Sample records for neptune gj 436b

  1. COMPOSITIONAL DIVERSITY IN THE ATMOSPHERES OF HOT NEPTUNES, WITH APPLICATION TO GJ 436b

    DOE Office of Scientific and Technical Information (OSTI.GOV)

    Moses, J. I.; Line, M. R.; Visscher, C.

    2013-11-01

    Neptune-sized extrasolar planets that orbit relatively close to their host stars—often called {sup h}ot Neptunes{sup —}are common within the known population of exoplanets and planetary candidates. Similar to our own Uranus and Neptune, inefficient accretion of nebular gas is expected produce hot Neptunes whose masses are dominated by elements heavier than hydrogen and helium. At high atmospheric metallicities of 10-10,000 times solar, hot Neptunes will exhibit an interesting continuum of atmospheric compositions, ranging from more Neptune-like, H{sub 2}-dominated atmospheres to more Venus-like, CO{sub 2}-dominated atmospheres. We explore the predicted equilibrium and disequilibrium chemistry of generic hot Neptunes and find thatmore » the atmospheric composition varies strongly as a function of temperature and bulk atmospheric properties such as metallicity and the C/O ratio. Relatively exotic H{sub 2}O, CO, CO{sub 2}, and even O{sub 2}-dominated atmospheres are possible for hot Neptunes. We apply our models to the case of GJ 436b, where we find that a CO-rich, CH{sub 4}-poor atmosphere can be a natural consequence of a very high atmospheric metallicity. From comparisons of our results with Spitzer eclipse data for GJ 436b, we conclude that although the spectral fit from the high-metallicity forward models is not quite as good as the best fit obtained from pure retrieval methods, the atmospheric composition predicted by these forward models is more physically and chemically plausible in terms of the relative abundance of major constituents. High-metallicity atmospheres (orders of magnitude in excess of solar) should therefore be considered as a possibility for GJ 436b and other hot Neptunes.« less

  2. An HST/STIS Optical Transmission Spectrum of Warm Neptune GJ 436b

    NASA Astrophysics Data System (ADS)

    Lothringer, Joshua D.; Benneke, Björn; Crossfield, Ian J. M.; Henry, Gregory W.; Morley, Caroline; Dragomir, Diana; Barman, Travis; Knutson, Heather; Kempton, Eliza; Fortney, Jonathan; McCullough, Peter; Howard, Andrew W.

    2018-02-01

    GJ 436b is a prime target for understanding warm Neptune exoplanet atmospheres and a target for multiple James Webb Space Telescope (JWST) Guaranteed Time Observation programs. Here, we report the first space-based optical transmission spectrum of the planet using two Hubble Space Telescope (HST) Space Telescope Imaging Spectrograph (STIS) transit observations from 0.53 to 1.03 μm. We find no evidence for alkali absorption features, nor evidence of a scattering slope longward of 0.53 μm. The spectrum is indicative of moderate to high metallicity (∼100–1000× solar), while moderate-metallicity scenarios (∼100× solar) require aerosol opacity. The optical spectrum also rules out some highly scattering haze models. We find an increase in transit depth around 0.8 μm in the transmission spectra of three different sub-Jovian exoplanets (GJ 436b, HAT-P-26b, and GJ 1214b). While most of the data come from STIS, data from three other instruments may indicate this is not an instrumental effect. Only the transit spectrum of GJ 1214b is well fit by a model with stellar plages on the photosphere of the host star. Our photometric monitoring of the host star reveals a stellar rotation rate of 44.1 days and an activity cycle of 7.4 years. Intriguingly, GJ 436 does not become redder as it gets dimmer, which is expected if star spots were dominating the variability. These insights into the nature of the GJ 436 system help refine our expectations for future observations in the era of JWST, whose higher precision and broader wavelength coverage will shed light on the composition and structure of GJ 436b’s atmosphere.

  3. HELIUM ATMOSPHERES ON WARM NEPTUNE- AND SUB-NEPTUNE-SIZED EXOPLANETS AND APPLICATIONS TO GJ 436b

    DOE Office of Scientific and Technical Information (OSTI.GOV)

    Hu, Renyu; Yung, Yuk L.; Seager, Sara, E-mail: renyu.hu@jpl.nasa.gov

    2015-07-01

    Warm Neptune- and sub-Neptune-sized exoplanets in orbits smaller than Mercury’s are thought to have experienced extensive atmospheric evolution. Here we propose that a potential outcome of this atmospheric evolution is the formation of helium-dominated atmospheres. The hydrodynamic escape rates of Neptune- and sub-Neptune-sized exoplanets are comparable to the diffusion-limited escape rate of hydrogen, and therefore the escape is heavily affected by diffusive separation between hydrogen and helium. A helium atmosphere can thus be formed—from a primordial hydrogen–helium atmosphere—via atmospheric hydrodynamic escape from the planet. The helium atmosphere has very different abundances of major carbon and oxygen species from those ofmore » a hydrogen atmosphere, leading to distinctive transmission and thermal emission spectral features. In particular, the hypothesis of a helium-dominated atmosphere can explain the thermal emission spectrum of GJ 436b, a warm Neptune-sized exoplanet, while also being consistent with the transmission spectrum. This model atmosphere contains trace amounts of hydrogen, carbon, and oxygen, with the predominance of CO over CH{sub 4} as the main form of carbon. With our atmospheric evolution model, we find that if the mass of the initial atmosphere envelope is 10{sup −3} planetary mass, hydrodynamic escape can reduce the hydrogen abundance in the atmosphere by several orders of magnitude in ∼10 billion years. Observations of exoplanet transits may thus detect signatures of helium atmospheres and probe the evolutionary history of small exoplanets.« less

  4. Orbital misalignment of the Neptune-mass exoplanet GJ 436b with the spin of its cool star

    NASA Astrophysics Data System (ADS)

    Bourrier, Vincent; Lovis, Christophe; Beust, Hervé; Ehrenreich, David; Henry, Gregory W.; Astudillo-Defru, Nicola; Allart, Romain; Bonfils, Xavier; Ségransan, Damien; Delfosse, Xavier; Cegla, Heather M.; Wyttenbach, Aurélien; Heng, Kevin; Lavie, Baptiste; Pepe, Francesco

    2018-01-01

    The angle between the spin of a star and the orbital planes of its planets traces the history of the planetary system. Exoplanets orbiting close to cool stars are expected to be on circular, aligned orbits because of strong tidal interactions with the stellar convective envelope. Spin–orbit alignment can be measured when the planet transits its star, but such ground-based spectroscopic measurements are challenging for cool, slowly rotating stars. Here we report the three-dimensional characterization of the trajectory of an exoplanet around an M dwarf star, derived by mapping the spectrum of the stellar photosphere along the chord transited by the planet. We find that the eccentric orbit of the Neptune-mass exoplanet GJ 436b is nearly perpendicular to the stellar equator. Both eccentricity and misalignment, surprising around a cool star, can result from dynamical interactions (via Kozai migration) with a yet-undetected outer companion. This inward migration of GJ 436b could have triggered the atmospheric escape that now sustains its giant exosphere.

  5. Investigating an SPI and Measuring Baseline FUV Variability in the GJ 436 Hot-Neptune System

    NASA Astrophysics Data System (ADS)

    Loyd, R. O.

