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">323</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2012RScI...83j3506S"> <span id="translatedtitle">Laser schlieren deflectometry for temperature analysis of filamentary <span class="hlt">non-thermal</span> atmospheric pressure plasma</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">The heat convection generated by micro filaments of a self-organized <span class="hlt">non-thermal</span> atmospheric pressure plasma jet in Ar is characterized by employing laser schlieren deflectometry (LSD). It is demonstrated as a proof of principle, that the spatial and temporal changes of the refractive index n in the optical beam path related to the neutral gas temperature of the plasma jet can be monitored and evaluated simultaneously. The refraction of a laser beam in a high gradient field of n(r) with cylindrical symmetry is given for a general real refraction index profile. However, the usually applied Abel approach represents an ill-posed problem and in particular for this plasma configuration. A simple analytical model is proposed in order to minimize the statistical error. Based on that, the temperature profile, specifically the absolute temperature in the filament core, the FWHM, and the frequencies of the collective filament dynamics are obtained for non-stationary conditions. For a gas temperature of 700 K inside the filament, the presented model predicts maximum deflection angles of the laser beam of 0.3 mrad which is in accordance to the experimental results obtained with LSD. Furthermore, the experimentally obtained FWHM of the temperature profile produced by the filament at the end of capillary is (1.5 +/- 0.2) mm, which is about 10 times wider than the visual radius of the filament. The obtained maximum temperature in the effluent is (450 +/- 30) K and is in consistence with results of other techniques. The study demonstrates that LSD represents a useful low-cost method for monitoring the spatiotemporal behaviour of microdischarges and allows to uncover their dynamic characteristics, e.g., the temperature profile even for challenging diagnostic conditions such as moving thin discharge filaments. The method is not restricted to the miniaturized and self-organized plasma studied here. Instead, it can be readily applied to other configurations that produce measurable gradients of refractive index by local gas heating and opens new diagnostics prospects particularly for microplasmas.</p> <div class="credits"> <p class="dwt_author">Schäfer, J.; Foest, R.; Reuter, S.; Kewitz, T.; Šperka, J.; Weltmann, K.-D.</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-10-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">324</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/22086408"> <span id="translatedtitle"><span class="hlt">NON-THERMAL</span> RESPONSE OF THE CORONA TO THE MAGNETIC FLUX DISPERSAL IN THE PHOTOSPHERE OF A DECAYING ACTIVE REGION</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">We analyzed Solar Dynamics Observatory line-of-sight magnetograms for a decaying NOAA active region (AR) 11451 along with co-temporal Extreme-Ultraviolet Imaging Spectrometer (EIS) data from the Hinode spacecraft. The photosphere was studied via time variations of the turbulent magnetic diffusivity coefficient, {eta}(t), and the magnetic power spectrum index, {alpha}, through analysis of magnetogram data from the Helioseismic and Magnetic Imager (HMI). These measure the intensity of the random motions of magnetic elements and the state of turbulence of the magnetic field, respectively. The time changes of the <span class="hlt">non-thermal</span> energy release in the corona was explored via histogram analysis of the <span class="hlt">non-thermal</span> velocity, v {sub nt}, in order to highlight the largest values at each time, which may indicate an increase in energy release in the corona. We used the 10% upper range of the histogram of v {sub nt} (which we called V {sup upp} {sub nt}) of the coronal spectral line of Fe XII 195 A. A 2 day time interval was analyzed from HMI data, along with the EIS data for the same field of view. Our main findings are the following. (1) The magnetic turbulent diffusion coefficient, {eta}(t), precedes the upper range of the v {sub nt} with the time lag of approximately 2 hr and the cross-correlation coefficient of 0.76. (2) The power-law index, {alpha}, of the magnetic power spectrum precedes V {sup upp} {sub nt} with a time lag of approximately 3 hr and the cross-correlation coefficient of 0.5. The data show that the magnetic flux dispersal in the photosphere is relevant to <span class="hlt">non-thermal</span> energy release dynamics in the above corona. The results are consistent with the nanoflare mechanism of the coronal heating, due to the time lags being consistent with the process of heating and cooling the loops heated by nanoflares.</p> <div class="credits"> <p class="dwt_author">Harra, L. K. [UCL-Mullard Space Science Laboratory, Holmbury St. Mary, Dorking, Surrey, RH5 6NT (United Kingdom); Abramenko, V. I. [Big Bear Solar Observatory, 40386 N. Shore Lane, Big Bear City, CA 92314 (United States)</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-11-10</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">325</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2009PhDT........23F"> <span id="translatedtitle">Modeling and simulations of DC and RF atmospheric pressure <span class="hlt">non-thermal</span> micro plasma discharges: Analysis and applications</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Atmospheric pressure <span class="hlt">non-thermal</span> plasma discharges are attractive for a wide range of applications due to their operational flexibility. Among the different atmospheric pressure <span class="hlt">non-thermal</span> plasma sources, atmospheric pressure <span class="hlt">non-thermal</span> micro plasma discharge is a very recent development. However, the micron scale size of these discharges makes it difficult to measure basic plasma characteristics (species density, gas and electron temperature, electric field etc) and also to analyze the different interplaying physico-chemical processes. In this work comprehensive multi-dimensional hybrid models were developed to simulate DC and RF atmospheric pressure <span class="hlt">non-thermal</span> plasma discharges, and validated against experimental data. The basic plasma characteristics and different physico-chemical processes were explored by performing systematic parameter variations. The developed discharge models included detailed discharge physics, gas phase chemistry, surface chemistry and external circuit model. DC micro plasma discharges in argon, hydrogen and methane-hydrogen gas were simulated. The effect of the external circuit was found to be crucial in predicting the discharge characteristics accurately. The simulations indicated the discharge to be operating as a 'normal' glow discharge. Predictions from the model compared favorably to the experimental measurements. A detailed surface chemistry model was developed for a DC methane-hydrogen micro glow to study the possibility of using these micro plasma discharges in plasma enhanced chemical vapor deposition. RF plasma discharges in argon gas together with an extensive external circuit was simulated; special attention was devoted to the effect of external circuit parameters on the discharge characteristics. The circuit elements were found to trigger change in the mode of operation. An atmospheric pressure plasma jet in helium-oxygen feed gas was also simulated to study the possibility of surface decontamination applications. To the author's knowledge, this is the first attempt where detailed simulation of atmospheric pressure micro plasma discharge has been conducted together with an external circuit. The discharge models were used to investigate the plasma characteristics, physico-chemical processes and study the effect of the external circuit and process parameters on the discharge. Better understanding of these processes will enable the tailoring and optimization of the operating conditions.</p> <div class="credits"> <p class="dwt_author">Farouk, Tanvir Iqbal</p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">326</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2008HEAD...10.2503W"> <span id="translatedtitle">The Continued Search for <span class="hlt">Non-thermal</span> Hard X-ray Emission in the Coma and Abell 3667 Galaxy Clusters</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">The X-ray bright, nearby galaxy clusters of Coma and Abell 3667 respectively host the brightest radio halo and the brightest radio relic known. These diffuse, Mpc-scale structures are due to synchrotron emission from relativistic electrons, which also produce inverse Compton (IC) emission that becomes competitive with thermal emission from the ICM at hard X-ray energies. Previous searches for IC emission from these radio structures have led to marginal and controversial detections due to background uncertainties and possible contaminating sources. The improved sensitivity and narrower FOV of the Suzaku PIN Hard X-ray Detector makes it an ideal instrument to search for hard X-ray IC emission. We present 180 ks and 95 ks Suzaku observations of the Coma and A3667 clusters, respectively, as well as mosaic XMM-Newton observations that cover the HXD-PIN field of view. Because these clusters' ICM is hot (T𕙟-8 keV), a clear detection of <span class="hlt">non-thermal</span> emission requires the thermal component within the same FOV to be completely assessed. XMM-Newton EPIC-PN spectra over the HXD field of view are weighted according to the spatial sensitivity of the HXD-PIN detector and combined so as to directly represent the HXD-detected thermal emission. The Suzaku PIN spectrum is simultaneously fit with this XMM spectrum for each cluster to pin down the thermal and <span class="hlt">non-thermal</span> components of the X-ray emission. While marginal <span class="hlt">non-thermal</span> components are detected in both clusters, they are not robust to variations of the HXD-PIN background within the systematic error. We derive conservative upper limits for the <span class="hlt">non-thermal</span> flux and corresponding lower limits for the average cluster magnetic field strength of both Coma and A3667. The results for Coma are consistent with other recent measurements and with equipartition estimates. For A3667, the lower limit on the magnetic field is rather high given the large projected cluster radius of the relic.</p> <div class="credits"> <p class="dwt_author">Wik, Daniel R.; Sarazin, C.; Nakazawa, K.; Finoguenov, A.; Kawaharada, M.; Kitaguchi, T.; Okuyama, S.; Matsushita, K.; Clarke, T.</p> <p class="dwt_publisher"></p> <p class="publishDate">2008-03-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">327</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2014PhST..161a4064S"> <span id="translatedtitle">Reformation of hydrocarbons using <span class="hlt">non-thermal</span> plasma at atmospheric pressure: discharge characteristics and associated nonlinear dynamics</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">This paper studies the atmospheric <span class="hlt">non-thermal</span> plasma generated in a hydrocarbon reforming system. Here, discharge is excited in a typically designed electrode configuration and has been carried out with four different combination pairs of electrodes. The plasma discharge is attained by applying high ac (pulsed) voltages between electrodes. The voltage–current characteristics have been studied in the system with respect to different electrode materials such as steel (SS304), copper and nickel. A Langmuir probe is used to measure fluctuations in the ion saturation region with all electrode configurations. The Hilbert transform technique and empirical mode decomposition have been used to understand the nonlinear dynamics of the fluctuation signals.</p> <div class="credits"> <p class="dwt_author">Sarma, Arun; Gopi, Supin; Saha, Debajyoti</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-05-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">328</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/41148568"> <span id="translatedtitle">Impact of selected combinations of <span class="hlt">non-thermal</span> processing technologies on the quality of an apple and cranberry juice blend</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">A blend of apple and cranberry juice was processed by a combination of a light-based technology (ultraviolet light (UV) (5.3J\\/cm2) or high intensity light pulses (HILP) (3.3J\\/cm2) in combination with pulsed electric fields (PEF) (34kV\\/cm, 18Hz, 93?s) or manothermosonication (MTS) (5bar, 43°C, 750W, 20kHz). Selected physical and chemical attributes were evaluated pre- and post-processing, and the sensory attributes of <span class="hlt">non-thermally</span></p> <div class="credits"> <p class="dwt_author">Irene M. Caminiti; Francesco Noci; Arantxa Muñoz; Paul Whyte; Desmond J. Morgan; Denis A. Cronin; James G. Lyng</p> <p class="dwt_publisher"></p> <p class="publishDate">2011-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">329</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=20020076304&hterms=thermal+emission&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D20%26Ntt%3Dthermal%2Bemission"> <span id="translatedtitle">A Search for Evidence of <span class="hlt">Non-Thermal</span> Emission from the Supernova Remnants 37A/B</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">The ADP grant NAG5-9211 entitled 'A Search for Evidence of <span class="hlt">Non-Thermal</span> Emission from the Supernova Remnants 37 A/B' was not used to support an analysis of the ASCA data for these two remnants because the ASCA mission ended before the remnants were observed. The grant was used to support similar research on two remnants in the Large Magellanic Cloud, N132D and N 103B. An analysis of the Chandra data for these two remnants exhibits some evidence of <span class="hlt">non-thermal</span> emission from small regions in the remnants. The X-ray spectra for these regions can not be adequately described by a single thermal X-ray emission model. However, if an X-ray synchrotron component is also included, the spectral data can be well described by the model and the values of the fit parameters are consistent with the values expected. These results were presented at the 199th Meeting of the American Astronomical Society. In summary, the grant has enabled us to strengthen the evidence that supernova remnants outside our Galaxy can also accelerate electrons to very-high energies. The results of this analysis will be published soon in the Astrophysical Journal,</p> <div class="credits"> <p class="dwt_author">Oliversen, R.</p> <p class="dwt_publisher"></p> <p class="publishDate">2002-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">330</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=2939732"> <span id="translatedtitle">Dentin surface treatment using a <span class="hlt">non-thermal</span> argon plasma brush for interfacial bonding improvement in composite restoration</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p class="result-summary">The objective of this study is to investigate the treatment effects of <span class="hlt">non-thermal</span> atmospheric gas plasmas on dentin surfaces for composite restoration. Extracted unerupted human third molars were used by removing the crowns and etching the exposed dentin surfaces with 35% phosphoric acid gel. The dentin surfaces were treated by using a <span class="hlt">non-thermal</span> atmospheric argon plasma brush for various durations. The molecular changes of the dentin surfaces were analyzed using FTIR/ATR and an increase in carbonyl groups on dentin surfaces was detected with plasma treated dentin. Adper Single Bond Plus adhesive and Filtek Z250 dental composite were applied as directed. To evaluate the dentin/composite interfacial bonding, the teeth thus prepared were sectioned into micro-bars as the specimens for tensile test. Student Newman Keuls tests showed that the bonding strength of the composite restoration to peripheral dentin was significantly increased (by 64%) after 30 s plasma treatment. However, the bonding strength to plasma treated inner dentin did not show any improvement. It was found that plasma treatment of peripheral dentin surface up to 100 s gave an increase in interfacial bonding strength, while a prolong plasma treatment of dentin surfaces, e.g., 5 min treatments, showed a decrease in interfacial bonding strength.</p> <div class="credits"> <p class="dwt_author">Ritts, Andy Charles; Li, Hao; Yu, Qingsong; Xu, Changqi; Yao, Xiaomei; Hong, Liang; Wang, Yong</p> <p class="dwt_publisher"></p> <p class="publishDate">2010-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">331</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4049833"> <span id="translatedtitle"><span class="hlt">Non-Thermal</span> Plasma Treatment Diminishes Fungal Viability and Up-Regulates Resistance Genes in a Plant Host</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p class="result-summary">Reactive oxygen and nitrogen species can have either harmful or beneficial effects on biological systems depending on the dose administered and the species of organism exposed, suggesting that application of reactive species can possibly produce contradictory effects in disease control, pathogen inactivation and activation of host resistance. A novel technology known as atmospheric-pressure <span class="hlt">non-thermal</span> plasma represents a means of generating various reactive species that adversely affect pathogens (inactivation) while simultaneously up-regulating host defense genes. The anti-microbial efficacy of this technology was tested on the plant fungal pathogen Fusarium oxysporum f.sp. lycopersici and its susceptible host plant species Solanum lycopercicum. Germination of fungal spores suspended in saline was decreased over time after exposed to argon (Ar) plasma for 10 min. Although the majority of treated spores exhibited necrotic death, apoptosis was also observed along with the up-regulation of apoptosis related genes. Increases in the levels of peroxynitrite and nitrite in saline following plasma treatment may have been responsible for the observed spore death. In addition, increased transcription of pathogenesis related (PR) genes was observed in the roots of the susceptible tomato cultivar (S. lycopercicum) after exposure to the same Ar plasma dose used in fungal inactivation. These data suggest that atmospheric-pressure <span class="hlt">non-thermal</span> plasma can be efficiently used to control plant fungal diseases by inactivating fungal pathogens and up-regulating mechanisms of host resistance.</p> <div class="credits"> <p class="dwt_author">Panngom, Kamonporn; Lee, Sang Hark; Park, Dae Hoon; Sim, Geon Bo; Kim, Yong Hee; Uhm, Han Sup; Park, Gyungsoon; Choi, Eun Ha</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">332</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/24911947"> <span id="translatedtitle"><span class="hlt">Non-thermal</span> plasma treatment diminishes fungal viability and up-regulates resistance genes in a plant host.