    2017-08-01

    Closely-orbiting, massive planets can measurably affect the activity of their host star through tides, magnetic disturbances, or even mass transfer. Observations of these star planet interactions (SPIs) provide a window into stellar and planetary physics that may eventually lead to constraints on planetary magnetic fields. Recently, the MUSCLES Treasury Survey of 11 exoplanet host stars revealed correlations providing the first-ever evidence of SPIs in M dwarf systems. This evidence additionally suggests that N V 1238,1242 Angstrom emission best traces SPIs, a feature that merits further investigation. To this end, we propose an experiment using the M dwarf + hot Neptune system GJ 436 that will also benefit upcoming transit observations. GJ 436 is ideal for an SPI experiment because (1) escaped gas from its known rapidly evaporating hot Neptune could be funneled onto the star and (2) it displays a tentative SPI signal in existing, incomplete N V observations. The proposed experiment will complete these N V observations to constrain a model of modulation in N V flux resulting from a stellar hot spot induced by the planet. The results will provide evidence for or against hot spot SPIs producing the correlations observed in the MUSCLES Survey. Furthemore, the acquired data will establish a broader FUV baseline to constrain day-timescale variability and facular emission in FUV lines, needed for the interpretation of upcoming transit observations of GJ 436b. For this reason, we waive our proprietary rights to the data. Establishing GJ 436's baseline FUV variability and testing the hot spot hypothesis are only possible through the FUV capabilities of HST.

  6. Transmission Spectra of Transiting Planet Atmospheres: Model Validation and Simulations of the Hot Neptune GJ 436b for the James Webb Space Telescope

    NASA Astrophysics Data System (ADS)

    Shabram, Megan; Fortney, Jonathan J.; Greene, Thomas P.; Freedman, Richard S.

    2011-02-01

    We explore the transmission spectrum of the Neptune-class exoplanet GJ 436b, including the possibility that its atmospheric opacity is dominated by a variety of nonequilibrium chemical products. We also validate our transmission code by demonstrating close agreement with analytic models that use only Rayleigh scattering or water vapor opacity. We find broad disagreement with radius variations predicted by another published model. For GJ 436b, the relative coolness of the planet's atmosphere, along with its implied high metallicity, may make it dissimilar in character compared to "hot Jupiters." Some recent observational and modeling efforts suggest low relative abundances of H2O and CH4 present in GJ 436b's atmosphere, compared to calculations from equilibrium chemistry. We include these characteristics in our models and examine the effects of absorption from methane-derived higher-order hydrocarbons. To our knowledge, the effects of these nonequilibrium chemical products on the spectra of close-in giant planets have not previously been investigated. Significant absorption from HCN and C2H2 is found throughout the infrared, while C2H4 and C2H6 are less easily seen. We perform detailed simulations of James Webb Space Telescope observations, including all likely noise sources, and find that we will be able to constrain chemical abundance regimes from this planet's transmission spectrum. For instance, the width of the features at 1.5, 3.3, and 7 μm indicates the amount of HCN versus C2H2 present. The NIRSpec prism mode will be useful due to its large spectral range and the relatively large number of photo-electrons recorded per spectral resolution element. However, extremely bright host stars like GJ 436 may be better observed with a higher spectroscopic resolution mode in order to avoid detector saturation. We find that observations with the MIRI low-resolution spectrograph should also have high signal-to-noise in the 5-10 μm range due to the brightness of the star

  7. The long egress of GJ 436b's giant exosphere

    NASA Astrophysics Data System (ADS)

    Lavie, B.; Ehrenreich, D.; Bourrier, V.; Lecavelier des Etangs, A.; Vidal-Madjar, A.; Delfosse, X.; Gracia Berna, A.; Heng, K.; Thomas, N.; Udry, S.; Wheatley, P. J.

    2017-09-01

    The M dwarf GJ 436 hosts a transiting warm Neptune known to experience atmospheric escape. Previous observations revealed the presence of a giant hydrogen exosphere transiting the star for more than 5 h, and absorbing up to 56% of the flux in the blue wing of the stellar Lyman-α line of neutral hydrogen (H I Lyα). The unexpected size of this comet-like exosphere prevented observing the full transit of its tail. In this Letter, we present new Lyα observations of GJ 436 obtained with the Space Telescope Imaging Spectrograph (STIS) instrument onboard the Hubble Space Telescope. The stability of the Lyα line over six years allowed us to combine these new observations with archival data sets, substantially expanding the coverage of the exospheric transit. Hydrogen atoms in the tail of the exospheric cloud keep occulting the star for 10-25 h after the transit of the planet, remarkably confirming a previous prediction based on 3D numerical simulations with the EVaporating Exoplanet code (EVE). This result strengthens the interpretation that the exosphere of GJ 436b is shaped by both radiative braking and charge exchanges with the stellar wind. We further report flux decreases of 15 ± 2% and 47 ± 10% in the red wing of the Lyα line and in the line of ionised silicon (Si III). Despite some temporal variability possibly linked with stellar activity, these two signals occur during the exospheric transit and could be of planetary origin. Follow-up observations will be required to assess the possibility that the redshifted Lyα and Si III absorption signatures arise from interactions between the exospheric flow and the magnetic field of the star.

  8. TRANSMISSION SPECTRA OF TRANSITING PLANET ATMOSPHERES: MODEL VALIDATION AND SIMULATIONS OF THE HOT NEPTUNE GJ 436b FOR THE JAMES WEBB SPACE TELESCOPE

    DOE Office of Scientific and Technical Information (OSTI.GOV)

    Shabram, Megan; Fortney, Jonathan J.; Greene, Thomas P.

    We explore the transmission spectrum of the Neptune-class exoplanet GJ 436b, including the possibility that its atmospheric opacity is dominated by a variety of nonequilibrium chemical products. We also validate our transmission code by demonstrating close agreement with analytic models that use only Rayleigh scattering or water vapor opacity. We find broad disagreement with radius variations predicted by another published model. For GJ 436b, the relative coolness of the planet's atmosphere, along with its implied high metallicity, may make it dissimilar in character compared to 'hot Jupiters'. Some recent observational and modeling efforts suggest low relative abundances of H{sub 2}Omore » and CH{sub 4} present in GJ 436b's atmosphere, compared to calculations from equilibrium chemistry. We include these characteristics in our models and examine the effects of absorption from methane-derived higher-order hydrocarbons. To our knowledge, the effects of these nonequilibrium chemical products on the spectra of close-in giant planets have not previously been investigated. Significant absorption from HCN and C{sub 2}H{sub 2} is found throughout the infrared, while C{sub 2}H{sub 4} and C{sub 2}H{sub 6} are less easily seen. We perform detailed simulations of James Webb Space Telescope observations, including all likely noise sources, and find that we will be able to constrain chemical abundance regimes from this planet's transmission spectrum. For instance, the width of the features at 1.5, 3.3, and 7 {mu}m indicates the amount of HCN versus C{sub 2}H{sub 2} present. The NIRSpec prism mode will be useful due to its large spectral range and the relatively large number of photo-electrons recorded per spectral resolution element. However, extremely bright host stars like GJ 436 may be better observed with a higher spectroscopic resolution mode in order to avoid detector saturation. We find that observations with the MIRI low-resolution spectrograph should also have high

  9. FORWARD AND INVERSE MODELING OF THE EMISSION AND TRANSMISSION SPECTRUM OF GJ 436B: INVESTIGATING METAL ENRICHMENT, TIDAL HEATING, AND CLOUDS

    DOE Office of Scientific and Technical Information (OSTI.GOV)