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">Reactive oxygen and nitrogen species can have either harmful or beneficial effects on biological systems depending on the dose administered and the species of organism exposed, suggesting that application of reactive species can possibly produce contradictory effects in disease control, pathogen inactivation and activation of host resistance. A novel technology known as atmospheric-pressure <span class="hlt">non-thermal</span> plasma represents a means of generating various reactive species that adversely affect pathogens (inactivation) while simultaneously up-regulating host defense genes. The anti-microbial efficacy of this technology was tested on the plant fungal pathogen Fusarium oxysporum f.sp. lycopersici and its susceptible host plant species Solanum lycopercicum. Germination of fungal spores suspended in saline was decreased over time after exposed to argon (Ar) plasma for 10 min. Although the majority of treated spores exhibited necrotic death, apoptosis was also observed along with the up-regulation of apoptosis related genes. Increases in the levels of peroxynitrite and nitrite in saline following plasma treatment may have been responsible for the observed spore death. In addition, increased transcription of pathogenesis related (PR) genes was observed in the roots of the susceptible tomato cultivar (S. lycopercicum) after exposure to the same Ar plasma dose used in fungal inactivation. These data suggest that atmospheric-pressure <span class="hlt">non-thermal</span> plasma can be efficiently used to control plant fungal diseases by inactivating fungal pathogens and up-regulating mechanisms of host resistance. PMID:24911947</p> <div class="credits"> <p class="dwt_author">Panngom, Kamonporn; Lee, Sang Hark; Park, Dae Hoon; Sim, Geon Bo; Kim, Yong Hee; Uhm, Han Sup; Park, Gyungsoon; Choi, Eun Ha</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">333</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2014ApJ...789...49F"> <span id="translatedtitle">Three-dimensional Simulations of the <span class="hlt">Non-thermal</span> Broadband Emission from Young Supernova Remnants Including Efficient Particle Acceleration</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Supernova remnants are believed to be major contributors to Galactic cosmic rays. In this paper, we explore how the <span class="hlt">non-thermal</span> emission from young remnants can be used to probe the production of energetic particles at the shock (both protons and electrons). Our model couples hydrodynamic simulations of a supernova remnant with a kinetic treatment of particle acceleration. We include two important back-reaction loops upstream of the shock: energetic particles can (1) modify the flow structure and (2) amplify the magnetic field. As the latter process is not fully understood, we use different limit cases that encompass a wide range of possibilities. We follow the history of the shock dynamics and of the particle transport downstream of the shock, which allows us to compute the <span class="hlt">non-thermal</span> emission from the remnant at any given age. We do this in three dimensions, in order to generate projected maps that can be compared with observations. We observe that completely different recipes for the magnetic field can lead to similar modifications of the shock structure, although to very different configurations of the field and particles. We show how this affects the emission patterns in different energy bands, from radio to X-rays and ?-rays. High magnetic fields (>100 ?G) directly impact the synchrotron emission from electrons, by restricting their emission to thin rims, and indirectly impact the inverse Compton emission from electrons and also the pion decay emission from protons, mostly by shifting their cut-off energies to respectively lower and higher energies.</p> <div class="credits"> <p class="dwt_author">Ferrand, Gilles; Decourchelle, Anne; Safi-Harb, Samar</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-07-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">334</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=20070018790&hterms=Sobczak&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D10%26Ntt%3DSobczak%2BE."> <span id="translatedtitle"><span class="hlt">Quasi-Periodic</span> Variability in NGC 5408 X-1</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">We report the discovery with XMM-Newton of quasiperiodic variability in the 0.2 - 10 keV X-ray flux from the ultraluminous X-ray source NGC 5408 X-1. The average power spectrum of all EPIC-pn data reveals a strong 20 mHz QPO with an average amplitude (rms) of 9%, and a coherence, Q identical with nu(sub 0)/sigma approximately equal to 6. In a 33 ksec time interval when the 20 mHz QPO is strongest we also find evidence for a 2nd QPO peak at 15 mHz, the first indication for a close pair of QPOs in a ULX source. Interestingly, the frequency ratio of this QPO pair is inconsistent with 3:2 at the 3 sigma level, but is consistent with a 4:3 ratio. A powerlaw noise component with slope near 1.5 is also present below 0.1 Hz with evidence for a break to a flatter slope at about 3 mHz. The source shows substantial broadband variability, with a total amplitude (rms) of about 30% in the 0.1 - 100 mHz frequency band, and there is strong energy dependence to the variability. The power spectrum of hard X-ray photons (greater than 2 keV) shows a "classic" flat-topped continuum breaking to a power law with index 1.5 - 2. Both the break and 20 mHz QPO are detected in the hard band, and the 20 mHz QPO is essentially at the break. The QPO is both strong and narrow in this band, having an amplitude (rms) of 15%, and Q approx. equal to 25. The energy spectrum is well fit by three components, a "cool" disk with kT = 0.15 keV, a steep power law with index 2.56, and a thermal plasma at kT = 0.87 keV. The disk, power law, and thermal plasma components contribute 35, 60, and 5% of the 0.3 - 10 keV flux, respectively. Both the timing and spectral properties of NGC 5408 X-1 are strikingly reminiscent of Galactic black hole systems at high inferred accretion rates, but with its characteristic frequencies (QPO and break frequencies) scaled down by a factor of 10 - 100. We discuss the implications of these findings in the context of models for ULXs, and their implications for the object's mass.</p> <div class="credits"> <p class="dwt_author">Strohmayer, Tod E.; Mushotzky, Richard F.; Winter, Lisa; Soria, Roberto; Uttley, Phil; Cropper, Mark</p> <p class="dwt_publisher"></p> <p class="publishDate">2007-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">335</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/50419957"> <span id="translatedtitle">Rapid 3-D electromagnetic simulation of <span class="hlt">quasi-periodic</span> structures</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">We describe a new 3-D electromagnetic simulation technique capable of fast, accurate modeling of complex cavity\\/waveguide structures. The method subdivides the structure into sections that can be analyzed independently, using 3-D finite element modeling then reassembled to compute a reduced-order matrix representation of Maxwell's equations. Eigensolutions of the reduced order matrix equations correspond to eigenmodes of the complete 3-D structure,</p> <div class="credits"> <p class="dwt_author">S. J. Cooke; B. Levush</p> <p class="dwt_publisher"></p> <p class="publishDate">2005-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">336</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/50652793"> <span id="translatedtitle">Multifractal properties of one dimension <span class="hlt">quasi-period</span> photonic crystal</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">Using transfer matrix method and multi-fractal theory, we studied the transmission properties of one-dimensional generalized Fibonacci structures GF(m,n), in which m, n different intervals are integer according to a substitution rule. By using a transfer-matrix method, the optical transmission through GF(m,n) is obtained. Multi-fractal analysis is employed to characterize the transmission spectra. It is demonstrated that the transmission coefficient has</p> <div class="credits"> <p class="dwt_author">Yuannong Zhang; Rui Zhou</p> <p class="dwt_publisher"></p> <p class="publishDate">2008-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">337</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/servlets/purl/10160974"> <span id="translatedtitle">Electrochemical synthesis of <span class="hlt">quasi-periodic</span> quantum dot arrays</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">The conventional route to nanosynthesis involves beam nanolithography (electron beam, ion beam or-x-ray lithography). Exposure to these beams during pattern delineation however causes severe radiation damage to nanostructures which is further compounded during later post-processing such as reactive ion etching. Consequently, finished nanostructures become replete with traps, vacancies, spurious charges and surface states. To circumvent this problem, we are developing a ``gentle`` electrochemical technique for the fabrication of periodic quantum dot arrays. It does not damage the structures through harsh processing steps, offers a minimum feature size down to {approximately} 40 {Angstrom}, allows the fabrication of structures on non-planar surfaces (e.g. spherical or cylindrical substrates), is amenable to mass production (millions of wafers can be processed simultaneously) and is potentially orders of magnitude cheaper than conventional nanofabrication. This paper describes initial results and show that this technique bears significant promise for future applications in nanostructure synthesis.</p> <div class="credits"> <p class="dwt_author">Miller, A.E.; Yue, D.F.; Banerjee, G.; Bandyopadhyay, S. [Univ. of Notre Dame, Notre Dame, IN (United States). Dept. of Electrical Engineering; Ricker, R.E.; Jones, S. [National Inst. of Standards and Technology, Gaithersburg, MD (United States). Materials Science and Engineering Laboratory; Eastman, J.A. [Argonne National Lab., IL (United States)</p> <p class="dwt_publisher"></p> <p class="publishDate">1994-06-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">338</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=19820029715&hterms=tilt+earth&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D40%26Ntt%3Dtilt%2Bearth"> <span id="translatedtitle"><span class="hlt">Quasi-periodic</span> climatic changes on Mars and earth</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">Evidence of climatic changes on Mars and the earth due to geologic and astronomical variations is discussed. Finely striped ice-free bands in the Martian polar caps have been taken to indicate that long term variations in the orbit and axial tilt of Mars have precipitated these features at the rate of a mm/yr. Photogrammetric and photometric methods have contributed to measurements of the composition and depth of the Martian caps (14-46 m), and observations of higher solar energy absorption in the northern ice cap implies greater dust deposition in that region than on the south cap; however, the transport mechanisms are not well understood. Comparisons of earth and Martian climatic variations data are made, noting a lack of information on the age intervals of marine and nonmarine sediments on the earth. The possibilities of using quantitative data other than layer thickness to constrain climate models are discussed, and the slope or albedo of layers, or the spacing of polar undulations are suggested.</p> <div class="credits"> <p class="dwt_author">Cutts, J. A.; Pollack, J. B.; Toon, O. B.; Howard, A. D.</p> <p class="dwt_publisher"></p> <p class="publishDate">1981-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">339</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ntis.gov/search/product.aspx?ABBR=N8633120"> <span id="translatedtitle"><span class="hlt">Quasi-Periodic</span> Hopf-Bifurcations in Forced Oscillators.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ntis.gov/search/index.aspx">National Technical Information Service (NTIS)</a></p> <p class="result-summary">The modified differential equation of Deffing-Van der Pol for nonlinear vibrations (Stoker's problem) is studied as an autonomous system or as a vector field over a certain phase-space (one forced oscillator over the product of n-dimensional real torus by...</p> <div class="credits"> <p class="dwt_author">H. W. Broer</p> <p class="dwt_publisher"></p> <p class="publishDate">1985-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">340</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ntis.gov/search/product.aspx?ABBR=DE94014013"> <span id="translatedtitle">Electrochemical synthesis of <span class="hlt">quasi-periodic</span> quantum dot arrays.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ntis.gov/search/index.aspx">National Technical Information Service (NTIS)</a></p> <p class="result-summary">The conventional route to nanosynthesis involves beam nanolithography (electron beam, ion beam or-x-ray lithography). Exposure to these beams during pattern delineation however causes severe radiation damage to nanostructures which is further compounded d...</p> <div class="credits"> <p class="dwt_author">A. E. Miller D. F. Yue G. Banerjee S. Bandyopadhyay R. E. Ricker</p> <p class="dwt_publisher"></p> <p class="publishDate">1994-01-01</p> </div> </div> </div> </div> <div id="filter_results_form" class="filter_results_form floatContainer" style="visibility: visible;"> <div style="width:100%" id="PaginatedNavigation" class="paginatedNavigationElement"> <a id="FirstPageLink" onclick='return showDiv("page_1");' href="#" title="First Page"> <img id="FirstPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.first.18x20.png" alt="First Page" /></a> <a id="PreviousPageLink" onclick='return showDiv("page_16");' href="#" title="Previous Page"> <img id="PreviousPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.previous.18x20.png" alt="Previous Page" /></a> <span id="PageLinks" class="pageLinks"> <span> <a onClick='return showDiv("page_1");' href="#">1</a> <a onClick='return showDiv("page_2");' href="#">2</a> <a onClick='return showDiv("page_3");' href="#">3</a> <a onClick='return showDiv("page_4");' 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onclick='return showDiv("page_25.0");' href="#" title="Last Page"> <img id="LastPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.last.18x20.png" alt="Last Page" /></a> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">341</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2004ThCFD..18..221M"> <span id="translatedtitle"><span class="hlt">Quasi-periodicity</span> and chaos in a differentially heated cavity</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Convective flows of a small Prandtl number fluid contained in a two-dimensional vertical cavity subject to a lateral thermal gradient are studied numerically. The chosen geometry and the values of the material parameters are relevant to semiconductor crystal growth experiments in the horizontal configuration of the Bridgman method. For increasing Rayleigh numbers we find a transition from a steady flow to periodic solutions through a supercritical Hopf bifurcation that maintains the centro-symmetry of the basic circulation. For a Rayleigh number of about ten times that of the Hopf bifurcation, the periodic solution loses stability in a subcritical Neimark Sacker bifurcation, which gives rise to a branch of quasiperiodic states. In this branch, several intervals of frequency locking have been identified. Inside the resonance horns the stable limit cycles lose and gain stability via some typical scenarios in the bifurcation of periodic solutions. After a complicated bifurcation diagram of the stable limit cycle of the 1:10 resonance horn, a soft transition to chaos is obtained.</p> <div class="credits"> <p class="dwt_author">Mercader, Isabel; Batiste, Oriol; Ruiz, Xavier</p> <p class="dwt_publisher"></p> <p class="publishDate">2004-11-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">342</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2011epsc.conf..638K"> <span id="translatedtitle">Excitation and Propagation of Jovian <span class="hlt">Quasi-Periodic</span> Radio Bursts</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">We discussed the source location, directivity, and propagation process of QP bursts based on the ray tracing analysis, comparing with the observation results, especially with the latitudinal beaming and shadow zone [Kimura et al., 2010]. The parametric survey indicated that QP bursts observed at high and low latitudes have the source region at 2-10 Rj altitude along high-latitudinal field lines (L>20). It was suggested that these QP bursts have significantly broadened beaming patterns like a "filled cone".</p> <div class="credits"> <p class="dwt_author">Kimura, T.; Misawa, H.; Morioka, A.; Tsuchiya, F.; Kasaba, Y.; Cecconi, B.; Zarka, P.; MacDowall, R. J.; Hess, R. A.</p> <p class="dwt_publisher"></p> <p class="publishDate">2011-10-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">343</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2006ApSS..253..600A"> <span id="translatedtitle">A <span class="hlt">non-thermal</span> lattice gas model for a dimer trimer reaction on a catalytic surface: A computer simulation study</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">The kinetics of an irreversible dimer-trimer reaction of the type 3A 2 + 2B 3 ? 6AB have been studied using a <span class="hlt">non-thermal</span> (precursor mechanism) model on a square as well as on a hexagonal lattice surface by Monte Carlo simulation. When the range of the precursors (A atoms) is increased, the model gives production rates (reactive window widths) that are quite large as compared with those for thermal (Langmuir-Hanshelwood mechanism) model. The phase diagrams qualitatively resemble with the standard ZGB model except that the continuous transition point is eliminated when the range of the precursors is extended up to the third nearest neighbourhood. The diffusion of A atoms on the surface as well as their desorption from the surface with a certain probability is also considered to see their effects on the reaction mechanism.</p> <div class="credits"> <p class="dwt_author">Ahmad, Waqar; Parvez, M.; Baloach, Musa Kaleem; Qaisrani, A. U.; Khalid, M.</p> <p class="dwt_publisher"></p> <p class="publishDate">2006-11-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">344</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2014CPL...607...15T"> <span id="translatedtitle">Investigate the microscopic properties and the <span class="hlt">non-thermal</span> effect of the electrolyte solution under microwave irradiation</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Non-equilibrium molecular dynamics (NMD) simulations are performed to investigate the microscopic properties and the <span class="hlt">non-thermal</span> effect of microwave irradiation on NaCl electrolyte solution at different temperatures using the SPC/E model. The electromagnetic wave propagates in the z-axis direction with a frequency of 2.45 GHz, and the intensity of the E/H field is 3.4 × 104 V/m. The results indicate that as the concentration of the electrolyte solution increased, the electrical conductivity gradually increased, but the hydrogen bonds number and the coordination number decreased. In addition, the change of conductivity decreases with the increase of temperature when electromagnetic field is applied.</p> <div class="credits"> <p class="dwt_author">Tian, Wen-Yan; Huang, Ka-Ma; Yang, Li-Jun; Guo, Yi-Na; Liu, Feng-Hai</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-06-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">345</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2013APS..MAR.V1342G"> <span id="translatedtitle"><span class="hlt">Non-thermal</span> excitation and control of dynamic magnetization in a Fe/GaAs heterojunction by ultrafast laser pulses</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Control carrier injection in metal semiconductor heterojunctions and therefore their magnetic dynamics is a major challenge in modern solid-state electronic devices. We report on our recent study of <span class="hlt">non-thermally</span> excitation and coherently control the spin reorientation by utilizing low-energy femtosecond laser pulses to induce a photo- current through a Fe/GaAs interface. The magnetization dynamics and hysteresis curves were recorded by the pump-probe differential magnetic Kerr (DMK) technique. We show that magnetization excitation and reorientation strongly depend on the polarization of pump pulses. A clear four-fold switching is identified in DMK signal when we rotate the polarization of pump pulses. Our results show that the dynamic magnetization can be induced and controlled by ultrafast laser pulses, and therefore indicate the feasibility of next generation femtosecond-switching magnetic storage devices.</p> <div class="credits"> <p class="dwt_author">Gong, Yu; Kutayiah, A. R.; Cevher, Z.; Zhang, X. H.; Zhao, J. H.; Ren, Y. H.</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-03-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">346</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2002AIPC..636..111P"> <span id="translatedtitle">Atmospheric Pollutant Removal by <span class="hlt">Non-Thermal</span> Plasmas: Basic Data Needs for Understanding and Optimization of the Process</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Since fifteen years, an increasing interest has been devoted to removal of atmospheric pollutant by <span class="hlt">non-thermal</span> plasmas achieved using e-beams or pulsed discharges, for the nitrous oxides the so-called de-NOx process, or for Volatils Organic Compounds, the so-called de-VOC process. However the physical and chemical mechanisms involved are not easy to understand: molecules or gas mixtures are quite complex, and the transient plasma created by the type of discharge often used, dielectric barrier or corona ones, is non homogeneous in space. In this paper is discussed some data needs for understanding of the NO-removal process and the destruction of some selected VOC molecules, TCE and TCA, by pulsed discharge plasmas. Some experimental studies performed to get insight into the discharge plasma kinetic involved in the pollutant removal are presented, in particular about the hydroxyl radical OH which play an important role in this kinetic.</p> <div class="credits"> <p class="dwt_author">Pasquiers, S.; Cormier, M.; Motret, O.</p> <p class="dwt_publisher"></p> <p class="publishDate">2002-10-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">347</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/21434398"> <span id="translatedtitle">[Dependence of the <span class="hlt">non-thermal</span> radiofrequency electromagnetic field bioeffects on the typological features of electroencephalogram in humans].</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">In researches with participation of volunteers bioeffects of short-term <span class="hlt">non-thermal</span> radiofrequency electromagnetic field (RF EMF) exposure were studied. The basic form of brain's reaction was the amplification of energy in a-range in electroencephalogram (EEG) spectra. Dependence of these changes, not only due to the changes of the exposure parameters, but also due to personal EEG typological features was shown. Moderate degree of the alpha frequencies domination in the background promoted development of reaction of a brain to the RF EMF exposure. To a lesser degree it was shown at hyperactivity of this range and, practically, was absent in the conditions of theta- or beta2-range domination in the EEG background with the open and closed eyes. The combination of RF EMF exposure and monotonous activity has authentically strengthened result, keeping the basic form of reaction (energy amplification in the alpha range of EEG spectrum) and dependence on EEG typological features. PMID:21434398</p> <div class="credits"> <p class="dwt_author">Luk'ianova, S N; Grigor'ev, Iu G; Grigor'ev, O A; Merkulov, A V</p> <p class="dwt_publisher"></p> <p class="publishDate">2010-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">348</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2005PhDT........27Y"> <span id="translatedtitle">Investigation of atmospheric pressure capillary <span class="hlt">non-thermal</span> plasmas and their applications to the degradation of volatile organic compounds</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Atmospheric pressure capillary <span class="hlt">non-thermal</span> plasma (AP-CNTP) has been investigated as a potential technology far the removal of volatile organic compounds (VOCs) in Advanced Life Support Systems (ALS). AP-CNTP is a destructive technology far the removal of VOCs from air streams by active plasma species, such as electrons, ions, and excited molecules. Complete VOC destruction ideally results in the formation of water, carbon dioxide (CO2), and other by-product's may also form, including ozone (O3), nitrous oxide (N2O), nitrogen dioxide (NO2), and decomposed hydrocarbons. Several organic compounds, such as BTEX, ethylene, n-heptane, isooctane, methanol and NH3, were tested in an AP-CNTP system. Parametric experiments were carried out by varying plasma discharge power, flowrates, and initial concentrations. The degradation efficiency varied depending on the chemical nature of the compounds. A plasmochemical kinetic model was derived for toluene, ethylbenzene, and m-xylene and n-heptane.</p> <div class="credits"> <p class="dwt_author">Yin, Shu-Min</p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">349</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/49220907"> <span id="translatedtitle">Combined effect of selected <span class="hlt">non-thermal</span> technologies on Escherichia coli and Pichia fermentans inactivation in an apple and cranberry juice blend and on product shelf life</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">The combination of novel, <span class="hlt">non-thermal</span> technologies for preservation purposes is a recent trend in food processing research. In the present study, <span class="hlt">non-thermal</span> hurdles such as ultraviolet light (UV) (5.3J\\/cm2), high intensity light pulses (HILP) (3.3J\\/cm2), pulsed electric fields (PEF) (34kV\\/cm, 18Hz, 93?s) or manothermosonication (MTS) (4bar, 43°C, 750W, 20kHz) were examined. The objective was to establish the potential of these</p> <div class="credits"> <p class="dwt_author">I. Palgan; I. M. Caminiti; A. Muñoz; F. Noci; P. Whyte; D. J. Morgan; D. A. Cronin; J. G. Lyng</p> <p class="dwt_publisher"></p> <p class="publishDate">2011-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">350</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2010A%26A...519A.111B"> <span id="translatedtitle"><span class="hlt">Non-thermal</span> radio emission from O-type stars. IV. Cygnus OB2 No. 8A</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Context. Several early-type colliding-wind binaries are known to emit synchrotron radiation due to relativistic electrons, which are most probably accelerated by the Fermi mechanism. By studying such systems we can learn more about this mechanism, which is also relevant in other astrophysical contexts. Colliding-wind binaries are furthermore important for binary frequency determination in clusters and for understanding clumping and porosity in stellar winds. Aims: We study the <span class="hlt">non-thermal</span> radio emission of the binary Cyg OB2 No. 8A, to see if it is variable and if that variability is locked to the orbital phase. We investigate if the synchrotron emission generated in the colliding-wind region of this binary can explain the observations and we verify that our proposed model is compatible with the X-ray data. Methods: We use both new and archive radio data from the Very Large Array (VLA) to construct a light curve as a function of orbital phase. We also present new X-ray data that allow us to improve the X-ray light curve. We develop a numerical model for the colliding-wind region and the synchrotron emission it generates. The model also includes free-free absorption and emission due to the stellar winds of both stars. In this way we construct artificial radio light curves and compare them with the observed one. Results: The observed radio fluxes show phase-locked variability. Our model can explain this variability because the synchrotron emitting region is not completely hidden by the free-free absorption. In order to obtain a better agreement for the phases of minimum and maximum flux we need to use stellar wind parameters for the binary components which are somewhat different from typical values for single stars. We verify that the change in stellar parameters does not influence the interpretation of the X-ray light curve. Our model has trouble explaining the observed radio spectral index. This could indicate the presence of clumping or porosity in the stellar wind, which - through its influence on both the Razin effect and the free-free absorption - can considerably influence the spectral index. <span class="hlt">Non-thermal</span> radio emitters could therefore open a valuable pathway to investigate the difficult issue of clumping in stellar winds. Partly based on observations with XMM-Newton, an ESA Science Mission with instruments and contributions directly funded by ESA Member States and the USA (NASA).Appendices are only available in electronic form at http://www.aanda.org</p> <div class="credits"> <p class="dwt_author">Blomme, R.; De Becker, M.; Volpi, D.; Rauw, G.</p> <p class="dwt_publisher"></p> <p class="publishDate">2010-09-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">351</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ntis.gov/search/product.aspx?ABBR=DE2006878291"> <span id="translatedtitle">Novel Composite Hydrogen-Permeable Membranes for <span class="hlt">Non-Thermal</span> Plasma Reactors for the Decomposition of Hydrogen Sulfide. Annual Report, October 1, 2004-September 30, 2005.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ntis.gov/search/index.aspx">National Technical Information Service (NTIS)</a></p> <p class="result-summary">The goal of this experimental project is to design and fabricate a reactor and membrane test cell to dissociate hydrogen sulfide (H2S) in a <span class="hlt">non-thermal</span> plasma and recover hydrogen (H2) through a superpermeable multi-layer membrane. Superpermeability of hy...</p> <div class="credits"> <p class="dwt_author">M. D. Argyle J. F. Ackerman S. Muknahallipatna J. C. Hamann S. Legowski</p> <p class="dwt_publisher"></p> <p class="publishDate">2005-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">352</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/22047127"> <span id="translatedtitle">Electrostatic solitary structures in presence of <span class="hlt">non-thermal</span> electrons and a warm electron beam on the auroral field lines</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">Electrostatic solitary waves (ESWs) have been observed by satellites in the auroral region of the Earth's magnetosphere. These ESWs are found to be having both positive and negative electrostatic potentials. Using the Sagdeeev psuedo-potential technique, arbitrary amplitude electron-acoustic solitary waves/double layers are studied in an unmagnetized plasma consisting of <span class="hlt">non-thermally</span> distributed hot electrons, fluid cold electrons, a warm electron beam, and ions. The inertia of the warm electrons, and not the beam speed, is essential for the existence of positive potential solitary structures. Existence domains for positive as well as negative potential electrostatic solitons/double layers are obtained. For the typical auroral region parameters, the electric field amplitude of the negative potential solitons is found to be in the range {approx}(3-30) mV/m and {approx}(5-80) mV/m for the positive potential solitons. For the negative potential solitons/double layers, the amplitudes are higher when their widths are smaller. On the other hand, the amplitude of the positive potential structures increase with their widths.</p> <div class="credits"> <p class="dwt_author">Singh, S. V. [Indian Institute of Geomagnetism, Navi Mumbai (India); School of Physics, University of Kwazulu-Natal, Durban (South Africa); Lakhina, G. S. [Indian Institute of Geomagnetism, Navi Mumbai (India); Bharuthram, R. [University of the Western Cape, Bellville (South Africa); Pillay, S. R. [School of Physics, University of Kwazulu-Natal, Durban (South Africa)</p> <p class="dwt_publisher"></p> <p class="publishDate">2011-12-15</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">353</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2012Nanot..23y5604Y"> <span id="translatedtitle">Silicon nanocrystal production through <span class="hlt">non-thermal</span> plasma synthesis: a comparative study between silicon tetrachloride and silane precursors</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Silicon nanocrystals with sizes between 5 and 10 nm have been produced in a <span class="hlt">non-thermal</span> plasma reactor using silicon tetrachloride as precursor. We demonstrate that high-quality material can be produced with this method and that production rates as high as 140 mg h-1 can be obtained, with a maximum precursor utilization rate of roughly 50%. Compared to the case in which particles are produced using silane as the main precursor, the gas composition needs to be modified and hydrogen needs to be added to the mixture to enable the nucleation and growth of the powder. The presence of chlorine in the system leads to the production of nanoparticles with a chlorine terminated surface which is significantly less robust against oxidation in air compared to the case of a hydrogen terminated surface. We also observe that significantly higher power input is needed to guarantee the formation of crystalline particles, which is a consequence not only of the different gas-phase composition, but also of the influence of chlorine on the stability of the crystalline structure.</p> <div class="credits"> <p class="dwt_author">Yasar-Inceoglu, Ozgul; Lopez, Thomas; Farshihagro, Ebrahim; Mangolini, Lorenzo</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-06-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">354</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=19900002982&hterms=instructive+case&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D20%26Ntt%3Dinstructive%2Bcase"> <span id="translatedtitle">The behavior of beams of relativistic <span class="hlt">non-thermal</span> electrons under the influence of collisions and synchrotron losses</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">For many astrophysical situations, such as in solar flares or cosmic gamma-ray bursts, continuum gamma rays with energies up to hundreds of MeV were observed, and can be interpreted to be due to bremsstrahlung radiation by relativistic electrons. The region of acceleration for these particles is not necessarily the same as the region in which the radiation is produced, and the effects of the transport of the electrons must be included in the general problem. Hence it is necessary to solve the kinetic equation for relativistic electrons, including all the interactions and loss mechanisms relevant at such energies. The resulting kinetic equation for <span class="hlt">non-thermal</span> electrons, including the effects of Coulomb collisions and losses due to synchrotron emission, was solved analytically in some simple limiting cases, and numerically for the general cases including constant and varying background plasma density and magnetic field. New approximate analytic solutions are presented for collision dominated cases, for small pitch angles and all energies, synchrotron dominated cases, both steady-state and time dependent, for all pitch angles and energies, and for cases when both synchrotron and collisional energy losses are important, but for relativistic electrons. These analytic solutions are compared to the full numerical results in the proper limits. These results will be useful for calculation of spectra and angular distribution of the radiation (x rays, gamma-rays, and microwaves) emitted via synchrotron or bremsstrahlung processes by the electrons. These properties and their relevance to observations will be observed in subsequent papers.</p> <div class="credits"> <p class="dwt_author">Mctiernan, James M.; Petrosian, Vahe</p> <p class="dwt_publisher"></p> <p class="publishDate">1989-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">355</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/servlets/purl/827748"> <span id="translatedtitle">A COMPACT CORONA DISCHARGE DEVICE (CDD{trademark}) FOR <span class="hlt">NON-THERMAL</span> PLASMA GENERATION IN GASOLINE OR DIESEL ENGINE EXHAUST</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">Higher fuel economy targets and hybrid vehicles are increasing the marketability of diesel engines. But in order to implement the growth of diesels to achieve the fuel economy benefits, all emission regulation issues must be met. To do this traps and catalysts are being utilized. One of the main problems is finding a technology that enables the exhaust emission system to not only meet the emission requirements when new, but also to meet them at the regulated intermediate and full life requirements. Work is being done that enables catalysts to remain highly efficient throughout their full life. It is done by using a corona discharge device (CDD{trademark}) that introduces <span class="hlt">non-thermal</span> plasma into the exhaust ahead of the converter. This low power device creates radicals that alter the chemistry of the exhaust so as to limit the poisoning of the catalyst. This can be done without so called ''purge'' cycles that lower fuel economy and degrade catalyst long-term durability. This device has been developed, not as a laboratory tool, but as a production ready product and is the first of its kind that is commercially available for testing. It is this product, the Corona Discharge Device, CDD{trademark}, which will be described.</p> <div class="credits"> <p class="dwt_author">Nowak,Victor J.</p> <p class="dwt_publisher"></p> <p class="publishDate">2000-08-20</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">356</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2011JCAP...12..002P"> <span id="translatedtitle">Non-minimal Higgs inflation and <span class="hlt">non-thermal</span> leptogenesis in a supersymmetric Pati-Salam model</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">We consider a supersymmetric (SUSY) Grand Unified Theory (GUT) based on the gauge group GPS = SU(4)C × SU(2)L × SU(2)R, which incorporates non-minimal chaotic inflation, driven by a quartic potential associated with the Higgs fields involved in the spontaneous breaking of GPS. The inflationary model relies on renormalizable superpotential terms and does not lead to overproduction of magnetic monopoles. It is largely independent of the one-loop radiative corrections and can become consistent with the current observational data on the inflationary observables, with the symmetry breaking scale of GPS assuming its SUSY value. Within our model, the strong CP and the ? problems of the minimal SUSY standard model can be resolved via a Peccei-Quinn symmetry. Moreover baryogenesis occurs via <span class="hlt">non-thermal</span> leptogenesis realized by the out-of-equilibrium decay of the right-handed neutrinos, which are produced by the inflaton's decay. We consider two versions of such a scenario, assuming that the inflaton decays to the lightest or to the next-to-lightest right-handed neutrino. Both scenaria can become compatible with the constraints arising from the baryon asymmetry of the universe, the gravitino limit on the reheating temperature and the upper bound on the light neutrino masses, provided that the gravitino is somehow heavy. In the second scenario, extra restrictions from the SU(4)C GUT symmetry on the heaviest Dirac neutrino mass and the data on the atmospheric neutrino oscillations can be also met.</p> <div class="credits"> <p class="dwt_author">Pallis, C.; Toumbas, N.