    Morley, Caroline V.; Knutson, Heather; Line, Michael

    The Neptune-mass GJ 436b is one of the most studied transiting exoplanets with repeated measurements of its thermal emission and transmission spectra. We build on previous studies to answer outstanding questions about this planet, including its potentially high metallicity and tidal heating of its interior. We present new observations of GJ 436b’s thermal emission at 3.6 and 4.5 μ m, which reduce uncertainties in estimates of GJ 436b’s flux at those wavelengths and demonstrate consistency between Spitzer observations spanning more than 7 yr. We analyze the Spitzer thermal emission photometry and Hubble WFC3 transmission spectrum. We use a dual-pronged modelingmore » approach of both self-consistent and retrieval models. We vary the metallicity, intrinsic luminosity from tidal heating, disequilibrium chemistry, and heat redistribution. We also study clouds and photochemical hazes, but do not find strong evidence for either. The self-consistent and retrieval models combine to suggest that GJ 436b has a high atmospheric metallicity, with best fits at or above several hundred times solar metallicity, tidal heating warming its interior with best-fit intrinsic effective temperatures around 300–350 K, and disequilibrium chemistry. High metal enrichments (>600× solar) occur from the accretion of rocky, rather than icy, material. Assuming the interior temperature T {sub int} ∼ 300–350 K, we find a dissipation factor Q ′ ∼ 2 × 10{sup 5}–10{sup 6}, larger than Neptune’s Q ′, implying a long tidal circularization timescale for the orbit. We suggest that Neptune-mass planets may be more diverse than imagined, with metal enhancements spanning several orders of magnitude, to perhaps over 1000× solar metallicity. High-fidelity observations with instruments like the James Webb Space Telescope will be critical for characterizing this diversity.« less

  10. Forward and Inverse Modeling of the Emission and Transmission Spectrum of GJ 436b: Investigating Metal Enrichment, Tidal Heating, and Clouds

    NASA Astrophysics Data System (ADS)

    Morley, Caroline V.; Knutson, Heather; Line, Michael; Fortney, Jonathan J.; Thorngren, Daniel; Marley, Mark S.; Teal, Dillon; Lupu, Roxana

    2017-02-01

    The Neptune-mass GJ 436b is one of the most studied transiting exoplanets with repeated measurements of its thermal emission and transmission spectra. We build on previous studies to answer outstanding questions about this planet, including its potentially high metallicity and tidal heating of its interior. We present new observations of GJ 436b’s thermal emission at 3.6 and 4.5 μm, which reduce uncertainties in estimates of GJ 436b’s flux at those wavelengths and demonstrate consistency between Spitzer observations spanning more than 7 yr. We analyze the Spitzer thermal emission photometry and Hubble WFC3 transmission spectrum. We use a dual-pronged modeling approach of both self-consistent and retrieval models. We vary the metallicity, intrinsic luminosity from tidal heating, disequilibrium chemistry, and heat redistribution. We also study clouds and photochemical hazes, but do not find strong evidence for either. The self-consistent and retrieval models combine to suggest that GJ 436b has a high atmospheric metallicity, with best fits at or above several hundred times solar metallicity, tidal heating warming its interior with best-fit intrinsic effective temperatures around 300-350 K, and disequilibrium chemistry. High metal enrichments (>600× solar) occur from the accretion of rocky, rather than icy, material. Assuming the interior temperature Tint ˜ 300-350 K, we find a dissipation factor Q‧ ˜ 2 × 105-106, larger than Neptune’s Q‧, implying a long tidal circularization timescale for the orbit. We suggest that Neptune-mass planets may be more diverse than imagined, with metal enhancements spanning several orders of magnitude, to perhaps over 1000× solar metallicity. High-fidelity observations with instruments like the James Webb Space Telescope will be critical for characterizing this diversity.

  11. A SEARCH FOR Hα ABSORPTION AROUND KELT-3 b AND GJ 436 b

    DOE Office of Scientific and Technical Information (OSTI.GOV)

    Cauley, P. Wilson; Redfield, Seth; Jensen, Adam G., E-mail: pcauley@wesleyan.edu

    2017-02-01

    Observations of extended atmospheres around hot planets have generated exciting results concerning the dynamics of escaping planetary material. The configuration of the escaping planetary gas can result in asymmetric transit features, producing both pre- and post-transit absorption in specific atomic transitions. Measuring the velocity and strength of the absorption can provide constraints on the mass loss mechanism, and potentially clues to the interactions between the planet and the host star. Here we present a search for H α absorption in the circumplanetary environments of the hot planets KELT-3 b and GJ 436 b. We find no evidence for absorption aroundmore » either planet at any point during the two separate transit epochs for which each system was observed. We provide upper limits on the radial extent and density of the excited hydrogen atmospheres around both planets. The null detection for GJ 436 b contrasts with the strong Ly α absorption measured for the same system, suggesting that the large cloud of neutral hydrogen is almost entirely in the ground state. The only confirmed exoplanetary H α absorption to date has been made around the active star HD 189733 b. KELT-3 and GJ 436 are less active than HD 189733, hinting that exoplanet atmospheres exposed to EUV photons from active stars are better suited for detection of H α absorption.« less

  12. A global analysis of Spitzer and new HARPS data confirms the loneliness and metal-richness of GJ 436 b

    NASA Astrophysics Data System (ADS)

    Lanotte, A. A.; Gillon, M.; Demory, B.-O.; Fortney, J. J.; Astudillo, N.; Bonfils, X.; Magain, P.; Delfosse, X.; Forveille, T.; Lovis, C.; Mayor, M.; Neves, V.; Pepe, F.; Queloz, D.; Santos, N.; Udry, S.

    2014-12-01

    Context. GJ 436b is one of the few transiting warm Neptunes for which a detailed characterisation of the atmosphere is possible, whereas its non-negligible orbital eccentricity calls for further investigation. Independent analyses of several individual datasets obtained with Spitzer have led to contradicting results attributed to the different techniques used to treat the instrumental effects. Aims: We aim at investigating these previous controversial results and developing our knowledge of the system based on the full Spitzer photometry dataset combined with new Doppler measurements obtained with the HARPS spectrograph. We also want to search for additional planets. Methods: We optimise aperture photometry techniques and the photometric deconvolution algorithm DECPHOT to improve the data reduction of the Spitzer photometry spanning wavelengths from 3-24 μm. Adding the high-precision HARPS radial velocity data, we undertake a Bayesian global analysis of the system considering both instrumental and stellar effects on the flux variation. Results: We present a refined radius estimate of RP = 4.10 ± 0.16 R⊕ , mass MP = 25.4 ± 2.1 M⊕, and eccentricity e = 0.162 ± 0.004 for GJ 436b. Our measured transit depths remain constant in time and wavelength, in disagreement with the results of previous studies. In addition, we find that the post-occultation flare-like structure at 3.6 μm that led to divergent results on the occultation depth measurement is spurious. We obtain occultation depths at 3.6, 5.8, and 8.0 μm that are shallower than in previous works, in particular at 3.6 μm. However, these depths still appear consistent with a metal-rich atmosphere depleted in methane and enhanced in CO/CO2, although perhaps less than previously thought. We could not detect a significant orbital modulation in the 8 μm phase curve. We find no evidence of a potential planetary companion, stellar activity, or a stellar spin-orbit misalignment. Conclusions: Recent theoretical

  13. Microphysical Modeling of Mineral Clouds in GJ1214 b and GJ436 b: Predicting Upper Limits on the Cloud-top Height

    NASA Astrophysics Data System (ADS)

    Ohno, Kazumasa; Okuzumi, Satoshi

    2018-05-01

    The ubiquity of clouds in the atmospheres of exoplanets, especially of super-Earths, is one of the outstanding issues for the transmission spectra survey. Understanding the formation process of clouds in super-Earths is necessary to interpret the observed spectra correctly. In this study, we investigate the vertical distributions of particle size and mass density of mineral clouds in super-Earths using a microphysical model that takes into account the vertical transport and growth of cloud particles in a self-consistent manner. We demonstrate that the vertical profiles of mineral clouds significantly vary with the concentration of cloud condensation nuclei and atmospheric metallicity. We find that the height of the cloud top increases with increasing metallicity as long as the metallicity is lower than the threshold. If the metallicity is larger than the threshold, the cloud-top height no longer increases appreciably with metallicity because coalescence yields larger particles of higher settling velocities. We apply our cloud model to GJ1214 b and GJ436 b, for which recent transmission observations suggest the presence of high-altitude opaque clouds. For GJ436 b, we show that KCl particles can ascend high enough to explain the observation. For GJ1214 b, by contrast, the height of KCl clouds predicted from our model is too low to explain its flat transmission spectrum. Clouds made of highly porous KCl particles could explain the observations if the atmosphere is highly metal-rich, and hence the particle microstructure might be a key to interpret the flat spectrum of GJ1214 b.