</p> <p class="dwt_publisher"></p> <p class="publishDate">2011-12-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">357</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/19348341"> <span id="translatedtitle">Compatibility studies of promethazine hydrochloride with tablet excipients by means of thermal and <span class="hlt">non-thermal</span> methods.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">The compatibility of promethazine hydrochloride (PMZ) with various tableting excipients has been investigated by isothermal stress testing (IST) and differential scanning calorimetry (DSC). DSC thermograms of PMZ and each of the excipients investigated were compared with their corresponding physical mixtures (1:1) for evaluation. Furthermore, Fourier transform infrared spectroscopy (FTIR) data was used to corroborate the results of DSC and IST. A preliminary sustained release tablet formulation of the drug, prepared using compatible excipients, was stored under accelerated storage conditions (40 degrees C/75% RH) and analyzed for stability, drug release and bioadhesion characteristics for up to 3 months. Based on DSC results alone, drug-excipient interactions were observed with Pearlitol SD200, lactose monohydrate and zinc stearate. Chromatographic analysis of the stressed binary mixture (stored at 55 degrees C for 3 weeks) containing PMZ-lactose monohydrate showed brown discoloration indicating potential interaction. However, stressed physical mixtures of PMZ-Pearlitol SD200 and PMZ-zinc stearate indicated compatibility as opposed to the thermal analysis. The tablet formulation was found to be very stable after 3 months of storage at accelerated stability conditions. Also, the release profiles and bioadhesive properties were found to be unaltered. Thus, both thermal and <span class="hlt">non-thermal</span> methods were utilized to successfully evaluate the compatibility of excipients with PMZ and the tablet formulation was found to be stable. PMID:19348341</p> <div class="credits"> <p class="dwt_author">Thumma, S; Repka, M A</p> <p class="dwt_publisher"></p> <p class="publishDate">2009-03-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">358</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/20017624"> <span id="translatedtitle">The <span class="hlt">non</span> <span class="hlt">thermal</span> effect of weak intensity millimeter waves on physicochemical properties of water and water solutions.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">The comparative study of the effects of 5.8 mW/cm(2) Millimeter Waves (MMW) and near Infrared (IR) irradiation on thermal properties, specific adsorption rate (SAR), specific electrical conductivity (SEC) and hydrogen peroxide (H(2)O(2)) content of distilled water (DW), and physiological solutions (PS) was performed. The thermal effect of MMW irradiation appeared only after the first minute of irradiation, while the IR heating started from the first minute of irradiation. The heat fusion of frozen MMW-treated DW and PS was significantly less than sham and IR-treated DW and PS. MMW irradiation had time-dependent elevation effect on water SEC and SAR, which was accompanied by the increase of H(2)O(2) formation in it. We suggest that the MMW-induced vibration of water dipole molecules caused the <span class="hlt">non</span> <span class="hlt">thermal</span> changes of physicochemical properties of DW and PS, which promote the formation of H(2)O(2) in water. PMID:20017624</p> <div class="credits"> <p class="dwt_author">Ayrapetyan, Gayane; Hayrapetyan, Hovik; Dadasyan, Erna; Barseghyan, Sedrak; Baghdasaryan, Naira; Mikayelyan, Erazik; Ayrapetyan, Sinerik</p> <p class="dwt_publisher"></p> <p class="publishDate">2009-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">359</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2014JAP...115c3303X"> <span id="translatedtitle">Characteristics of atmospheric-pressure <span class="hlt">non-thermal</span> N2 and N2/O2 gas mixture plasma jet</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">An atmospheric-pressure <span class="hlt">non-thermal</span> plasma jet driven by high frequency alternating current and operating on N2 and N2/O2 gas mixture is investigated. The plasma jet can reach 55 mm in length at a gas flow rate of 2500 l/h. The gas temperature at a distance of 4 mm from the nozzle is close to room temperature. Optical emission spectroscopy is employed to investigate the important plasma parameters such as the excited species, rotational temperature, vibrational temperature, and excitation temperature under different discharge conditions. The results show that the plasma source operates under non-equilibrium conditions. The absolute irradiance intensity of the vibrational band N2(C-B) in the active region is measured. Taking into account the irradiance intensity of N2(C-B,0-0) and N2(B-X,0-0) as well as measured current, the electron density, which is determined by considering direct and step-wise electron impact excitation of nitrogen emission, reaches a maximum value of 5.6 × 1020/m3.</p> <div class="credits"> <p class="dwt_author">Xiao, Dezhi; Cheng, Cheng; Shen, Jie; Lan, Yan; Xie, Hongbing; Shu, Xingsheng; Meng, Yuedong; Li, Jiangang; Chu, Paul K.</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">360</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3393702"> <span id="translatedtitle">Inactivation of Candida Biofilms by <span class="hlt">Non-Thermal</span> Plasma and Its Enhancement for Fungistatic Effect of Antifungal Drugs</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p class="result-summary">We investigated the antifungal effect of <span class="hlt">non-thermal</span> plasma, as well as its combination with common antifungal drugs, against Candida biofilms. A direct current atmospheric pressure He/O2 (2%) plasma microjet (PMJ) was used to treat Candida biofilms in a 96-well plate. Inactivation efficacies of the biofilms were evaluated by XTT assay and counting colony forming units (CFUs). Morphological properties of the biofilms were evaluated by Scanning Electron Microscope (SEM). The sessile minimal inhibitory concentrations (SMICs) of fluconazole, amphotericin B, and caspofungin for the biofilms were also tested. Electron Spin Resonance (ESR) spectroscopy was used to detect the reactive oxygen species (ROS) generated directly and indirectly by PMJ. The Candida biofilms were completely inactivated after 1 min PMJ treatment, where severely deformed fungal elements were observed in SEM images. The SMICs of the tested antifungal drugs for the plasma-treated biofilms were decreased by 2–6 folds of dilution, compared to those of the untreated controls. ROS such as hydroxyl radical (•OH), superoxide anion radical (•O2-) and singlet molecular oxygen (1O2) were detected by ESR. We hence conclude that He/O2 (2%) plasma alone, as well as in combination with common antifungal drugs, is able to inactivate Candida biofilms rapidly. The generation of ROS is believed to be one of the underlying mechanisms for the fungicidal activity of plasma.</p> <div class="credits"> <p class="dwt_author">Sun, Peng; Wu, Haiyan; Zhu, Weidong; Liu, Wei; Zhang, Jue; Fang, Jing; Li, Ruoyu</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-01-01</p> </div> </div> </div> </div> <div id="filter_results_form" class="filter_results_form floatContainer" style="visibility: visible;"> <div style="width:100%" id="PaginatedNavigation" class="paginatedNavigationElement"> <a id="FirstPageLink" onclick='return showDiv("page_1");' href="#" title="First Page"> <img id="FirstPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.first.18x20.png" alt="First Page" /></a> <a id="PreviousPageLink" onclick='return showDiv("page_17");' href="#" title="Previous Page"> <img id="PreviousPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.previous.18x20.png" alt="Previous Page" /></a> <span id="PageLinks" 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id="NextPageLink" onclick='return showDiv("page_20");' href="#" title="Next Page"> <img id="NextPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.next.18x20.png" alt="Next Page" /></a> <a id="LastPageLink" onclick='return showDiv("page_25.0");' href="#" title="Last Page"> <img id="LastPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.last.18x20.png" alt="Last Page" /></a> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">361</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/21054557"> <span id="translatedtitle"><span class="hlt">Non-thermal</span> atmospheric-pressure plasma can influence cell adhesion molecules on HaCaT-keratinocytes.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary"><span class="hlt">Non-thermal</span> atmospheric-pressure plasmas provide new hope for improvement in chronic wound management because of their potency in killing microorganisms. However, the effectiveness of the procedure has to be verified and negative effects on healthy tissues have to be excluded. In wound healing adhesion molecules play a crucial role for cell migration and proliferation. We investigated whether an atmospheric-pressure plasma jet (kINPen09) influences the expression of adhesion molecules responsible for cell-cell and cell-matrix interactions after treatment of HaCaT-keratinocytes for 10 and 30 s. Twenty-four hours after plasma treatment expression of ?(2) - and ?(1)-integrin, E-cadherin and the epidermal growth factor receptor (EGFR) was determined by flow cytometry. Plasma-treated HaCaT-cells were characterized by normal ?(2)-integrin and increased ?(1)-integrin expression. E-cadherin and EGFR expression was reduced after the 30-s treatment. We did not observe any effects following the 10-s plasma treatment. In conclusion, short-term plasma treatment can be applied without effects for cell-cell and cell-matrix adhesion. PMID:21054557</p> <div class="credits"> <p class="dwt_author">Haertel, Beate; Wende, Kristian; von Woedtke, Thomas; Weltmann, Klaus Dieter; Lindequist, Ulrike</p> <p class="dwt_publisher"></p> <p class="publishDate">2011-03-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">362</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/18763534"> <span id="translatedtitle">[Effects of gas compositions on the oxidation of gas phase elementary mercury by <span class="hlt">non-thermal</span> plasma].</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">The effects of flue gas compositions such as NO, SO2, CO, H2O on elementary mercury oxidation by <span class="hlt">non-thermal</span> plasma induced by positive streamer discharge were experimentally investigated by using a link tooth wheel-cylinder reactor. The results showed that the oxidation of elementary mercury decreased in the presence of CO2 and NO, which was attributed to the reduction of number of the active radicals reacted with elementary mercury. Adding 670 mg/m3 NO, only 37% elementary mercury was oxidized when the voltage was 9.5 kV. And CO was produced because of the reaction between CO2 and active radicals. The presence of SO2 resulted in an increase of elementary mercury oxidation, and white HgSO4 and Hg2SO4 were formed, little elementary mercury was detected at the outlet of the reactor when the voltage was 10 kV. Similarly, H2O and HCI promoted the oxidation of elementary mercury, which may be due to the formation of oxidative *OH and the presence of Cl- ions. The total mercury concentration dramatically decreased after the discharge reactor because the charging mercury was collected. PMID:18763534</p> <div class="credits"> <p class="dwt_author">Tang, Ping; Zhu, Tian-le; Li, Huan; Luo, Hong-jing; Li, Jing</p> <p class="dwt_publisher"></p> <p class="publishDate">2008-06-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">363</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2014JPhD...47w5402L"> <span id="translatedtitle">Development of hydrophilic dental wax without surfactant using a <span class="hlt">non-thermal</span> air atmospheric pressure plasma jet</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Dental wax (DW), a low-melting and high-molecular-weight organic mixture, is widely used in dentistry for forming moulds of teeth. Hydrophilicity is an important property for DW, as a wet dental investment is used to surround the wax before wax burnout is performed. However, recent attempts to improve the hydrophilicity of DW using a surfactant have resulted in the reduced mechanical properties of the dental investment, leading to the failure of the dental restoration. This study applied a <span class="hlt">non-thermal</span> air atmospheric pressure plasma jet (AAPPJ) for DW surface treatment and investigated its effect on both DW hydrophilicity and the dental investment's mechanical properties. The results showed that the application of the AAPPJ significantly improved the hydrophilicity of the DW, and that the results were similar to that of cleaner-treated DW using commercially available products with surfactant. A surface chemical analysis indicated that the improvement of hydrophilicity was related to an increase in the number of oxygen-related bonds on the DW surface following the removal of carbon hydrate in both AAPPJ and cleaner-treated DW. However, cleaner treatment compromised the mechanical property of the dental investment when the dental investment was in contact with the treated DW, while the AAPPJ treatment did not. Therefore, the use of AAPPJ to treat DW is a promising method for accurate dental restoration, as it induces an improvement in hydrophilicity without harming the dental investment.</p> <div class="credits"> <p class="dwt_author">Lee, Jung-Hwan; Kim, Yong-Hee; Choi, Eun-Ha; Kim, Kwang-Mahn; Kim, Kyoung-Nam</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-06-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">364</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2012JPhD...45v5203S"> <span id="translatedtitle">Studies on a <span class="hlt">non-thermal</span> pulsed corona plasma between two parallel-plate electrodes in water</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">A <span class="hlt">non-thermal</span> plasma generated between two parallel-plate electrodes submerged in water was studied in this work. The surface of one of the stainless-steel electrodes (the cathode) was coated with a ceramic layer of Al2O3. This reactor cell was connected to a water cycle and the discharge was carried out in a closed loop and therefore an equilibrium was established during discharge. The dependence of hydrogen peroxide formation as an indicator for the generation of most important oxidative species OH radicals on the pulse repetition rate, the solution conductivity and the pH of the solution was investigated. The highest yield of H2O2 (3.5 mg L-1) was obtained at 20 pps in a NaCl solution with a conductivity of 400 µS cm-1 and pH 7 in 90 min. The maximum energy efficiency of ˜0.1 g kWh-1 H2O2 was obtained. The surface of the coated electrodes, before and after applying of electrical discharges, was analysed by scanning electron microscopy. During the discharge process, the coating was destroyed and the formation of H2O2 decreased to 10% after discharging of nearly 35 h.</p> <div class="credits"> <p class="dwt_author">Sein, M. M.; Nasir, Z. Bin; Telgheder, U.; Schmidt, T. C.</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-06-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">365</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/servlets/purl/827866"> <span id="translatedtitle">NO{sub X} REDUCTION BEHAVIOR OF ALUMINA AND ZEOLITE CATALYSTS IN COMBINATION WITH <span class="hlt">NON-THERMAL</span> PLASMA</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">Lean burn gasoline and diesel engines provide improved fuel economy when compared to engines operating under stoichiometric fuel/air conditions. At the same time, lean burn and diesel engines present a problem for emission control. Because they operate under oxidizing conditions, the conventional three-way catalyst is not effective in NOx reduction [1,2]. In addition, the wide temperature range of automobile exhaust gases present a challenge for catalyst design. The temperature of exhaust gases from a light duty diesel engine can vary from 150 to 500 C, depending on the operating conditions. To date, a catalyst that operates with high NOx conversion efficiency over the entire operating range has not been found. <span class="hlt">Non-thermal</span> plasma assisted catalysis has been shown to be a promising technology for NOx reduction in lean burn and diesel exhaust gases [3,4]. The approach exploited in this paper is to use a plasma in combination with several catalysts, each of which are active over unique temperature ranges. It was reported in the literature, that the one of the essential roles of plasma treatment is to oxidize NO to easier reducible NO2 [7]. In this contribution, the other important function of plasma treatment, namely partial oxidation of propylene, will be demonstrated.</p> <div class="credits"> <p class="dwt_author">Panov, A.G.</p> <p class="dwt_publisher"></p> <p class="publishDate">2000-08-20</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">366</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/21893360"> <span id="translatedtitle">Combined effect of selected <span class="hlt">non-thermal</span> technologies on Escherichia coli and Pichia fermentans inactivation in an apple and cranberry juice blend and on product shelf life.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">The combination of novel, <span class="hlt">non-thermal</span> technologies for preservation purposes is a recent trend in food processing research. In the present study, <span class="hlt">non-thermal</span> hurdles such as ultraviolet light (UV) (5.3 J/cm²), high intensity light pulses (HILP) (3.3 J/cm²), pulsed electric fields (PEF) (34 kV/cm, 18 Hz, 93 ?s) or manothermosonication (MTS) (4bar, 43 °C, 750 W, 20 kHz) were examined. The objective was to establish the potential of these technologies, applied individually or in paired sequences, to inactivate Escherichia coli and Pichia fermentans inoculated in a fresh blend of apple and cranberry juice. The shelf-life evaluation of selected <span class="hlt">non-thermally</span> treated samples was conducted over 35 days and compared to pasteurised samples and untreated juices. All treatments applied individually significantly reduced (1.8-6.0 log cfu/ml) microbial counts compared to the untreated sample (p<0.01). Furthermore, UV treatment produced significantly greater inactivation (p<0.05) for E. coli compared to P. fermentans. Combinations of <span class="hlt">non-thermal</span> hurdles consisting of UV or HILP followed by either PEF or MTS resulted in comparable reductions for both microorganisms (p ? 0.05) to those observed in thermally pasteurised samples (approx. 