  14. RAYLEIGH SCATTERING IN THE ATMOSPHERE OF THE WARM EXO-NEPTUNE GJ 3470B

    DOE Office of Scientific and Technical Information (OSTI.GOV)

    Dragomir, Diana; Benneke, Björn; Pearson, Kyle A.

    2015-12-01

    GJ 3470b is a warm Neptune-size planet transiting an M dwarf star. Like the handful of other small exoplanets for which transmission spectroscopy has been obtained, GJ 3470b exhibits a flat spectrum in the near- and mid-infrared. Recently, a tentative detection of Rayleigh scattering in its atmosphere has been reported. This signal manifests itself as an observed increase of the planetary radius as a function of decreasing wavelength in the visible. We set out to verify this detection and observed several transits of this planet with the LCOGT network and the Kuiper telescope in four different bands (Sloan g, Sloanmore » i, Harris B, and Harris V). Our analysis reveals a strong Rayleigh scattering slope, thus confirming previous results. This makes GJ 3470b the smallest known exoplanet with a detection of Rayleigh scattering. We find that the most plausible scenario is a hydrogen/helium-dominated atmosphere covered by clouds which obscure absorption features in the infrared and hazes which give rise to scattering in the visible. Our results demonstrate the feasibility of exoplanet atmospheric characterization from the ground, even with meter-class telescopes.« less

  15. New follow-up study of the atmosphere of GJ1214b

    NASA Astrophysics Data System (ADS)

    Kabath, P.; Cáceres, C.; Hoyer, S.; Ivanov, V. D.; Rojo, P.; Girard, J. H.; Kempton, E. M.-R.; Fortney, J. J.; Minniti, D.

    2014-03-01

    GJ1214b is an extremely interesting 6.55Mearth and 2.6 Earth radii sub-Neptune planet orbiting a M-dwarf host. Its proximity, only 14pc, makes it an excellent target for studies of exoplanetary atmospheres (Charbonneau et al. 2009). Furthermore, the sub-Neptunes/Super Earth-sized planets are only one step between Jupiter-sized and habitable Earth-sized planets with a biosphere. Due to favorable parameters of GJ1214 system, we posses great coverage of many wavelengths in planetary transmission spectra from optical to NIR regions (Miller-Ricci & Fortney 2009). However, the scenarios for the atmospheric compositions are still open. Based on the available measurements, the solar composition (hydrogen rich) atmosphere can be most probably ruled out. That is given by fact that we observe rather a flat spectrum than the absorption features in the hydrogen rich model. Thus, currently more plausible models are atmosphere composed of heavy elements such as water or atmosphere covered by clouds (Bean, Desert, Kabath et al. 2011). Here, we present our spectrophotometric and photometric measurements obtained with SOI and OSIRIS instruments (both SOAR telescope) and SOFI (ESO NTT). We observed 5 transit events of GJ1214b and determined the Rp/Rs ratios for every measured wavelength (Caceres, Kabath, Hoyer et al. 2013). Our photometric measurements at 0.8 micron (Bessel-I) and at 2.14 micron (NIR narrow band) correlate with the flat transmission spectrum, therefore strongly supporting the water or cloudy atmosphere. Our spectrophotometric measurements in the H+K region do not posses the sufficient precision in the Rp/Rs ratios. We conclude that the hydrogen rich model is less probable. However, to be able to decide if the planetary atmosphere is hidden in clouds or if we encountered a water world, we still need more measurements with extremely high accuracy. Here, literally, every new point counts. Finally, we would like to present preliminary results obtained from our 2013

  16. Two nearby Sub-Earth-sized Exoplanet Candidates in the GJ 436 System

    NASA Astrophysics Data System (ADS)

    Stevenson, Kevin B.; Harrington, Joseph; Lust, Nate B.; Lewis, Nikole K.; Montagnier, Guillaume; Moses, Julianne I.; Visscher, Channon; Blecic, Jasmina; Hardy, Ryan A.; Cubillos, Patricio; Campo, Christopher J.

    2012-08-01

    We report the detection of UCF-1.01, a strong exoplanet candidate with a radius 0.66 ± 0.04 times that of Earth (R ⊕). This sub-Earth-sized planet transits the nearby M-dwarf star GJ 436 with a period of 1.365862 ± 8 × 10-6 days. We also report evidence of a 0.65 ± 0.06 R ⊕ exoplanet candidate (labeled UCF-1.02) orbiting the same star with an undetermined period. Using the Spitzer Space Telescope, we measure the dimming of light as the planets pass in front of their parent star to assess their sizes and orbital parameters. If confirmed today, UCF-1.01 and UCF-1.02 would be designated GJ 436c and GJ 436d, respectively, and would be part of the first multiple-transiting-planet system outside of the Kepler field. Assuming Earth-like densities of 5.515 g cm-3, we predict both candidates to have similar masses (~0.28 Earth-masses, M ⊕, 2.6 Mars-masses) and surface gravities of ~0.65 g (where g is the gravity on Earth). UCF-1.01's equilibrium temperature (T eq, where emitted and absorbed radiation balance for an equivalent blackbody) is 860 K, making the planet unlikely to harbor life as on Earth. Its weak gravitational field and close proximity to its host star imply that UCF-1.01 is unlikely to have retained its original atmosphere; however, a transient atmosphere is possible if recent impacts or tidal heating were to supply volatiles to the surface. We also present additional observations of GJ 436b during secondary eclipse. The 3.6 μm light curve shows indications of stellar activity, making a reliable secondary eclipse measurement impossible. A second non-detection at 4.5 μm supports our previous work in which we find a methane-deficient and carbon monoxide-rich dayside atmosphere.

  17. Atmospheric Circulation and Composition of GJ1214b

    NASA Astrophysics Data System (ADS)

    Menou, Kristen

    2012-01-01

    The exoplanet GJ1214b presents an interesting example of compositional degeneracy for low-mass planets. Its atmosphere may be composed of water, super-solar or solar metallicity material. We present atmospheric circulation models of GJ1214b for these three compositions, with explicit gray radiative transfer and an optional treatment of MHD bottom drag. All models develop strong, superrotating zonal winds (~1-2 km s-1). The degree of eastward heat advection, which can be inferred from secondary eclipse and thermal phase curve measurements, varies greatly between the models. These differences are understood as resulting from variations in the radiative times at the thermal photosphere, caused by separate molecular weight and opacity effects. Our GJ1214b models illustrate how atmospheric circulation can be used as a probe of composition for similar tidally locked exoplanets in the mini-Neptune/waterworld class.

  18. How to distinguish between cloudy mini-Neptunes and water/volatile-dominated super-Earths

    DOE Office of Scientific and Technical Information (OSTI.GOV)

    Benneke, Björn; Seager, Sara, E-mail: bbenneke@mit.edu

    One of the most profound questions about the newly discovered class of low-density super-Earths is whether these exoplanets are predominately H{sub 2}-dominated mini-Neptunes or volatile-rich worlds with gas envelopes dominated by H{sub 2}O, CO{sub 2}, CO, CH{sub 4}, or N{sub 2}. Transit observations of the super-Earth GJ 1214b rule out cloud-free H{sub 2}-dominated scenarios, but are not able to determine whether the lack of deep spectral features is due to high-altitude clouds or the presence of a high mean molecular mass atmosphere. Here, we demonstrate that one can unambiguously distinguish between cloudy mini-Neptunes and volatile-dominated worlds based on wing steepnessmore » and relative depths of absorption features in moderate-resolution near-infrared transmission spectra (R ∼ 100). In a numerical retrieval study, we show for GJ 1214b that an unambiguous distinction between a cloudy H{sub 2}-dominated atmosphere and cloud-free H{sub 2}O atmosphere will be possible if the uncertainties in the spectral transit depth measurements can be reduced by a factor of ∼3 compared to the published Hubble Space Telescope Wide-Field Camera 3 and Very Large Telescope transit observations by Berta et al. and Bean et al. We argue that the required precision for the distinction may be achievable with currently available instrumentation by stacking 10-15 repeated transit observations. We provide a scaling law that scales our quantitative results to other transiting super-Earths and Neptunes such as HD 97658b, 55 Cnc e, GJ 3470b and GJ 436b. The analysis in this work is performed using an improved version of our Bayesian atmospheric retrieval framework. The new framework not only constrains the gas composition and cloud/haze parameters, but also determines our confidence in having detected molecules and cloud/haze species through Bayesian model comparison. Using the Bayesian tool, we demonstrate quantitatively that the subtle transit depth variation in the Berta et al

  19. Super-Earths, Warm-Neptunes, and Hot-Jupiters: Transmission Spectroscopy for Comparative Planetology

    NASA Astrophysics Data System (ADS)

    Fraine, Jonathan D.; Deming, Drake; Knutson, Heather; Jordán, Andrés

    2014-11-01

    We used the Kepler, Hubble, and Spitzer Space Telescopes to probe the diversity of exoplanetary atmospheres with transmission spectroscopy, constraining atomic and molecular absorption in Jupiter- and Neptune-sized exoplanets. The detections and non-detections of molecular species such as water, methane, and carbon monoxide lead to greater understanding of planet formation and evolution. Recent significant advances in both theoretical and observational discoveries from planets like HD189733b, HD209458b, GJ436, as well as our own work with HAT-P-11b and GJ1214b, have shown that the range of measurable atmospheric properties spans from clear, molecular absorption dominated worlds to opaque worlds, with cloudy, hazy, or high mean molecular weight atmospheres. Characterization of these significant non-detections allows us to infer the existence of cloud compositions at high altitudes, or mean molecular weights upwards of ~1000x solar. Neither scenario was expected from extrapolations of solar system analogs. We present here our published results from GJ1214b and HAT-P-11b, as well as our recent work on HAT-P-7b and HAT-P-13b. We search for evidence of atmospheric hazes and clouds, and place constraints on the relative abundance of water vapor, methane, and carbon monoxide-- in the case of cloud-free atmospheres. We conclude by discussing how our results compare to transmission spectra obtained for other similar planets, and use these combined data to develop a better understanding for the nature of these distant and alien worlds.

  20. SEARCH FOR RAYLEIGH SCATTERING IN THE ATMOSPHERE OF GJ1214b

    DOE Office of Scientific and Technical Information (OSTI.GOV)

    De Mooij, E. J. W.; Jayawardhana, R.; Brogi, M.

    2013-07-10

    We investigate the atmosphere of GJ1214b, a transiting super-Earth planet with a low mean density, by measuring its transit depth as a function of wavelength in the blue optical portion of the spectrum. It is thought that this planet is either a mini-Neptune, consisting of a rocky core with a thick, hydrogen-rich atmosphere, or a planet with a composition dominated by water. Most observations favor a water-dominated atmosphere with a small scale-height, however, some observations indicate that GJ1214b could have an extended atmosphere with a cloud layer muting the molecular features. In an atmosphere with a large scale-height, Rayleigh scatteringmore » at blue wavelengths is likely to cause a measurable increase in the apparent size of the planet toward the blue. We observed the transit of GJ1214b in the B band with the FOcal Reducing Spectrograph at the Very Large Telescope and in the g band with both ACAM on the William Herschel Telescope (WHT) and the Wide Field Camera at the Isaac Newton Telescope (INT). We find a planet-to-star radius ratio in the B band of 0.1162 {+-} 0.0017, and in the g band 0.1180 {+-} 0.0009 and 0.1174 {+-} 0.0017 for the WHT and INT observations, respectively. These optical data do not show significant deviations from previous measurements at longer wavelengths. In fact, a flat transmission spectrum across all wavelengths best describes the combined observations. When atmospheric models are considered, a small scale-height water-dominated model fits the data best.« less

  1. 3D MODELING OF GJ1214b's ATMOSPHERE: FORMATION OF INHOMOGENEOUS HIGH CLOUDS AND OBSERVATIONAL IMPLICATIONS

    DOE Office of Scientific and Technical Information (OSTI.GOV)

    Charnay, B.; Meadows, V.; Misra, A.

    2015-11-01

    The warm sub-Neptune GJ1214b has a featureless transit spectrum that may be due to the presence of high and thick clouds or haze. Here, we simulate the atmosphere of GJ1214b with a 3D General Circulation Model for cloudy hydrogen-dominated atmospheres, including cloud radiative effects. We show that the atmospheric circulation is strong enough to transport micrometric cloud particles to the upper atmosphere and generally leads to a minimum of cloud at the equator. By scattering stellar light, clouds increase the planetary albedo to 0.4–0.6 and cool the atmosphere below 1 mbar. However, the heating by ZnS clouds leads to themore » formation of a stratospheric thermal inversion above 10 mbar, with temperatures potentially high enough on the dayside to evaporate KCl clouds. We show that flat transit spectra consistent with Hubble Space Telescope observations are possible if cloud particle radii are around 0.5 μm, and that such clouds should be optically thin at wavelengths >3 μm. Using simulated cloudy atmospheres that fit the observed spectra we generate transit, emission, and reflection spectra and phase curves for GJ1214b. We show that a stratospheric thermal inversion would be readily accessible in near- and mid-infrared atmospheric spectral windows. We find that the amplitude of the thermal phase curves is strongly dependent on metallicity, but only slightly impacted by clouds. Our results suggest that primary and secondary eclipses and phase curves observed by the James Webb Space Telescope in the near- to mid-infrared should provide strong constraints on the nature of GJ1214b's atmosphere and clouds.« less

  2. Kepler and Ground-Based Transits of the exo-Neptune HAT-P-11b

    NASA Technical Reports Server (NTRS)

    Deming, Drake; Sada, Pedro V.; Jackson, Brian; Peterson, Steven W.; Agol, Eric; Knutson, Heather A.; Jennings, Donald E.; Haase, Plynn; Bays, Kevin

    2011-01-01

    We analyze 26 archival Kepler transits of the exo-Neptune HAT-P-11b, supplemented by ground-based transits observed in the blue (B band) and near-IR (J band). Both the planet and host star are smaller than previously believed; our analysis yields Rp = 4.31 R xor 0.06 R xor and Rs = 0.683 R solar mass 0.009 R solar mass, both about 3 sigma smaller than the discovery values. Our ground-based transit data at wavelengths bracketing the Kepler bandpass serve to check the wavelength dependence of stellar limb darkening, and the J-band transit provides a precise and independent constraint on the transit duration. Both the limb darkening and transit duration from our ground-based data are consistent with the new Kepler values for the system parameters. Our smaller radius for the planet implies that its gaseous envelope can be less extensive than previously believed, being very similar to the H-He envelope of GJ 436b and Kepler-4b. HAT-P-11 is an active star, and signatures of star spot crossings are ubiquitous in the Kepler transit data. We develop and apply a methodology to correct the planetary radius for the presence of both crossed and uncrossed star spots. Star spot crossings are concentrated at phases 0.002 and +0.006. This is consistent with inferences from Rossiter-McLaughlin measurements that the planet transits nearly perpendicular to the stellar equator. We identify the dominant phases of star spot crossings with active latitudes on the star, and infer that the stellar rotational pole is inclined at about 12 deg 5 deg to the plane of the sky. We point out that precise transit measurements over long durations could in principle allow us to construct a stellar Butterfly diagram to probe the cyclic evolution of magnetic activity on this active K-dwarf star.