6 log cfu/ml). Thermally pasteurised samples had a shelf life exceeding 35 days, while that of UV+PEF and HILP+PEF-treated samples was 14 and 21 days, respectively. These results indicate that combinations of these <span class="hlt">non-thermal</span> technologies could successfully reduce levels of E. coli and P. fermentans in apple and cranberry juice, although optimisation is required in order to further extend shelf life. PMID:21893360</p> <div class="credits"> <p class="dwt_author">Palgan, I; Caminiti, I M; Muñoz, A; Noci, F; Whyte, P; Morgan, D J; Cronin, D A; Lyng, J G</p> <p class="dwt_publisher"></p> <p class="publishDate">2011-11-15</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">367</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=20030020814&hterms=supernovae&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D90%26Ntt%3Dsupernovae"> <span id="translatedtitle">A Study of the <span class="hlt">Non-Thermal</span> X-Ray Emission of Shell-Type Supernova Remnants</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">We present an analysis of the X-ray spectrum of the Galactic shell-type SNR G347.3-0.5 (RX 51713.7-3946). This SNR is a member of a growing class of SNRs which are dynamically young, shell-type sources that emit <span class="hlt">non-thermal</span> X-rays from specific regions on their outer shells. By performing a joint spectral analysis of data from observations made of G347.3-0.5 using the ROSAT PSPC, the ASCA GIS and the RXTE PCA, we have fit the spectra of particular regions of this SNR (including the bright northwestern and southwestern rims, the northeast rim and the interior diffuse emission) over the approximate energy range of 0.5 through 30 keV. We find that fits to the spectra of this SNR over this energy range using the SRCUT model were superior to a simple power law model or the SRESC model. We find that the inclusion of a thermal model with the SRCUT model helps to improve the fit to the observed X-ray spectrum: this represents the first detection of thermal X-ray emission from G347.3-0.5. Thermal emission appears to be more clearly associated with the diffuse emission in the interior of the SNR than with the bright X-ray emitting rims. A weak emission feature seen near 6.4 keV in the RXTE PCA spectrum most likely originates from diffuse X-ray emission from the surrounding Galactic Ridge rather than from G347.3-0.5 itself. We have analyzed our RXTE PCA data to search for pulsations from a recently discovered radio pulsar (PSR 51713-3949) which may be associated with G347.3-0.5, and we do not detect any X-ray pulsations at the measured radio period of 392 ms. Using the best-fit parameters obtained from the SRCUT model, we estimate the maximum energy of cosmic-ray electrons accelerated by the rims of G347.3-0.5 to be 19-25 TeV (assuming a magnetic field strength of B = 10muG), consistent with the results of Ellison et al. We present a broadband (radio to gamma ray) photon energy-flux spectrum for the northwestern rim of G347.3-0.5, where we have fit the spectrum using a more sophisticated synchrotron-inverse Compton model with a variable magnetic field strength. Our fit derived from this model yields a maximum energy of only 8.8 (+4.1) (-3.4) TeV for the accelerated cosmic-ray electrons and a much greater magnetic field strength of 150 (+250) (-80). Finally, we compare the gross properties of G347.3-0.5 with other SNRs known to possess X-ray spectra dominated by <span class="hlt">non-thermal</span> emission.</p> <div class="credits"> <p class="dwt_author">Allen, Glenn E.</p> <p class="dwt_publisher"></p> <p class="publishDate">2003-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">368</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2009SPIE.7380E..91M"> <span id="translatedtitle">Novel <span class="hlt">non-thermal</span> atrial fibrillation treatment with photosensitization reaction: possibility of permanent electrical blockade in rat chronic model</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">We demonstrated a possibility of electrical conduction block by ex vivo and in vivo experiments using rat models to establish a <span class="hlt">non-thermal</span> treatment for atrial fibrillation by photosensitization reaction (PR). One hour after the injection of 2 mg/kg Talaporfin sodium to Wistar rat, the right ventricle (1.4 mmT) was extracted. Paced with a stimulation electrode, this tissue was placed in a tissue bath and immersed in irrigated Tyrode's solution of 37°C with 8 ?g/ml Talaporfin sodium and the gas mixture bubbling of 95% CO2 and 5% O2. The propagated electrical signal was measured by two bipolar electrodes. Exciting light of 670 nm in wavelength was irradiated to the tissue between the bipolar electrodes by the power density of 1 W/cm2. After this irradiation, propagation signal blockade was obtained and continued up to three hours. Rat atrioventricular (AV) node was employed as a target region for chronic model. The heart of Wistar rat was surgically exposed. External four-lead electrocardiogram of this rat was measured. Thirty minutes after the injection of 10 mg/kg Talaporfin sodium to the rat, exciting light of 663 nm in wavelength was irradiated to the AV node by the power density of 500 mW/cm2 for ten minutes. Acute AV block was obtained during the irradiation. Two weeks after this procedure, complete AV block was confirmed. The rat was sacrificed to obtain the tissue specimen. We found that the AV node was replaced by scarring tissue under the microscopic observation of the specimen. We verified possibility of permanent electrical conduction block using PR.</p> <div class="credits"> <p class="dwt_author">Matsuo, Hiroki; Ito, Arisa; Miyoshi, Shunichiro; Soejima, Kyoko; Ogawa, Satoshi; Arai, Tsunenori</p> <p class="dwt_publisher"></p> <p class="publishDate">2009-06-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">369</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/24613643"> <span id="translatedtitle">The <span class="hlt">non-thermal</span> effects of pulsed ultrasound irradiation on the development of disuse muscle atrophy in rat gastrocnemius muscle.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">This study examined the effects of therapeutic pulsed ultrasound (US) on the development of disuse muscle atrophy in rat gastrocnemius muscle. Male Wistar rats were randomly distributed into control, immobilization (Im), sham US, and US groups. In the Im, sham US and US groups, the bilateral ankle joints of each rat were immobilized in full plantar flexion with a plaster cast for a 4-wk period. The pulsed US (frequency, 1 MHz; intensity, 1.0 W/cm(2); pulsed mode 1:4; 15 min) was irradiated to the gastrocnemius muscle in the US group over a 4-wk immobilization period. The pulsed US irradiation delivered only <span class="hlt">non-thermal</span> effects to the muscle. In conjunction with US irradiation, 5-bromo-2'-deoxyuridine (BrdU) was injected subcutaneously to label the nuclei of proliferating satellite cells 1 h before each pulsed US irradiation. Immobilization resulted in significant decreases in the mean diameters of type I, IIA and IIB muscle fibers of the gastrocnemius muscle in the Im, sham US and US groups compared with the control group. However, the degrees of muscle fiber atrophy for all types were significantly lower in the US group compared with the Im and sham US groups. Although the number of capillaries and the concentrations of insulin-like growth factor and basic fibroblast growth factor did not change in the muscle, the number of BrdU-positive nuclei in the muscle was significantly increased by pulsed US irradiation in the US group. The results of this study suggest that pulsed US irradiation inhibits the development of disuse muscle atrophy partly via activation of satellite cells. PMID:24613643</p> <div class="credits"> <p class="dwt_author">Matsumoto, Yoko; Nakano, Jiro; Oga, Satoshi; Kataoka, Hideki; Honda, Yuichiro; Sakamoto, Junya; Okita, Minoru</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-07-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">370</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3881910"> <span id="translatedtitle">High-efficiency tooth bleaching using <span class="hlt">non-thermal</span> atmospheric pressure plasma with low concentration of hydrogen peroxide</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p class="result-summary">Light-activated tooth bleaching with a high hydrogen peroxide (HP; H2O2) concentration has risks and the actual role of the light source is doubtful. The use of conventional light might result in an increase in the temperature and cause thermal damage to the health of the tooth tissue. Objective: This study investigated the efficacy of tooth bleaching using <span class="hlt">non-thermal</span> atmospheric pressure plasma (NAPP) with 15% carbamide peroxide (CP; CH6N2O3) including 5.4% HP, as compared with conventional light sources. Material and Methods: Forty human teeth were randomly divided into four groups: Group I (CP+NAPP), Group II (CP+plasma arc lamp; PAC), Group III (CP+diode laser), and Group IV (CP alone). Color changes (?E ) of the tooth and tooth surface temperatures were measured. Data were evaluated by one-way analysis of variance (ANOVA) and post-hoc Tukey's tests. Results: Group I showed the highest bleaching efficacy, with a ?E value of 1.92-, 2.61 and 2.97-fold greater than those of Groups II, III and IV, respectively (P<0.05). The tooth surface temperature was maintained around 37ºC in Group I, but it reached 43ºC in Groups II and III. Conclusions: The NAPP has a greater capability for effective tooth bleaching than conventional light sources with a low concentration of HP without causing thermal damage. Tooth bleaching using NAPP can become a major technique for in-office bleaching in the near future.</p> <div class="credits"> <p class="dwt_author">NAM, Seoul Hee; LEE, Hyun Woo; CHO, Soo Hyun; LEE, Jae Koo; JEON, Young Chan; KIM, Gyoo Cheon</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">371</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2011SPIE.7897E..14D"> <span id="translatedtitle">Characterizing temperature-dependent photo-oxidation to explain the abrupt transition from thermal to <span class="hlt">non-thermal</span> laser damage mechanisms at 413 nm</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Laser exposure duration dictates whether tissues subjected to short visible wavelengths ( <= 514 nm) are damaged by thermal (e.g. 0.1 s) or <span class="hlt">non-thermal</span> ( >= 100 s) mechanisms. Somewhere between these extremes, an abrupt transition between the two damage mechanisms has been found for both in vitro and animal retinal models (J. Biomed. Opt. 15, 030512, 2010). <span class="hlt">Non-thermal</span> (photochemical) damage is characterized by an inverse relationship between damage threshold irradiance and exposure duration (irradiance reciprocity). We have found that exposures of 40 - 60 s in an in vitro retinal model require radiant exposures well above the expected requirement for nonthermal damage, introducing the concept that damage was forced to be thermal in mechanism. Here we quantify and compare photo-oxidative processes at ambient temperatures between 35 - 50 °C.</p> <div class="credits"> <p class="dwt_author">Denton, Michael L.; Clark, C. D., III; Noojin, Gary D.; Estlack, Larry E.; Schenk, Adam C.; Burney, Curtis W.; Rockwell, Benjamin A.; Thomas, Robert J.</p> <p class="dwt_publisher"></p> <p class="publishDate">2011-02-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">372</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/55871067"> <span id="translatedtitle">Higher-order growth rate of instability of obliquely propagating kinetic Alfvén and ion-acoustic solitons in a magnetized <span class="hlt">non-thermal</span> plasma</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">The higher-order growth rate of instability for obliquely propagating kinetic Alfvén and ion-acoustic solitons in a magnetized <span class="hlt">non-thermal</span> plasma have been obtained by the multiple-scale perturbation expansion method developed by Allen and Rowlands (1993). The growth rate of instability is obtained correct to order k2, where k is the wave number of a long-wavelength plane-wave perturbation. The corresponding lowest-order stability</p> <div class="credits"> <p class="dwt_author">Anup Bandyopadhyay; K. P. Das</p> <p class="dwt_publisher"></p> <p class="publishDate">2001-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">373</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/19454589"> <span id="translatedtitle">Ion-acoustic solitons and double-layers in a plasma consisting of positive and negative ions with <span class="hlt">non-thermal</span> electrons</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">In this research paper, the authors have studied the properties of ion-acoustic solitons and double-layers in a plasma consisting of warm positive and negative ions with different concentration of masses, charged states and <span class="hlt">non-thermal</span> electrons using small amplitude approximation. Reductive perturbation method is used to derive KdV and m-KdV equations. Existence of ion-acoustic solitons and double-layer is explored over a</p> <div class="credits"> <p class="dwt_author">T. S. Gill; P. Bala; H. Kaur; N. S. Saini; S. Bansal; J. Kaur</p> <p class="dwt_publisher"></p> <p class="publishDate">2004-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">374</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/23408366"> <span id="translatedtitle">Effect of thermal and <span class="hlt">non-thermal</span> pasteurisation on the microbial inactivation and phenolic degradation in fruit juice: a mini-review.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">Fruit juice has been traditionally preserved by thermal pasteurisation. However, the applied heat can cause detrimental effects on health-promoting components such as phenolic compounds. Several <span class="hlt">non-thermal</span> technologies such as membrane filtration, pulsed electric field (PEF) and ultraviolet (UV) exposure are promising methods developed for liquid food preservation. In particular, the combination of UV and PEF has proven to be more effective for microbial inactivation and maintaining nutritional quality of fruit juice compared with individual applications. PMID:23408366</p> <div class="credits"> <p class="dwt_author">Chen, Yougui; Yu, Li Juan; Rupasinghe, H P Vasantha</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-03-30</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">375</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3482274"> <span id="translatedtitle">Effect of a <span class="hlt">non-thermal</span>, atmospheric-pressure, plasma brush on conversion of model self-etch adhesive formulations compared to conventional photo-polymerization</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p class="result-summary">Objective To determine the effectiveness and efficiency of <span class="hlt">non-thermal</span>, atmospheric plasmas for inducing polymerization of model dental self-etch adhesives. Methods The monomer mixtures used were bis-[2-(methacryloyloxy)ethyl] phosphate (2MP) and 2-hydroxyethyl methacrylate (HEMA), with mass ratios of 70/30, 50/50 and 30/70. Water was added to the above formulations: 10–30 wt%. These monomer/water mixtures were treated steadily for 40 s under a <span class="hlt">non-thermal</span> atmospheric plasma brush working at temperatures from 32° to 35°C. For comparison, photo-initiators were added to the above formulations for photo-polymerization studies, which were light-cured for 40 s. The degree of conversion (DC) of both the plasma- and light-cured samples was measured using FTIR spectroscopy with an attenuated total reflectance attachment. Results The <span class="hlt">non-thermal</span> plasma brush was effective in inducing polymerization of the model self-etch adhesives. The presence of water did not negatively affect the DC of plasma-cured samples. Indeed, DC values slightly increased, with increasing water content in adhesives: from 58.3% to 68.7% when the water content increased from 10% to 30% in the adhesives with a 50/50 (2MP/HEMA) mass ratio. Conversion values of the plasma-cured groups were higher than those of light-cured samples with the same mass ratio and water content. Spectral differences between the plasma- and light-cured groups indicate subtle structural distinctions in the resultant polymer networks. Significance This research if the first to demonstrate that the <span class="hlt">non-thermal</span> plasma brush induces polymerization of model adhesives under clinical settings by direct/indirect energy transfer. This device shows promise for polymerization of dental composite restorations having enhanced properties and performance.</p> <div class="credits"> <p class="dwt_author">Chen, Mingsheng; Zhang, Ying; Yao, Xiaomei; Li, Hao; Yu, Qingsong; Wang, Yong</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">376</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/22156983"> <span id="translatedtitle"><span class="hlt">Non-thermal</span> processes in standard big bang nucleosynthesis: II. Two-body disintegration of D, {sup 7}Li, {sup 7}Be nuclei by fast neutrons</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">Continuing the analysis of <span class="hlt">non-thermal</span> effects in standard big bang nucleosynthesis (JCAP05(2008)010), we examine the role of suprathermal nuclear reactions induced in the early universe plasma by energetic nucleons of various origins. The processes of present interest are break-ups of D, {sup 7}Li, {sup 7}Be nuclei induced by 14-MeV neutrons generated in the plasma via the T(d, n){sup 4}He reaction. It is shown that this reaction forms the ensemble of fast neutrons whose fraction in the plasma neutron component is at the level of 0.01 %. In spite of the small percentage, such neutrons can effectively destroy the loosely bound D, {sup 7}Li, {sup 7}Be nuclei. It is found that at temperatures T{sub 9} < 0.8 the n-induced <span class="hlt">non-thermal</span> break-ups of D and {sup 7}Li dominate over other reactions occurring in the n+D and n+{sup 7}Li systems. However, the <span class="hlt">non-thermal</span> neutronic effects prove to be insufficiently strong to modify the standard picture of nucleosynthesis. The D, {sup 3}He, {sup 4}He abundances are obtained to remain unchanged, and only a little effect is marked for primordial {sup 7}Li. The 0.01 % fraction of plasma neutrons (fast DT neutrons) reduces the {sup 7}Li abundance by 0.02 %.</p> <div class="credits"> <p class="dwt_author">Voronchev, Victor T. [Institute of Nuclear Physics, Moscow State University, Leninskie gory 1(2), Moscow 119991 (Russian Federation)] [Institute of Nuclear Physics, Moscow State University, Leninskie gory 1(2), Moscow 119991 (Russian Federation); Nakamura, Makoto [Central Research Institute of Electrical Power Industry, Iwado-kita 2-11-1, Komae, Tokyo 201-8511 (Japan)] [Central Research Institute of Electrical Power Industry, Iwado-kita 2-11-1, Komae, Tokyo 201-8511 (Japan); Nakao, Yasuyuki, E-mail: voronchev@srd.sinp.msu.ru, E-mail: makoto-n@criepi.denken.or.jp, E-mail: nakao@nucl.kyushu-u.ac.jp [Department of Applied Quantum Physics and Nuclear Engineering, Kyushu University, Motooka, Fukuoka 819-0395 (Japan)] [Department of Applied Quantum Physics and Nuclear Engineering, Kyushu University, Motooka, Fukuoka 819-0395 (Japan)</p> <p class="dwt_publisher"></p> <p class="publishDate">2009-05-15</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">377</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2014AAS...22411105D"> <span id="translatedtitle"><span class="hlt">Non-thermal</span> Motions in and Above Flare Loop Tops Measured by the Extreme-ultraviolet Imaging Spectrometer (EIS) on Hinode</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">The plasma volume above the soft X-ray emitting loop tops is of particular interest for studying the formation of flare loops. We present EIS observations of <span class="hlt">non-thermal</span> motions (turbulence) determined from spectral line profiles of Fe XXIII and Fe XXIV ions for three well-observed flares near the solar limb. We compare the <span class="hlt">non-thermal</span> motions at temperatures near 10 MK with the motions along the same lines-of-sight determined from lines of coronal ions such as Fe XII, Fe XIV, and Fe XV formed at 1-2 MK. The take-away is that the <span class="hlt">non-thermal</span> motions obtained from Fe XXIII and Fe XXIV lines increase with height towards the reconnection region, up to speeds of about 50-60 km/s for the largest heights that we can observe. The implication is that considerable plasma heating occurs outside the reconnection region. In addition, we discuss the implications of results obtained for flares from earlier X-ray Yohkoh observations of line profiles of Fe XXV and Ca XIX on the current results from EIS and AIA. Fe XXV is formed at significantly higher temperatures than any strong flare EUV spectral line observed by EIS or by imaging telescopes such as AIA or TRACE. This work is supported by NASA grants.