  3. Astrometric Discovery of GJ 164B

    NASA Technical Reports Server (NTRS)

    Pravdo, Steven H.; Shaklan, Stuart B.; Henry, Todd; Benedict, G. Fritz

    2004-01-01

    We discovered a low-mass companion to the M dwarf GJ 164 with the CCD-based imaging system of the Stellar Planet Survey astrometric program. The existence of GJ 164B was confirmed with Hubble Space Telescope NICMOS imaging observations. A high-dispersion spectral observation in V sets a lower limit of Deltam > 2.2 mag between the two components of the system. Based on our parallax value of 82 +/- 8 mas, we derive the following orbital parameters: P = 2.04 +/- 0.03 yr, a = 103 +/- 0.03, and M-total 0.265 +/- 0.020 M-circle dot. The component masses are M-A = 0.170 +/- 0.015 M-circle dot and M-B = 0.095 +/- 0/015 M-circle dot. Based on its mass, colors, and spectral properties, GJ 164B has spectral type M6-M8 V.

  4. Super-Earth and Sub-Neptune Exoplanets: a First Look from the MEarth Project

    NASA Astrophysics Data System (ADS)

    Berta, Zachory K.

    Exoplanets that transit nearby M dwarfs allow us to measure the sizes, masses, and atmospheric properties of distant worlds. Between 2008 and 2013, we searched for such planets with the MEarth Project, a photometric survey of the closest and smallest main-sequence stars. This thesis uses the first planet discovered with MEarth, the warm 2.7 Earth radius exoplanet GJ1214b, to explore the possibilities that planets transiting M dwarfs provide. First, we perform a broad reconnaissance of the GJ1214b planetary system to refine the system's physical properties. We fit many transits to improve the planetary parameters, use starspots to measure GJ1214's rotation period (>50 days), and search for additional transiting planets, placing strong limits on habitable-zone Neptune-sized exoplanets in the system. We present Hubble Space Telescope observations of GJ1214b's atmosphere. We find the transmission spectrum to be flat between 1.1 and 1.7 microns, ruling out at 8 sigma the presence of a clear hydrogen-rich envelope that had been proposed to explain GJ1214b's large radius. Additional observations will determine whether the absence of deep absorption features in GJ1214b's transmission spectrum is due to the masking influence of high altitude clouds or to the presence of a compact, hydrogen-poor atmosphere. We describe a new algorithm to find transiting planets in light curves plagued by stellar variability and systematic noise sources. This Method to Include Starspots and Systematics in the Marginalized Probability of a Lone Eclipse (MISS MarPLE) reliably assesses the significance of individual transit events, a necessary requirement for detecting habitable zone planets from the ground with MEarth. We compare MEarth's achieved sensitivity to planet occurrence statistics from the NASA Kepler Mission, and find that MEarth's single discovery of GJ1214b is consistent with expectations. We find that warm Neptunes are rare around mid-to-late M dwarfs (<0.15 planets

  5. Simultaneous multicolour optical and near-IR transit photometry of GJ 1214b with SOFIA

    NASA Astrophysics Data System (ADS)

    Angerhausen, D.; Dreyer, C.; Placek, B.; Csizmadia, Sz.; Eigmüller, Ph.; Godolt, M.; Kitzmann, D.; Mallonn, M.; Becklin, E. E.; Collins, P.; Dunham, E. W.; Grenfell, J. L.; Hamilton, R. T.; Kabath, P.; Logsdon, S. E.; Mandell, A.; Mandushev, G.; McElwain, M.; McLean, I. S.; Pfueller, E.; Rauer, H.; Savage, M.; Shenoy, S.; Vacca, W. D.; Van Cleve, J. E.; Wiedemann, M.; Wolf, J.

    2017-12-01

    Context. The benchmark exoplanet GJ 1214b is one of the best studied transiting planets in the transition zone between rocky Earth-sized planets and gas or ice giants. This class of super-Earth or mini-Neptune planets is unknown in our solar system, yet is one of the most frequently detected classes of exoplanets. Understanding the transition from rocky to gaseous planets is a crucial step in the exploration of extrasolar planetary systems, in particular with regard to the potential habitability of this class of planets. Aims: GJ 1214b has already been studied in detail from various platforms at many different wavelengths. Our airborne observations with the Stratospheric Observatory for Infrared Astronomy (SOFIA) add information in the Paschen-α cont. 1.9 μm infrared wavelength band, which is not accessible by any other current ground- or space-based instrument due to telluric absorption or limited spectral coverage. Methods: We used FLIPO, the combination of the High-speed Imaging Photometer for Occultations (HIPO) and the First Light Infrared TEst CAMera (FLITECAM) and the Focal Plane Imager (FPI+) on SOFIA to comprehensively analyse the transmission signal of the possible water-world GJ 1214b through photometric observations during transit in three optical and one infrared channels. Results: We present four simultaneous light curves and corresponding transit depths in three optical and one infrared channel, which we compare to previous observations and current synthetic atmospheric models of GJ 1214b. The final precision in transit depth is between 1.5 and 2.5 times the theoretical photon noise limit, not sensitive enough to constrain the theoretical models any better than previous observations. This is the first exoplanet observation with SOFIA that uses its full set of instruments available to exoplanet spectrophotometry. Therefore we use these results to evaluate SOFIA's potential in this field and suggest future improvements. Tables of the lightcurve data

  6. BROADBAND TRANSMISSION SPECTROSCOPY OF THE SUPER-EARTH GJ 1214b SUGGESTS A LOW MEAN MOLECULAR WEIGHT ATMOSPHERE

    DOE Office of Scientific and Technical Information (OSTI.GOV)

    Croll, Bryce; Jayawardhana, Ray; Albert, Loic

    We use the Wide-field Infrared Camera (WIRCam) on the Canada-France-Hawaii Telescope to observe four transits of the super-Earth planet GJ 1214b in the near-infrared. For each transit, we observe GJ 1214 in two bands nearly simultaneously by rapidly switching the WIRCam filter wheel back and forth for the duration of the observations. By combining all our J-band ({approx}1.25 {mu}m) observations we find a transit depth, analogous to the planet-to-star radius ratio squared, in this band of (R{sub PJ} /R{sub *}){sup 2} = (1.338 {+-} 0.013)%-a value consistent with the optical transit depth reported by Charbonneau and collaborators. However, our best-fitmore » combined K{sub s}-band ({approx}2.15 {mu}m) transit depth is deeper: (R{sub PKs} /R{sub *}){sup 2} = (1.438 {+-} 0.019)%. Formally, our K{sub s}-band transits are deeper than the J-band transits observed simultaneously by a factor of (R{sub PKs} /R{sub PJ}){sup 2} = 1.072 {+-} 0.018-a 4{sigma} discrepancy. The most straightforward explanation for our deeper K{sub s}-band transit depth is a spectral absorption feature from the limb of the atmosphere of the planet; for the spectral absorption feature to be this prominent, the atmosphere of GJ 1214b must have a large-scale height and a low mean molecular weight. That is, its atmosphere would have to be hydrogen/helium dominated and this planet would be better described as a mini-Neptune. However, recently published observations from 0.78 to 1.0 {mu}m, by Bean and collaborators, show a lack of spectral features and transit depths consistent with those obtained by Charbonneau and collaborators. The most likely atmospheric composition for GJ 1214b that arises from combining all these observations is less clear; if the atmosphere of GJ 1214b is hydrogen/helium dominated, then it must have either a haze layer that is obscuring transit-depth differences at shorter wavelengths or significantly different spectral features from what current models predict. Our