</p> <div class="credits"> <p class="dwt_author">Doschek, George A.; McKenzie, David Eugene; Warren, Harry P</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-06-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">378</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/22133881"> <span id="translatedtitle">THE LOCATION OF <span class="hlt">NON-THERMAL</span> VELOCITY IN THE EARLY PHASES OF LARGE FLARES-REVEALING PRE-ERUPTION FLUX ROPES</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary"><span class="hlt">Non-thermal</span> velocity measurements of the solar atmosphere, particularly from UV and X-ray emission lines have demonstrated over the decades that this parameter is important in understanding the triggering of solar flares. Enhancements have often been observed before intensity enhancements are seen. However, until the launch of Hinode, it has been difficult to determine the spatial location of the enhancements to better understand the source region. The Hinode EUV Imaging Spectrometer has the spectral and spatial resolution to allow us to probe the early stages of flares in detail. We analyze four events, all of which are GOES M- or X-classification flares, and all are located toward the limb for ease of flare geometry interpretation. Three of the flares were eruptive and one was confined. In all events, pre-flare enhancement in <span class="hlt">non-thermal</span> velocity at the base of the active region and its surroundings has been found. These enhancements seem to be consistent with the footpoints of the dimming regions, and hence may be highlighting the activation of a coronal flux rope for the three eruptive events. In addition, pre-flare enhancements in <span class="hlt">non-thermal</span> velocity were found above the looptops for the three eruptive events.</p> <div class="credits"> <p class="dwt_author">Harra, Louise K.; Matthews, Sarah; Culhane, J. L. [UCL-Mullard Space Science Laboratory, Holmbury St Mary, Dorking, Surrey RH5 6NT (United Kingdom); Cheung, Mark C. M. [Lockheed Martin Solar and Astrophysics Laboratory, 3251 Hanover Street, Building/252, Palo Alto, CA 94304 (United States); Kontar, Eduard P. [School of Physics and Astronomy, University of Glasgow, Glasgow G12 8QQ (United Kingdom); Hara, Hirohisa, E-mail: l.harra@ucl.ac.uk [National Astronomical Observatory of Japan, Osawa, Mitaka, Tokyo 181-8588 (Japan)</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-09-10</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">379</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2009AIPC.1103..501V"> <span id="translatedtitle">Proposed Use of Zero Bias Diode Arrays as Thermal Electric Noise Rectifiers and <span class="hlt">Non-Thermal</span> Energy Harvesters</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">The well known built-in voltage potential for some select semiconductor p-n junctions and various rectifying devices is proposed to be favorable for generating DC electricity at ``zero bias'' (with no DC bias voltage applied) in the presence of Johnson noise or 1/f noise which originates from the quantum vacuum (Koch et al., 1982). The 1982 Koch discovery that certain solid state devices exhibit measurable quantum noise has also recently been labeled a finding of dark energy in the lab (Beck and Mackey, 2004). Tunnel diodes are a class of rectifiers that are qualified and some have been credited with conducting only because of quantum fluctuations. Microwave diodes are also good choices since many are designed for zero bias operation. A completely passive, unamplified zero bias diode converter/detector for millimeter (GHz) waves was developed by HRL Labs in 2006 under a DARPA contract, utilizing a Sb-based ``backward tunnel diode'' (BTD). It is reported to be a ``true zero-bias diode.'' It was developed for a ``field radiometer'' to ``collect thermally radiated power'' (in other words, `night vision'). The diode array mounting allows a feed from horn antenna, which functions as a passive concentrating amplifier. An important clue is the ``noise equivalent power'' of 1.1 pW per root hertz and the ``noise equivalent temperature difference'' of 10° K, which indicate sensitivity to Johnson noise (Lynch, et al., 2006). There also have been other inventions such as ``single electron transistors'' that also have ``the highest signal to noise ratio'' near zero bias. Furthermore, ``ultrasensitive'' devices that convert radio frequencies have been invented that operate at outer space temperatures (3 degrees above zero point: 3° K). These devices are tiny nanotech devices which are suitable for assembly in parallel circuits (such as a 2-D array) to possibly produce zero point energy direct current electricity with significant power density (Brenning et al., 2006). Photovoltaic p-n junction cells are also considered for possible higher frequency ZPE transduction. Diode arrays of self-assembled molecular rectifiers or preferably, nano-sized cylindrical diodes are shown to reasonably provide for rectification of electron fluctuations from thermal and <span class="hlt">non-thermal</span> ZPE sources to create an alternative energy DC electrical generator in the picowatt per diode range.</p> <div class="credits"> <p class="dwt_author">Valone, Thomas F.</p> <p class="dwt_publisher"></p> <p class="publishDate">2009-03-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">380</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/servlets/purl/878291"> <span id="translatedtitle">Novel Composite Hydrogen-Permeable Membranes for <span class="hlt">Non-Thermal</span> Plasma Reactors for the Decomposition of Hydrogen Sulfide</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">The goal of this experimental project is to design and fabricate a reactor and membrane test cell to dissociate hydrogen sulfide (H{sub 2}S) in a <span class="hlt">non-thermal</span> plasma and recover hydrogen (H{sub 2}) through a superpermeable multi-layer membrane. Superpermeability of hydrogen atoms (H) has been reported by some researchers using membranes made of Group V transition metals (niobium, tantalum, vanadium, and their alloys), although it has yet to be confirmed in this study. A pulsed corona discharge (PCD) reactor has been fabricated and used to dissociate H{sub 2}S into hydrogen and sulfur. A nonthermal plasma cannot be produced in pure H{sub 2}S with our reactor geometry, even at discharge voltages of up to 30 kV, because of the high dielectric strength of pure H{sub 2}S ({approx}2.9 times higher than air). Therefore, H{sub 2}S was diluted in another gas with lower breakdown voltage (or dielectric strength). Breakdown voltages of H{sub 2}S in four balance gases (Ar, He, N{sub 2} and H{sub 2}) have been measured at different H{sub 2}S concentrations and pressures. Breakdown voltages are proportional to the partial pressure of H{sub 2}S and the balance gas. H{sub 2}S conversion and the reaction energy efficiency depend on the balance gas and H{sub 2}S inlet concentrations. With increasing H{sub 2}S concentrations, H{sub 2}S conversion initially increases, reaches a maximum, and then decreases. H{sub 2}S conversion in atomic balance gases, such as Ar and He, is more efficient than that in diatomic balance gases, such as N{sub 2} and H{sub 2}. These observations can be explained by the proposed reaction mechanism of H{sub 2}S dissociation in different balance gases. The results show that nonthermal plasmas are effective for dissociating H{sub 2}S into hydrogen and sulfur.</p> <div class="credits"> <p class="dwt_author">Morris D. Argyle; John F. Ackerman; Suresh Muknahallipatna; Jerry C. Hamann; Stanislaw Legowski; Guibling Zhao; Ji-Jun Zhang; Sanil John</p> <p class="dwt_publisher"></p> <p class="publishDate">2005-10-01</p> </div> </div> </div> </div> <div id="filter_results_form" class="filter_results_form floatContainer" style="visibility: visible;"> <div style="width:100%" id="PaginatedNavigation" class="paginatedNavigationElement"> <a id="FirstPageLink" onclick='return showDiv("page_1");' href="#" title="First Page"> <img id="FirstPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.first.18x20.png" alt="First Page" /></a> <a id="PreviousPageLink" onclick='return showDiv("page_18");' href="#" title="Previous Page"> <img id="PreviousPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.previous.18x20.png" alt="Previous Page" /></a> <span id="PageLinks" class="pageLinks"> <span> <a onClick='return showDiv("page_1");' href="#">1</a> <a onClick='return showDiv("page_2");' href="#">2</a> <a onClick='return showDiv("page_3");' 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src="http://www.science.gov/scigov/images/icon.next.18x20.png" alt="Next Page" /></a> <a id="LastPageLink" onclick='return showDiv("page_25.0");' href="#" title="Last Page"> <img id="LastPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.last.18x20.png" alt="Last Page" /></a> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">381</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2012MNRAS.423.3512C"> <span id="translatedtitle"><span class="hlt">Non-thermal</span> insights on mass and energy flows through the Galactic Centre and into the Fermi bubbles</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">We construct a simple model of the star-formation- (and resultant supernova-) driven mass and energy flows through the inner ˜200 pc (in diameter) of the Galaxy. Our modelling is constrained, in particular, by the <span class="hlt">non-thermal</span> radio continuum and ?-ray signals detected from the region. The modelling points to a current star formation rate of 0.04-0.12 M? yr-1 at 2? confidence within the region with best-fitting value in the range 0.08-0.12 M? yr-1 which - if sustained over 10 Gyr - would fill out the ˜109 M? stellar population of the nuclear bulge. Mass is being accreted on to the Galactic Centre (GC) region at a rate ? yr-1. The region's star formation activity drives an outflow of plasma, cosmic rays and entrained, cooler gas. Neither the plasma nor the entrained gas reaches the gravitational escape speed, however, and all this material fountains back on to the inner Galaxy. The system we model can naturally account for the recently observed ?106 M?'halo' of molecular gas surrounding the Central Molecular Zone out to 100-200 pc heights. The injection of cooler, high-metallicity material into the Galactic halo above the GC may catalyze the subsequent cooling and condensation of hot plasma out of this region and explain the presence of relatively pristine, nuclear-unprocessed gas in the GC. This process may also be an important ingredient in understanding the long-term stability of the GC star formation rate. The plasma outflow from the GC reaches a height of a few kpc and is compellingly related to the recently discovered Fermi bubbles by a number of pieces of evidence. These include that the outflow advects precisely (i) the power in cosmic rays required to sustain the bubbles'?-ray luminosity in saturation; (ii) the hot gas required to compensate for gas cooling and drop-out from the bubbles and (iii) the magnetic field required to stabilize the walls of these structures. Our modelling demonstrates that ˜109 M? of hot gas is processed through the GC over 10 Gyr. We speculate that the continual star formation in the GC over the age of the Milky Way has kept the supermassive black hole in a quiescent state thus preventing it from significantly heating the coronal gas, allowing for the continual accretion of gas on to the disc and the sustenance of star formation on much wider scales in the Galaxy. In general, our investigations explicitly reveal the GC's important role in the Milky Way's wider stellar ecology.</p> <div class="credits"> <p class="dwt_author">Crocker, R. M.</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-07-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">382</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2013JAP...113w3302T"> <span id="translatedtitle">Optical emission spectroscopic diagnostics of a <span class="hlt">non-thermal</span> atmospheric pressure helium-oxygen plasma jet for biomedical applications</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">In this work, we have applied optical emission spectroscopy diagnostics to investigate the characteristics of a <span class="hlt">non-thermal</span> atmospheric pressure helium plasma jet. The discharge characteristics in the active and afterglow region of the plasma jet, that are critical for biomedical applications, have been investigated. The voltage-current characteristics of the plasma discharge were analyzed and the average plasma power was measured to be around 18 W. The effect of addition of small fractions of oxygen at 0.1%-0.5% on the plasma jet characteristics was studied. The addition of oxygen resulted in a decrease in plasma plume length due to the electronegativity property of oxygen. Atomic and molecular lines of selected reactive plasma species that are considered to be useful to induce biochemical reactions such as OH transitions A2?+(?=0,1)-->X2?(??=0) at 308 nm and A2?+(?=0,1)-->X2?(??=1) at 287 nm, O I transitions 3p5P-->3s5S0 at 777.41 nm, and 3p3P-->3s3S0 at 844.6 nm, N2(C-B) second positive system with electronic transition C3?u -->B3?g in the range of 300-450 nm and N2+(B-X) first negative system with electronic transition B2?u+-->X2?g+(??=0) at 391.4 nm have been studied. The atomic emission lines of helium were identified, including the He I transitions 3p3P0-->2s3S at 388.8 nm, 3p1P0--> 2s1S at 501.6 nm, 3d3D-->2p3P0 at 587.6 nm, 3d1D-->2p1P0 at 667.8 nm, 3s3S1-->2p3P0 at 706.5 nm, 3s1S0-->2p1P0 at 728.1 nm, and H? transition 2p-3d at 656.3 nm. Using a spectral fitting method, the OH radicals at 306-312 nm, the rotational and vibrational temperatures equivalent to gas temperatures of the discharge was measured and the effective non-equilibrium nature of the plasma jet was demonstrated. Our results show that, in the entire active plasma region, the gas temperature remains at 310 +/- 25 K and 340 +/- 25 K and it increases to 320 +/- 25 K and 360 +/- 25 K in the afterglow region of the plasma jet for pure helium and helium/oxygen (0.1%) mixture, respectively. Additionally, the vibrational temperatures range from 2200 +/- 100 K and 2500 +/- 100 K for pure helium and helium/oxygen (0.1%) mixture, respectively. The plasma jet was tested on heat sensitive polymer films used in biomedical applications such as polyethylene terephthalate and poly-L-lactide samples continuously for several minutes without causing any physical or thermal damage to the films. The plasma jet produces significant reactive species of interest while the gas temperatures remain very low demonstrating its potential for a range of biomedical applications.</p> <div class="credits"> <p class="dwt_author">Thiyagarajan, Magesh; Sarani, Abdollah; Nicula, Cosmina</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-06-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">383</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2009SPIE.7231E...6M"> <span id="translatedtitle">Reduced <span class="hlt">non-thermal</span> roll-over in violet-emitting GaInN wide-well LEDs grown on low-dislocation-density substrates</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Near-UV LEDs emitting at around 400 nm can be used e.g. as pump light source in tri-phosphor RGB white luminescence-conversion LEDs with high color rendering.1 Although <span class="hlt">non-thermal</span> roll-over decreases towards shorter emission wavelengths in GaInN-based LEDs, this effect still limits the efficiency of 400 nm emitting LEDs at current densities above 50 A/cm2. One way to overcome <span class="hlt">non-thermal</span> roll-over is to combine a GaInN wide-well active region with the growth on low dislocation density (DD) substrates. Single-well LEDs with GaInN layer widths between 3 nm and 18 nm were grown (a) directly on sapphire substrates with a resulting DD of 109 cm-2, (b) on low DD GaN templates on sapphire (DD of 108 cm-2), and (c) on freestanding GaN substrates (FS-GaN, DD of 4×107 cm-2). At low current densities (pulsed mode operation) the LEDs with a 3 nm GaInN QW active region showed the highest efficiency, irrespective of the substrate. However, the electroluminescence (EL) efficiency peaks at around 50 A/cm2 and shows a clear <span class="hlt">non-thermal</span> roll-over towards higher current densities. The efficiency of LEDs with well widths >3 nm grown on sapphire decreases with increasing well width over the whole range of current densities (<=300 A/cm2). However, when grown on low DD GaN templates or FS-GaN, the efficiency of the LEDs with 11 and 18 nm wide GaInN layers surpasses that of the conventional LEDs (well widths <=6 nm) for current densities >=250 A/cm2, yielding the highest EL efficiency of all LED-structures.</p> <div class="credits"> <p class="dwt_author">Maier, Markus; Passow, Thorsten; Kunzer, Michael; Schirmacher, Wilhelm; Pletschen, Wilfried; Kirste, Lutz; Köhler, Klaus; Wagner, Joachim</p> <p class="dwt_publisher"></p> <p class="publishDate">2009-02-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">384</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/21567515"> <span id="translatedtitle">THE LACK OF DIFFUSE, <span class="hlt">NON-THERMAL</span> HARD X-RAY EMISSION IN THE COMA CLUSTER: THE SWIFT BURST ALERT TELESCOPE'S EYE VIEW</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">The Coma Cluster of galaxies hosts the brightest radio halo known and has therefore been the target of numerous searches for associated inverse Compton (IC) emission, particularly at hard X-ray energies where the IC signal must eventually dominate over thermal emission. The most recent search with the Suzaku Hard X-ray Detector failed to confirm previous IC detections with RXTE and BeppoSAX, instead setting an upper limit 2.5 times below their <span class="hlt">non-thermal</span> flux. However, this discrepancy can be resolved if the IC emission is very extended, beyond the scale of the cluster radio halo. Using reconstructed sky images from the 58-month Swift Burst Alert Telescope (BAT) all-sky survey, the feasibility of such a solution is investigated. Building on Renaud et al., we test and implement a method for extracting the fluxes of extended sources, assuming specified spatial distributions. BAT spectra are jointly fit with an XMM-Newton EPIC-pn spectrum derived from mosaic observations. We find no evidence for large-scale IC emission at the level expected from the previously detected <span class="hlt">non-thermal</span> fluxes. For all <span class="hlt">non-thermal</span> spatial distributions considered, which span the gamut of physically reasonable IC models, we determine upper limits for which the largest (most conservative) limit is {approx}<4.2 x 10{sup -12} erg s{sup -1} cm{sup -2} (20-80 keV), which corresponds to a lower limit on the magnetic field B > 0.2 {mu} G. A nominal flux upper limit of <2.7 x 10{sup -12} erg s{sup -1} cm{sup -2}, with corresponding B > 0.25 {mu} G, is derived for the most probable IC distribution given the size of the radio halo and likely magnetic field radial profile.