  7. Broadband Transmission Spectroscopy of the Super-Earth GJ 1214b Suggests a Low Mean Molecular Weight Atmosphere

    NASA Astrophysics Data System (ADS)

    Croll, Bryce; Albert, Loic; Jayawardhana, Ray; Miller-Ricci Kempton, Eliza; Fortney, Jonathan J.; Murray, Norman; Neilson, Hilding

    2011-08-01

    We use the Wide-field Infrared Camera (WIRCam) on the Canada-France-Hawaii Telescope to observe four transits of the super-Earth planet GJ 1214b in the near-infrared. For each transit, we observe GJ 1214 in two bands nearly simultaneously by rapidly switching the WIRCam filter wheel back and forth for the duration of the observations. By combining all our J-band (~1.25 μm) observations we find a transit depth, analogous to the planet-to-star radius ratio squared, in this band of (RPJ /R *)2 = (1.338 ± 0.013)%—a value consistent with the optical transit depth reported by Charbonneau and collaborators. However, our best-fit combined K s-band (~2.15 μm) transit depth is deeper: (RPKs /R *)2 = (1.438 ± 0.019)%. Formally, our K s-band transits are deeper than the J-band transits observed simultaneously by a factor of (RPKs /RPJ )2 = 1.072 ± 0.018—a 4σ discrepancy. The most straightforward explanation for our deeper K s-band transit depth is a spectral absorption feature from the limb of the atmosphere of the planet; for the spectral absorption feature to be this prominent, the atmosphere of GJ 1214b must have a large-scale height and a low mean molecular weight. That is, its atmosphere would have to be hydrogen/helium dominated and this planet would be better described as a mini-Neptune. However, recently published observations from 0.78 to 1.0 μm, by Bean and collaborators, show a lack of spectral features and transit depths consistent with those obtained by Charbonneau and collaborators. The most likely atmospheric composition for GJ 1214b that arises from combining all these observations is less clear; if the atmosphere of GJ 1214b is hydrogen/helium dominated, then it must have either a haze layer that is obscuring transit-depth differences at shorter wavelengths or significantly different spectral features from what current models predict. Our observations disfavor a water-world composition, but such a composition will remain a possibility for GJ 1214b

  8. Constraining the atmosphere of GJ 1214b using an optimal estimation technique

    NASA Astrophysics Data System (ADS)

    Barstow, J. K.; Aigrain, S.; Irwin, P. G. J.; Fletcher, L. N.; Lee, J.-M.

    2013-09-01

    We explore cloudy, extended H2-He atmosphere scenarios for the warm super-Earth GJ 1214b using an optimal estimation retrieval technique. This planet, orbiting an M4.5 star only 13 pc from the Earth, is of particular interest because it lies between the Earth and Neptune in size and may be a member of a new class of planet that is neither terrestrial nor gas giant. Its relatively flat transmission spectrum has so far made atmospheric characterization difficult. The Non-linear optimal Estimator for MultivariateE spectral analySIS (NEMESIS) algorithm is used to explore the degenerate model parameter space for a cloudy, H2-He-dominated atmosphere scenario. Optimal estimation is a data-led approach that allows solutions beyond the range permitted by ab initio equilibrium model atmosphere calculations, and as such prevents restriction from prior expectations. We show that optimal estimation retrieval is a powerful tool for this kind of study, and present an exploration of the degenerate atmospheric scenarios for GJ 1214b. Whilst we find a family of solutions that provide a very good fit to the data, the quality and coverage of these data are insufficient for us to more precisely determine the abundances of cloud and trace gases given an H2-He atmosphere, and we also cannot rule out the possibility of a high molecular weight atmosphere. Future ground- and space-based observations will provide the opportunity to confirm or rule out an extended H2-He atmosphere, but more precise constraints will be limited by intrinsic degeneracies in the retrieval problem, such as variations in cloud top pressure and temperature.

  9. WARM SPITZER PHOTOMETRY OF THREE HOT JUPITERS: HAT-P-3b, HAT-P-4b AND HAT-P-12b

    DOE Office of Scientific and Technical Information (OSTI.GOV)

    Todorov, Kamen O.; Deming, Drake; Knutson, Heather A.

    2013-06-20

    We present Warm Spitzer/IRAC secondary eclipse time series photometry of three short-period transiting exoplanets, HAT-P-3b, HAT-P-4b and HAT-P-12b, in both the available 3.6 and 4.5 {mu}m bands. HAT-P-3b and HAT-P-4b are Jupiter-mass objects orbiting an early K and an early G dwarf star, respectively. For HAT-P-3b we find eclipse depths of 0.112%+0.015%-0.030% (3.6 micron) and 0.094%+0.016%-0.009% (4.5 {mu}m). The HAT-P-4b values are 0.142%+0.014%-0.016% (3.6 micron) and 0.122%+0.012%-0.014% 4.5 {mu}m). The two planets' photometry is consistent with inefficient heat redistribution from their day to night sides (and low albedos), but it is inconclusive about possible temperature inversions in their atmospheres. HAT-P-12bmore » is a Saturn-mass planet and is one of the coolest planets ever observed during secondary eclipse, along with the hot Neptune GJ 436b and the hot Saturn WASP-29b. We are able to place 3{sigma} upper limits on the secondary eclipse depth of HAT-P-12b in both wavelengths: <0.042% (3.6 {mu}m) and <0.085% (4.5 {mu}m). We discuss these results in the context of the Spitzer secondary eclipse measurements of GJ 436b and WASP-29b. It is possible that we do not detect the eclipses of HAT-P-12b due to high eccentricity, but find that weak planetary emission in these wavelengths is a more likely explanation. We place 3{sigma} upper limits on the |e cos {omega}| quantity (where e is eccentricity and {omega} is the argument of periapsis) for HAT-P-3b (<0.0081) and HAT-P-4b (<0.0042), based on the secondary eclipse timings.« less

  10. Super-Earths, Warm Neptunes, and Hot Jupiters: Transmission Spectroscopy for Comparative Planetology

    NASA Astrophysics Data System (ADS)

    Fraine, Jonathan D.; Deming, Drake; Jordan, Andres; Knutson, Heather

    2015-01-01

    The detections and non-detections of molecular species in transiting planets-- such as water, methane, and carbon monoxide-- lead to greater understanding of planet formation and evolution. Recent significant advances in both theoretical and observational discoveries from planets like HD189733b, HD209458b, GJ436b, as well as our own work with HAT-P-11b and GJ1214b, have shown that the range of measurable atmospheric properties spans from clear, molecular absorption dominated worlds to opaque worlds, with cloudy, hazy, or high mean molecular weight atmospheres. Characterization of significant non-detections allowed us to infer the existence of opaque cloud layers at very high altitudes or mean molecular weights upwards of ~1000x solar. The prevalence of these atmospheres was unexpected from extrapolations of solar system analogs. I will present our published results from GJ1214b and HAT-P-11b, as well as our recent work using both Spitzer and Magellan. Our results, combined with transmission spectra obtained for other similar planets, connect to develop a better understanding about the nature of these distant and alien worlds

  11. THERMAL EVOLUTION AND STRUCTURE MODELS OF THE TRANSITING SUPER-EARTH GJ 1214b

    DOE Office of Scientific and Technical Information (OSTI.GOV)

    Nettelmann, N.; Fortney, J. J.; Kramm, U.