</p> <div class="credits"> <p class="dwt_author">Wik, Daniel R.; Baumgartner, Wayne H.; Okajima, Takashi; Tueller, Jack [Astrophysics Science Division, Laboratory for High Energy Astrophysics, Code 662, NASA/Goddard Space Flight Center, Greenbelt, MD 20771 (United States); Sarazin, Craig L. [Department of Astronomy, University of Virginia, 530 McCormick Road Charlottesville, VA 22904 (United States); Finoguenov, Alexis [Max-Planck-Institut fuer Extraterrestrische Physik, Giessenbachstr., 85748 Garching (Germany); Mushotzky, Richard F. [Department of Astronomy, University of Maryland, College Park, MD 20742 (United States); Clarke, Tracy E., E-mail: daniel.r.wik@nasa.gov [Naval Research Laboratory, 4555 Overlook Ave. SW, Code 7213, Washington, DC 20375 (United States)</p> <p class="dwt_publisher"></p> <p class="publishDate">2011-02-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">385</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2014PhPl...21e3510X"> <span id="translatedtitle">Electron density measurements of atmospheric-pressure <span class="hlt">non-thermal</span> N2 plasma jet by Stark broadening and irradiance intensity methods</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">An atmospheric-pressure <span class="hlt">non-thermal</span> plasma jet excited by high frequency alternating current using nitrogen is developed and the electron density in the active region of this plasma jet is investigated by two different methods using optical emission spectroscopy, Stark broadening, and irradiance intensity method. The irradiance intensity method shows that the average electron density is about 1020/m3 which is slightly smaller than that by the Stark broadening method. However, the trend of the change in the electron density with input power obtained by these two methods is consistent.</p> <div class="credits"> <p class="dwt_author">Xiao, Dezhi; Cheng, Cheng; Shen, Jie; Lan, Yan; Xie, Hongbing; Shu, Xingsheng; Meng, Yuedong; Li, Jiangang; Chu, Paul K.</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-05-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">386</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/servlets/purl/350825"> <span id="translatedtitle">Final Report: Fiscal Year 1997 demonstration of omnivorous <span class="hlt">non-thermal</span> mixed waste treatment: Direct chemical oxidation of organic solids and liquids using peroxydisulfate</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">Direct Chemical Oxidation (DCO) is a <span class="hlt">non-thermal</span>, ambient pressure, aqueous-based technology for the oxidative destruction of the organic components of hazardous or mixed waste streams. The process has been developed for applications in waste treatment, chemical demilitarization and decontamination at LLNL since 1992. The process uses solutions of the peroxydisulfate ion (typically sodium or ammonium salts) to completely mineralize the organics to carbon dioxide and water. The expended oxidant may be electrolytically regenerated to minimize secondary waste. The paper briefly describes: free radical and secondary oxidant formation; electrochemical regeneration; offgas stream; and throughput.</p> <div class="credits"> <p class="dwt_author">Cooper, J.F.</p> <p class="dwt_publisher"></p> <p class="publishDate">1998-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">387</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/doepatents/biblio/908311"> <span id="translatedtitle">Method and system for the combination of <span class="hlt">non-thermal</span> plasma and metal/metal oxide doped .gamma.-alumina catalysts for diesel engine exhaust aftertreatment system</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/doepatents">DOEpatents</a></p> <p class="result-summary">The present disclosure pertains to a system and method for treatment of oxygen rich exhaust and more specifically to a method and system that combines <span class="hlt">non-thermal</span> plasma with a metal doped .gamma.-alumina catalyst. Current catalyst systems for the treatment of oxygen rich exhaust are capable of achieving only approximately 7 to 12% NO.sub.x reduction as a passive system and only 25 40% reduction when a supplemental hydrocarbon reductant is injected into the exhaust stream. It has been found that treatment of an oxygen rich exhaust initially with a <span class="hlt">non-thermal</span> plasma and followed by subsequent treatment with a metal doped .gamma.-alumina prepared by the sol gel method is capable of increasing the NO.sub.x reduction to a level of approximately 90% in the absence of SO.sub.2 and 80% in the presence of 20 ppm of SO.sub.2. Especially useful metals have been found to be indium, gallium, and tin.</p> <div class="credits"> <p class="dwt_author">Aardahl, Christopher L. (Richland, WA); Balmer-Miller, Mari Lou (West Richland, WA); Chanda, Ashok (Peoria, IL); Habeger, Craig F. (West Richland, WA); Koshkarian, Kent A. (Peoria, IL); Park, Paul W. (Peoria, IL)</p> <p class="dwt_publisher"></p> <p class="publishDate">2006-07-25</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">388</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=2773321"> <span id="translatedtitle"><span class="hlt">Non-thermal</span> ablation of rabbit liver VX2 tumor by pulsed high intensity focused ultrasound with ultrasound contrast agent: Pathological characteristics</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p class="result-summary">AIM: To investigate the pathological characteristics of <span class="hlt">non-thermal</span> damage induced by pulsed high intensity focused ultrasound (PHIFU) combined with ultrasound contrast agent (UCA), SonoVue (Bracco SpA, Milan, Italy) in rabbit liver VX2 tumor. METHODS: Liver VX2 tumor models were established in 20 rabbits, which were divided randomly into PHIFU combined with ultrasound contrast agent group (PHIFU + UCA group) and sham group. In the PHIFU + UCA group, 0.2 mL of SonoVue was injected intravenously into the tumor, followed by ultrasound exposure of ISP 5900 W/cm2. The rabbits were sacrificed one day after ultrasound exposure. Specimens of the exposed tumor tissues were obtained and observed pathologically under light microscope and transmission electron microscope. The remaining tumor tissues were sent for 2,3,5-Triphenyltetrazolium chloride (TTC) staining. RESULTS: Before TTC staining, tumor tissues in both the sham and the PHIFU + UCA groups resembled gray fish meat. After TTC staining, the tumor tissues were uniformly stained red, with a clear boundary between tumor tissue and normal tissue. Histological examination showed signs of tumor cell injury in PHIFU + UCA group, with cytoplasmic vacuoles of various sizes, chromatin margination and karyopyknosis. Electron microscopic examination revealed tumor cell volume reduction, karyopyknosis, chromatin margination, intercellular space widening, the presence of high electron-density apoptotic bodies and vacuoles in cytoplasm. CONCLUSION: The <span class="hlt">non-thermal</span> effects of PHIFU combined with UCA can be used to ablate rabbit liver VX2 tumors.</p> <div class="credits"> <p class="dwt_author">Zhou, Cheng-Wen; Li, Fa-Qi; Qin, Yan; Liu, Chun-Mei; Zheng, Xiao-Lin; Wang, Zhi-Biao</p> <p class="dwt_publisher"></p> <p class="publishDate">2008-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">389</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2009SPIE.7380E..87I"> <span id="translatedtitle">The new application of photosensitization reaction to atrial fibrillation treatment: mechanism and demonstration of <span class="hlt">non-thermal</span> electrical conduction block with porcine heart</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">We have proposed <span class="hlt">non-thermal</span> electrical conduction block for atrial fibrillation treatment by the photosensitization reaction, in which the interval time between the photosensitizer injection and irradiation is less than tenth of that in conventional way. To study the mechanism of photosensitization reaction-induced electrical conduction block, intracellular Ca2+ concentration change in rat myocardial cells was measured by fluorescent Ca2+ indicator Fluo-4 AM with confocal laser microscopy. Measured rapid increase in the fluorescence intensity and a change in cell morphology indicated that cell membrane damage; that is Ca2+ influx and eventually cell death caused by the photosensitization reaction. To demonstrate myocardial electrical conduction block induced by the photosensitization reaction, surgically exposed porcine heart under deep anesthesia was used. The myocardial tissue was paced with a stimulation electrode. The propagated electrical signals were measured by bipolar electrodes at two different positions. Thirty minutes after the injection of 5-10 mg/kg Porfimer sodium or Talaporfin sodium, the red laser light was irradiated to the tissue point by point crossing the measuring positions by the total energy density of less than 200 J/cm2. The electrical signal conduction between the measuring electrodes in the myocardial tissue was delayed by each irradiation procedure. The electrical conduction delay corresponded to the block line length was obtained. These results demonstrated the possibility of <span class="hlt">non-thermal</span> electrical conduction block for atrial fibrillation treatment by the photosensitization reaction.</p> <div class="credits"> <p class="dwt_author">Ito, Arisa; Matsuo, Hiroki; Suenari, Tsukasa; Kajihara, Takuro; Kimura, Takehiro; Miyoshi, Shunichiro; Ogawa, Satoshi; Arai, Tsunenori</p> <p class="dwt_publisher"></p> <p class="publishDate">2009-06-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">390</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/1073568"> <span id="translatedtitle">Multiple <span class="hlt">Non-Thermal</span> Reaction Steps for the Photooxidation CO to CO2 on Reduced TiO2(110)</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">The photooxidation of CO on reduced, rutile TiO2(110) was studied on a millisecond timescale. For a saturation coverage of chemisorbed O2 (0sat) and for half that coverage, the CO2 photon-stimulated desorption (PSD) signal is initially zero, increases to a maximum after several tens of milliseconds, and then decreases at longer times. The CO2 PSD signal increases ~5 times more quickly for 0.50sat. The initial rate of increase of the CO2 PSD signal is proportional to the flux of UV photons. The intermediate species involved in the reactions is stable for at least 100 s at 30 K. These results show that two or more <span class="hlt">non-thermal</span> reaction steps are required to photooxidize CO adsorbed on TiO2(110). In contrast, previous models had suggested that CO photooxidation required only one <span class="hlt">non-thermal</span> reaction. The likely initial and final charge states of the system suggest that an electron-mediated reaction and a hole-mediated reaction are needed for the complete photooxidation reaction.</p> <div class="credits"> <p class="dwt_author">Petrik, Nikolay G.; Kimmel, Gregory A.</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-02-07</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">391</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=20020039528&hterms=4996&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D40%26Ntt%3D%25224996%2522"> <span id="translatedtitle">Observations of the <span class="hlt">Non-Thermal</span> X-ray Emission from the Galactic Supernova Remnant G347.3-0.5</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">G347.3-0.5 (ALEX J1713.7-3946) is a member of the new class of shell-type Galactic supernova remnants (SNRs) that feature <span class="hlt">non-thermal</span> components to their X-ray emission. We have analyzed the X-ray spectrum of this SNR over a broad energy range (0.5 to 30 key) using archived data from observations made with two satellites, the R6ntgensatellit (ROSA I) and the Advanced Satellite for Cosmology and Astrophysics (ASCA), along with data from our own observations made with the Rossi X-ray Timing Explorer (RXTE) Using a combination of the models EQUIL and SRCUT to fit thermal and <span class="hlt">non-thermal</span> emission, respectively, from this SNR, we find evidence for a modest thermal component to G347.30.5's diffuse emission with a corresponding energy of kT approx. = 1.4 key. We also obtain an estimate of 70 Texas for the maximum energy of the cosmic-ray electrons that, have been accelerated by this SNR.</p> <div class="credits"> <p class="dwt_author">Pannuti, Thomas G.; Allen, Glenn E.</p> <p class="dwt_publisher"></p> <p class="publishDate">2002-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">392</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2013ApJ...779...49C"> <span id="translatedtitle">A Chandra View of <span class="hlt">Non-thermal</span> Emission in the Northwestern Region of Supernova Remnant RCW 86: Particle Acceleration and Magnetic Fields</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">The shocks of supernova remnants are believed to accelerate particles to cosmic ray (CR) energies. The amplification of the magnetic field due to CRs propagating in the shock region is expected to have an impact on both the emission from the accelerated particle population as well as the acceleration process itself. Using a 95 ks observation with the Advanced CCD Imaging Spectrometer on board the Chandra X-Ray Observatory, we map and characterize the synchrotron emitting material in the northwest region of RCW 86. We model spectra from several different regions, both filamentary and diffuse, where emission appears to be dominated by synchrotron radiation. The fine spatial resolution of Chandra allows us to obtain accurate emission profiles across three different <span class="hlt">non-thermal</span> rims in this region. The narrow width (l ? 10''-30'') of these filaments constrains the minimum magnetic field strength at the post-shock region to approximately 80 ?G.</p> <div class="credits"> <p class="dwt_author">Castro, Daniel; Lopez, Laura A.; Slane, Patrick O.; Yamaguchi, Hiroya; Ramirez-Ruiz, Enrico; Figueroa-Feliciano, Enectali</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-12-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">393</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2012MNRAS.423.2753J"> <span id="translatedtitle">Extended X-ray emission from <span class="hlt">non-thermal</span> sources in the COSMOS field: a detailed study of a large radio galaxy at z= 1.168</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">X-ray selected galaxy group samples are usually generated by searching for extended X-ray sources that reflect the thermal radiation of the intragroup medium. On the other hand, large radio galaxies that regularly occupy galaxy groups also emit in the X-ray window, and their contribution to X-ray selected group samples is still not well understood. In order to investigate their relative importance, we have carried out a systematic search for <span class="hlt">non-thermal</span> extended X-ray sources in the Cosmic Evolution Survey (COSMOS) field. Based on the morphological coincidence of X-ray and radio extensions, out of 60 radio galaxies, and ˜300 extended X-ray sources, we find only one candidate where the observed extended X-ray emission arises from <span class="hlt">non-thermal</span> processes related to radio galaxies. We present a detailed analysis of this source, and its environment. Our results yield that external inverse Compton emission of the lobes is the dominant process that generates the observed X-ray emission of our extended X-ray candidate, with a minor contribution from the gas of the galaxy group hosting the radio galaxy. Finally, we show that finding only one potential candidate in the COSMOS field (in a redshift range 0 < z < 6 and with radio luminosity between 1025 and 1030 W Hz-1) is consistent with expected X-ray counts arising from synchrotron lobes. This implies that these sources are not a prominent source of contamination in samples of X-ray selected clusters/groups, but they could potentially dominate the z > 1 cluster counts at the bright end (SX > 7 × 10-15 erg s-1 cm2).</p> <div class="credits"> <p class="dwt_author">Jeli?, Vibor; Smol?i?, Vernesa; Finoguenov, Alexis; Tanaka, Masayuki; Civano, Francesca; Schinnerer, Eva; Cappelluti, Nico; Koekemoer, Anton</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-07-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">394</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3493438"> <span id="translatedtitle">Preferential induction of apoptotic cell death in melanoma cells as compared with normal keratinocytes using a <span class="hlt">non-thermal</span> plasma torch</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p class="result-summary">Selective induction of apoptosis in melanoma cells is optimal for therapeutic development. To achieve this goal, a <span class="hlt">non-thermal</span> helium plasma torch was modified for use on cultured cells in a temperature-controlled environment. Melanoma cells were targeted with this torch (1) in parallel cultures with keratinocytes, (2) in co-culture with keratinocytes and (3) in a soft agar matrix. Melanoma cells displayed high sensitivity to reactive oxygen species generated by the torch and showed a 6-fold increase in cell death compared with keratinocytes. The extent of cell death was compared between melanoma cells and normal human keratinocytes in both short-term (5 min) co-culture experiments and longer assessments of apoptotic cell death (18–24 h). Following a 10 sec plasma exposure there was a 4.9-fold increase in the cell death of melanoma vs. keratinocytes as measured after 24 h at the target site of the plasma beam. When the treatment time was increased to 30 sec, a 98% cell death was reported for melanoma cells, which was 6-fold greater than the extent of cell death in keratinocytes. Our observations further indicate that this preferential cell death is largely due to apoptosis.. In addition, we report that this <span class="hlt">non-thermal</span> plasma torch kills melanoma cells growing in soft agar, suggesting that the plasma torch is capable of inducing melanoma cell death in 3D settings. We demonstrate that the presence of gap junctions may increase the area of cell death, likely due to the “bystander effect” of passing apoptotic signals between cells. Our findings provide a basis for further development of this non-invasive plasma torch as a potential treatment for melanoma.</p> <div class="credits"> <p class="dwt_author">Zucker, Shoshanna N.; Zirnheld, Jennifer; Bagati, Archis; DiSanto, Thomas M.; Des Soye, Benjamin; Wawrzyniak, Joseph A.; Etemadi, Kasra; Nikiforov, Mikhail; Berezney, Ronald</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">395</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2011EPJAP..5624019B"> <span id="translatedtitle">Nano-droplet ejection and nucleation of materials submitted to <span class="hlt">non-thermal</span> plasma filaments<xref ref-type="fn" rid="FN1"></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Methods to induce <span class="hlt">non-thermal</span> atmospheric pressure plasma filaments are presented with related properties for micro, streamer and prevented spark discharges, respectively, induced in planar Dielectric Barrier Discharges with one electrode covered by dielectric material (mono-DBD) or point-to-plane Corona. Two mechanisms of nano-particles formation are depicted from aerosol size distributions and TEM analysis. 0.1-10 mJ prevented spark discharges produce 10-100 nm droplets ejected from melted craters as well as nucleated primary particles and subsequent 10-100 nm agglomerates, by nucleation and coagulation in expanding vapor jets. With smaller energy per filament, 0.1-10 ?J micro-discharges and 0.1-100 ?J streamers, the initial local vapor fluxes emitted from spots of interaction between plasma filaments and electrodes are reduced. Subsequent smaller primary particle density limits the local coagulation in the vapor plume since 2-10 nm non-agglomerated crystalline metal nano-particles are produced in mono-DBD with Au, Ag and Cu electrode. Besides, the evolution of the aerosol size from primary nano-particles to agglomerates with transit time suggests slow coagulation of these primary metal particles in mono-DBD. Aerosol properties depend on the energy per filament and on the electrode. The final size is controlled by plasma parameters and transit time in and after the plasma. The aim is to underline emerging applications of atmospheric pressure plasmas for the production of tailored particles with tunable size, composition and structure with <span class="hlt">non-thermal</span> plasma filaments to control the resulting properties of nano-powders and materials. Production rates and related energetic yields are compared.</p> <div class="credits"> <p class="dwt_author">Borra, J.-P.; Jidenko, N.; Dutouquet, C.; Aguerre, O.; Hou, J.; Weber, A.</p> <p class="dwt_publisher"></p> <p class="publishDate">2011-11-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">396</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2008A%26A...491..363O"> <span id="translatedtitle">Suzaku broad-band spectroscopy of RX J1347.5-1145: constraints on the extremely hot gas and <span class="hlt">non-thermal</span> emission</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Context: We present the results of our analysis of long Suzaku observations (149 ks and 122 ks for XIS and HXD, respectively) of the most X-ray luminous galaxy cluster, RX J1347.5-1145, at z=0.451. Aims: To understand the gas physics of a violent, cluster merger, we study physical properties of the hot ( 20 keV) gas clump in the south-east (SE) region discovered previously by Sunyaev-Zel'dovich (SZ) effect observations. Using hard X-ray data, a signature of <span class="hlt">non-thermal</span> emission is also explored. Methods: We perform single as well as multi-temperature fits to the Suzaku XIS spectra. The Suzaku XIS and HXD, and the Chandra ACIS-I data are then combined to examine the properties of the hot gas component in the SE region. We finally look for <span class="hlt">non-thermal</span> emission in the Suzaku HXD data. Results: The single-temperature model fails to reproduce the 0.5-10 keV continuum emission and Fe-K lines measured by XIS simultaneously. A two-temperature model with a very hot component improves the fit, although the XIS data can only provide a lower limit to the temperature of the hot component. In the Suzaku HXD data, we detect hard X-ray emission above the background in the 12-40 keV band at the 9? level; however, the significance becomes marginal when the systematic error in the background estimation is included. With the joint analysis of the Suzaku and Chandra data, we determine the temperature of the hot gas in the SE region to be 25.3+6.1-4.5 (statistical; 90% confidence level) +6.9-9.5 (systematic; 90% confidence level) keV, which is in an excellent agreement with the previous joint analysis of the SZ effect in radio and the Chandra X-ray data. This is the first time that the X-ray analysis alone provides a good measurement of the hot component temperature in the SE region, which is possible because of Suzaku's unprecedented sensitivity over the wide X-ray band. These results indicate strongly that RX J1347.5-1145 has undergone a recent, violent merger. The spectral analysis shows that the SE component is consistent with being thermal. We measure the 3? upper limit to the <span class="hlt">non-thermal</span> flux, F<8×10-12 erg s-1 cm^{-2} in the 12-60 keV band, which provides a limit on the inverse Compton scattering of relativistic electrons off the CMB photons. Combining this limit with the discovery of a radio mini halo in this cluster at 1.4 GHz, which measures the synchrotron radiation, we find a lower limit to the strength of the intracluster magnetic field, such that B>0.007 {? G}.</p> <div class="credits"> <p class="dwt_author">Ota, N.; Murase, K.; Kitayama, T.; Komatsu, E.; Hattori, M.; Matsuo, H.; Oshima, T.; Suto, Y.; Yoshikawa, K.</p> <p class="dwt_publisher"></p> <p class="publishDate">2008-11-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">397</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/servlets/purl/334238"> <span id="translatedtitle">Reactions of oxides of nitrogen (NO{sub x}) leading to the formation of nitric acid (HNO{sub 3}) in <span class="hlt">non-thermal</span> plasmas (NTPs). White paper for the Strategic Environmental Research and Development Program (SERDP) (Compliance Project CP-1038: Development of <span class="hlt">non-thermal</span> plasma reactor technology for control of atmospheric emissions)</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">SERDP Compliance Project CP-1038 (Development of <span class="hlt">Non-Thermal</span> Plasma Reactor Technology for Control of Atmospheric Emissions) has been commissioned to evaluate and develop <span class="hlt">non-thermal</span> plasma (NTP) reactor technology, a form of low-temperature plasma chemical processing, for Department of Defense (DoD) applications. The primary emphasis is on the control of emissions of oxides of nitrogen (NO{sub x}), with a secondary emphasis on hazardous air pollutant (HAP) emission control (primarily volatile organic compounds--VOCs). In this white paper, as a SERDP-requested deliverable, the authors will verify the NO{sub x} removal reactions in NTPs, especially those converging on nitric acid (HNO{sub 3}) as a primary reaction product. The benefit of making HNO{sub 3} as a primary terminal de-NO{sub x} product is that it can be easily neutralized by relatively simple caustic (base) scrubbers--although the economics of scrubber systems needs to be compared with the conversion to particles that can be filtered or precipitated. Jet engines also emit a significant amount of SO{sub x} in their exhaust; NTPs also remove SO{sub x} and actually do it more effectively in combination with NO{sub x}. This will not be dealt with in this particular white paper.</p> <div class="credits"> <p class="dwt_author">Rosocha, L.A. [Los Alamos National Lab., NM (United States); Miziolek, A.W.; Nusca, M.J. [Army Research Lab., Watertown, MA (United States); Chang, J.S. [McMaster Univ., Hamilton, Ontario (Canada); Herron, J.T. [National Inst. for Standards and Technology (United States)</p> <p class="dwt_publisher"></p> <p class="publishDate">1998-08-17</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">398</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2012A%26A...548A..38A"> <span id="translatedtitle">Probing the extent of the <span class="hlt">non-thermal</span> emission from the Vela X region at TeV energies with H.E.S.S.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Context. Vela X is a region of extended radio emission in the western part of the Vela constellation: one of the nearest pulsar wind nebulae, and associated with the energetic Vela pulsar (PSR B0833-45). Extended very-high-energy (VHE) ?-ray emission (HESS J0835-455) was discovered using the H.E.S.S. experiment in 2004. The VHE ?-ray emission was found to be coincident with a region of X-ray emission discovered with ROSAT above 1.5 keV (the so-called Vela X cocoon): a filamentary structure extending southwest from the pulsar to the centre of Vela X. Aims: A deeper observation of the entire Vela X nebula region, also including larger offsets from the cocoon, has been performed with H.E.S.S. This re-observation was carried out in order to probe the extent of the <span class="hlt">non-thermal</span> emission from the Vela X region at TeV energies and to investigate its spectral properties. Methods: To increase the sensitivity to the faint ?-ray emission from the very extended Vela X region, a multivariate analysis method combining three complementary reconstruction techniques of Cherenkov-shower images is applied for the selection of ?-ray events. The analysis is performed with the On/Off background method, which estimates the background from separate observations pointing away from Vela X; towards regions free of ?-ray sources but with comparable observation conditions. Results: The ?-ray surface brightness over the large Vela X region reveals that the detection of <span class="hlt">non-thermal</span> VHE ?-ray emission from the PWN HESS J0835-455 is statistically significant over a region of radius 1.2° around the position ? = 08h35m00s, ? = -45°36'00'' (J2000). The Vela X region exhibits almost uniform ?-ray spectra over its full extent: the differential energy spectrum can be described by a power-law function with a hard spectral index ? = 1.32 ± 0.06stat ± 0.12sys and an exponential cutoff at an energy of (14.0 ± 1.6stat ± 2.6sys) TeV. Compared to the previous H.E.S.S. observations of Vela X the new analysis confirms the general spatial overlap of the bulk of the VHE ?-ray emission with the X-ray cocoon, while its extent and morphology appear more consistent with the (more extended) radio emission, contradicting the simple correspondence between VHE ?-ray and X-ray emissions. Morphological and spectral results challenge the interpretation of the origin of ?-ray emission in the GeV and TeV ranges in the framework of current models.</p> <div class="credits"> <p class="dwt_author">Abramowski, A.; Acero, F.; Aharonian, F.; Akhperjanian, A. G.; Anton, G.; Balenderan, S.; Balzer, A.; Barnacka, A.; Becherini, Y.; Becker Tjus, J.; Bernlöhr, K.; Birsin, E.; Biteau, J.; Bochow, A.; Boisson, C.; Bolmont, J.; Bordas, P.; Brucker, J.; Brun, F.; Brun, P.; Bulik, T.; Carrigan, S.; Casanova, S.; Cerruti, M.; Chadwick, P. M.; Charbonnier, A.; Chaves, R. C. G.; Cheesebrough, A.; Cologna, G.; Conrad, J.; Couturier, C.; Dalton, M.; Daniel, M. K.; Davids, I. D.; Degrange, B.; Deil, C.; deWilt, P.; Dickinson, H. J.; Djannati-Ataï, A.; Domainko, W.; Drury, L. O.' C.; Dubois, F.; Dubus, G.; Dutson, K.; Dyks, J.; Dyrda, M.; Egberts, K.; Eger, P.; Espigat, P.; Fallon, L.; Farnier, C.; Fegan, S.; Feinstein, F.; Fernandes, M. V.; Fernandez, D.; Fiasson, A.; Fontaine, G.; Förster, A.; Füßling, M.; Gajdus, M.; Gallant, Y. A.; Garrigoux, T.; Gast, H.; Giebels, B.; Glicenstein, J. F.; Glück, B.; Göring, D.; Grondin, M.-H.; Häffner, S.; Hague, J. D.; Hahn, J.; Hampf, D.; Harris, J.; Heinz, S.; Heinzelmann, G.; Henri, G.; Hermann, G.; Hillert, A.; Hinton, J. A.; Hofmann, W.; Hofverberg, P.; Holler, M.; Horns, D.; Jacholkowska, A.; Jahn, C.; Jamrozy, M.; Jung, I.; Kastendieck, M. A.; Katarzy?ski, K.; Katz, U.; Kaufmann, S.; Khélifi, B.; Klochkov, D.; Klu?niak, W.; Kneiske, T.; Komin, Nu.; Kosack, K.; Kossakowski, R.; Krayzel, F.; Krüger, P. P.; Laffon, H.; Lamanna, G.; Lenain, J.-P.; Lennarz, D.; Lohse, T.; Lopatin, A.; Lu, C.-C.; Marandon, V.; Marcowith, A.; Masbou, J.; Maurin, G.; Maxted, N.; Mayer, M.; McComb, T. J. L.; Medina, M. C.; Méhault, J.; Menzler, U.; Moderski, R.; Mohamed, M.; Moulin, E.; Naumann, C. L.; Naumann-Godo, M.; de Naurois, M.; Nedbal, D.; Nguyen, N.; Niemiec, J.; Nolan, S. J.; Ohm, S.; de Oña Wilhelmi, E.; Opitz, B.; Ostrowski, M.; Oya, I.; Panter, M.; Parsons, D.; Paz Arribas, M.; Pekeur, N. W.; Pelletier, G.; Perez, J.; Petrucci, P.-O.; Peyaud, B.; Pita, S.; Pühlhofer, G.; Punch, M.; Quirrenbach, A.; Raue, M.; Reimer, A.; Reimer, O.; Renaud, M.; de los Reyes, R.; Rieger, F.; Ripken, J.; Rob, L.; Rosier-Lees, S.; Rowell, G.; Rudak, B.; Rulten, C. B.; Sahakian, V.; Sanchez, D. A.; Santangelo, A.; Schlickeiser, R.; Schulz, A.; Schwanke, U.; Schwarzburg, S.; Schwemmer, S.; Sheidaei, F.; Skilton, J. L.; Sol, H.; Spengler, G.; Stawarz, ?.; Steenkamp, R.; Stegmann, C.; Stinzing, F.; Stycz, K.; Sushch, I.; Szostek, A.; Tavernet, J.-P.; Terrier, R.; Tluczykont, M.; Trichard, C.; Valerius, K.; van Eldik, C.; Vasileiadis, G.; Venter, C.; Viana, A.; Vincent, P.; Völk, H. J.; Volpe, F.; Vorobiov, S.; Vorster, M.; Wagner, S. J.; Ward, M.; White, R.; Wierzcholska, A.; Wouters, D.; Zacharias, M.; Zajczyk, A.; Zdziarski, A. A.; Zech, A.; Zechlin, H.-S.</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-12-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">399</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://oaspub.epa.gov/eims/eimsapi.dispdetail?deid=18856"> <span id="translatedtitle">ECONOMIC ASSESSMENT OF PROPOSED ELECTRIC-DISCHARGE <span class="hlt">NON-THERMAL</span> PLASMA FIELD-PILOT DEMONSTRATION UNITS FOR NOX REMOVAL IN JET-ENGINE EXHAUST: WHITE PAPER FOR SERDP PROJECT CP-1038</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://oaspub.epa.gov/eims/query.page">EPA Science Inventory</a></p> <p class="result-summary">This project is currently evaluating <span class="hlt">non-thermal</span> plasma (NTP) technologies for treating jet-engine exhaust arising from DoD test facilities. In the past, some economic analyses for NTP de-NOx have shown that it is not economical, compared to other techniques. The main reasons fo...</p> <div class="credits"> <p class="dwt_author"></p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">400</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://oaspub.epa.gov/eims/eimsapi.dispdetail?deid=20148"> <span id="translatedtitle">DEVELOPMENT OF SCALING ALGORITHMS AND ECONOMIC EVALUATION FOR <span class="hlt">NON-THERMAL</span> PLASMA REACTORS - ADSORBANT/CATALYZER HYBRID SYSTEM FOR CONTROL OF NOX RELEASED DURING ARMY AND RELATED U.S. DEPARTMENT OF DEF</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://oaspub.epa.gov/eims/query.page">EPA Science Inventory</a></p> <p class="result-summary">Computer code (SUENTP-J) to predict scale-up and economic evaluation of several eligible <span class="hlt">non-thermal</span> plasma processes for air pollution control - electron beam process, pulsed corona process, and corona radical shower process - was developed for a commercial power plant. This cod...</p> <div class="credits"> <p class="dwt_author"></p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div id="filter_results_form" class="filter_results_form floatContainer" style="visibility: visible;"> <div style="width:100%" id="PaginatedNavigation" class="paginatedNavigationElement"> <a id="FirstPageLink" onclick='return showDiv("page_1");' href="#" title="First Page"> <img id="FirstPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.first.18x20.png" alt="First Page" /></a> <a id="PreviousPageLink" onclick='return showDiv("page_19");' href="#" title="Previous Page"> <img id="PreviousPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.previous.18x20.png" alt="Previous Page" /></a> <span id="PageLinks" class="pageLinks"> <span> <a onClick='return showDiv("page_1");' href="#">1</a> <a onClick='return showDiv("page_2");' href="#">2</a> <a onClick='return showDiv("page_3");' href="#">3</a> <a 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href="#">11</a> <a onClick='return showDiv("page_12");' href="#">12</a> <a onClick='return showDiv("page_13");' href="#">13</a> <a onClick='return showDiv("page_14");' href="#">14</a> <a onClick='return showDiv("page_15");' href="#">15</a> <a onClick='return showDiv("page_16");' href="#">16</a> <a onClick='return showDiv("page_17");' href="#">17</a> <a onClick='return showDiv("page_18");' href="#">18</a> <a onClick='return showDiv("page_19");' href="#">19</a> <a onClick='return showDiv("page_20");' href="#">20</a> <a style="font-weight: bold;">21</a> <a onClick='return showDiv("page_22");' href="#">22</a> <a onClick='return showDiv("page_23");' href="#">23</a> <a onClick='return showDiv("page_24");' href="#">24</a> <a onClick='return showDiv("page_25");' href="#">25</a> </span> </span> <a id="NextPageLink" onclick='return showDiv("page_22");' href="#" title="Next Page"> <img id="NextPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.next.18x20.png" alt="Next Page" /></a> <a id="LastPageLink" onclick='return showDiv("page_25.0");' href="#" title="Last Page"> <img id="LastPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.last.18x20.png" alt="Last Page" /></a> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">401</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3530450"> <span id="translatedtitle">Effects of a <span class="hlt">Non</span> <span class="hlt">Thermal</span> Plasma Treatment Alone or in Combination with Gemcitabine in a MIA PaCa2-luc Orthotopic Pancreatic Carcinoma Model</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p class="result-summary">Pancreatic tumors are the gastrointestinal cancer with the worst prognosis in humans and with a survival rate of 5% at 5 years. Nowadays, no chemotherapy has demonstrated efficacy in terms of survival for this cancer. Previous study focused on the development of a new therapy by <span class="hlt">non</span> <span class="hlt">thermal</span> plasma showed significant effects on tumor growth for colorectal carcinoma and glioblastoma. To allow targeted treatment, a fibered plasma (Plasma Gun) was developed and its evaluation was performed on an orthotopic mouse model of human pancreatic carcinoma using a MIA PaCa2-luc bioluminescent cell line. The aim of this study was to characterize this pancreatic carcinoma model and to determine the effects of Plasma Gun alone or in combination with gemcitabine. During a 36 days period, quantitative BLI could be used to follow the tumor progression and we demonstrated that plasma gun induced an inhibition of MIA PaCa2-luc cells proliferation in vitro and in vivo and that this effect could be improved by association with gemcitabine possibly thanks to its radiosensitizing properties.</p> <div class="credits"> <p class="dwt_author">Brulle, Laura; Vandamme, Marc; Ries, Delphine; Martel, Eric; Robert, Eric; Lerondel, Stephanie; Trichet, Valerie; Richard, Serge; Pouvesle, Jean-Michel; Le Pape, Alain</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">402</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2013JPhD...46P5401N"> <span id="translatedtitle">Evaluation of extra- and intracellular OH radical generation, cancer cell injury, and apoptosis induced by a <span class="hlt">non-thermal</span> atmospheric-pressure plasma jet</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">In this study, we investigated the effects of a <span class="hlt">non-thermal</span> atmospheric-pressure plasma jet inducing extracellular and intracellular OH radical generation as well as cell injury and apoptosis for the cultured human breast cancer cells. Increased OH radical generation in the extracellular culture medium (liquid phase) was observed with increased irradiation time, distance to the liquid surface, and voltage. From the voltage-response relationships for two breast cancer cell lines (invasive MDA-MB-231 cells and non-invasive MCF-7 cells) and normal breast cells (HMEC), the half-maximal effective peak-to-peak voltage (EV50) values were 16.7 ± 0.3 kV, 15.0 ± 0.4 kV and 11.2 ± 0.7 kV for MDA-MB-231, MCF-7 and HMEC cells, respectively. This indicated that there was almost no selective cancer cell injury induced by plasma jet irradiation under these conditions. Compared with control condition without a plasma jet, intracellular OH radical accumulation and apoptotic cells were observed with a plasma jet using conditions that induced injury to 50% of cells irrespective of the cancer cell line.</p> <div class="credits"> <p class="dwt_author">Ninomiya, Kazuaki; Ishijima, Tatsuo; Imamura, Masatoshi; Yamahara, Takayuki; Enomoto, Hiroshi; Takahashi, Kenji; Tanaka, Yasunori; Uesugi, Yoshihiko; Shimizu, Nobuaki</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-10-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">403</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2013JPhD...46s5201K"> <span id="translatedtitle">Development of ultra-hydrophilic and non-cytotoxic dental vinyl polysiloxane impression materials using a <span class="hlt">non-thermal</span> atmospheric-pressure plasma jet</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Dental vinyl polysiloxane (VPS) impression materials are widely used for the replication of intraoral tissue where hydrophilicity is important as the oral tissues are surrounded by wet saliva. Recent attempts to improve the wettability of VPS using a ‘surfactant’, however, have resulted in a high level of cytotoxicity. Hence, in this study, application of a <span class="hlt">non-thermal</span> atmospheric-pressure plasma jet (NTAPPJ) on VPS and its effects in terms of both hydrophilicity and cytotoxicity were investigated. The results showed that the application of the plasma j