    The planet GJ 1214b is the second known super-Earth with a measured mass and radius. Orbiting a quiet M star, it receives considerably less mass-loss driving X-ray and UV radiation than CoRoT-7b, so that the interior may be quite dissimilar in composition, including the possibility of a large fraction of water. We model the interior of GJ 1214b assuming a two-layer (envelope+rock core) structure where the envelope material is either H/He, pure water, or a mixture of H/He and H{sub 2}O. Within this framework, we perform models of the thermal evolution and contraction of the planet. We discuss possible compositionsmore » that are consistent with M{sub p} = 6.55 M{sub +}, R{sub p} = 2.678 R{sub +}, an age {tau} = 3-10 Gyr, and the irradiation level of the atmosphere. These conditions require that if water exists in the interior, it must remain in a fluid state, with important consequences for magnetic field generation. These conditions also require the atmosphere to have a deep isothermal region extending down to 80-800 bar, depending on composition. Our results bolster the suggestion of a metal-enriched H/He atmosphere for the planet, as we find water-world models that lack an H/He atmosphere to require an implausibly large water-to-rock ratio of more than 6:1. We instead favor an H/He/H{sub 2}O envelope with high water mass fraction ({approx}0.5-0.85), similar to recent models of the deep envelope of Uranus and Neptune. Even with these high water mass fractions in the H/He envelope, generally the bulk composition of the planet can have subsolar water:rock ratios. Dry, water-enriched, and pure water envelope models differ to an observationally significant level in their tidal Love numbers k{sub 2} of, respectively, {approx}0.018, {approx}0.15, and {approx}0.7.« less

  12. Kepler planet-detection mission: introduction and first results.

    PubMed

    Borucki, William J; Koch, David; Basri, Gibor; Batalha, Natalie; Brown, Timothy; Caldwell, Douglas; Caldwell, John; Christensen-Dalsgaard, Jørgen; Cochran, William D; DeVore, Edna; Dunham, Edward W; Dupree, Andrea K; Gautier, Thomas N; Geary, John C; Gilliland, Ronald; Gould, Alan; Howell, Steve B; Jenkins, Jon M; Kondo, Yoji; Latham, David W; Marcy, Geoffrey W; Meibom, Søren; Kjeldsen, Hans; Lissauer, Jack J; Monet, David G; Morrison, David; Sasselov, Dimitar; Tarter, Jill; Boss, Alan; Brownlee, Don; Owen, Toby; Buzasi, Derek; Charbonneau, David; Doyle, Laurance; Fortney, Jonathan; Ford, Eric B; Holman, Matthew J; Seager, Sara; Steffen, Jason H; Welsh, William F; Rowe, Jason; Anderson, Howard; Buchhave, Lars; Ciardi, David; Walkowicz, Lucianne; Sherry, William; Horch, Elliott; Isaacson, Howard; Everett, Mark E; Fischer, Debra; Torres, Guillermo; Johnson, John Asher; Endl, Michael; MacQueen, Phillip; Bryson, Stephen T; Dotson, Jessie; Haas, Michael; Kolodziejczak, Jeffrey; Van Cleve, Jeffrey; Chandrasekaran, Hema; Twicken, Joseph D; Quintana, Elisa V; Clarke, Bruce D; Allen, Christopher; Li, Jie; Wu, Haley; Tenenbaum, Peter; Verner, Ekaterina; Bruhweiler, Frederick; Barnes, Jason; Prsa, Andrej

    2010-02-19

    The Kepler mission was designed to determine the frequency of Earth-sized planets in and near the habitable zone of Sun-like stars. The habitable zone is the region where planetary temperatures are suitable for water to exist on a planet's surface. During the first 6 weeks of observations, Kepler monitored 156,000 stars, and five new exoplanets with sizes between 0.37 and 1.6 Jupiter radii and orbital periods from 3.2 to 4.9 days were discovered. The density of the Neptune-sized Kepler-4b is similar to that of Neptune and GJ 436b, even though the irradiation level is 800,000 times higher. Kepler-7b is one of the lowest-density planets (approximately 0.17 gram per cubic centimeter) yet detected. Kepler-5b, -6b, and -8b confirm the existence of planets with densities lower than those predicted for gas giant planets.

  13. Thermochemistry and Photochemistry in Thick Atmospheres on Super Earths and Mini Neptunes

    NASA Astrophysics Data System (ADS)

    Hu, R.; Seager, S.

    2013-12-01

    Dectection and characterization of low-mass exoplanets is poised to accelerate in the coming decade. Some low-mass exoplanets, namely super Earths and some mini Neptunes, will likely have thick atmospheres that are not H2-dominated. We have developed a photochemistry-thermochemistry model for exploring the compositions of thick atmospheres on super Earths and mini Neptunes, applicable for both H2-dominated atmospheres and non-H2-dominated atmospheres. Using this model, we have simulated the molecular composition of thick atmospheres on warm and hot super Earths/mini Neptunes, and classified thick atmospheres into hydrogen-rich atmospheres, water-rich atmospheres, oxygen-rich atmospheres, and hydrocarbon-rich atmospheres, depending on the hydrogen abundance and the carbon to oxygen abundance ratio. We find that carbon has to be in the form of CO2 rather than CH4 or CO in an H2-depleted water-dominated thick atmosphere, and that the preferred loss of light elements from an oxygen-poor carbon-rich atmosphere leads to formation of unsaturated hydrocarbons. For future observations, we find for GJ 1214b that (1) C2H2 features at 1.0 and 1.5 μm in transmission are diagnostic for hydrocarbon-rich atmospheres; (2) a constraint on the thermal emission at 4.5 μm could differentiate water-rich atmospheres versus hydrocarbon-rich atmospheres; (3) a detection of water-vapor features and a confirmation of nonexistence of methane features would provide sufficient evidence for a water-dominated atmosphere. For a hot super Earth like 55 Cnc e, the diagnostic features of water-rich atmospheres (H2O) and the diagnostic features of hydrocarbon-rich atmospheres (CO and C2H2) are well separated in transmission spectra at 0.6-5 μm, which would enable straightforward characterization. In general, our simulations show that chemical stability has to be taken into account when interpreting the spectrum of a super Earth/mini Neptune. Theoretical transmission spectra and thermal emission

  14. Photochemistry in terrestrial exoplanet atmospheres. III. Photochemistry and thermochemistry in thick atmospheres on super Earths and mini Neptunes

    DOE Office of Scientific and Technical Information (OSTI.GOV)

    Hu, Renyu; Seager, Sara, E-mail: hury@caltech.edu

    Some super Earths and mini Neptunes will likely have thick atmospheres that are not H{sub 2}-dominated. We have developed a photochemistry-thermochemistry kinetic-transport model for exploring the compositions of thick atmospheres on super Earths and mini Neptunes, applicable for both H{sub 2}-dominated atmospheres and non-H{sub 2}-dominated atmospheres. Using this model to study thick atmospheres for wide ranges of temperatures and elemental abundances, we classify them into hydrogen-rich atmospheres, water-rich atmospheres, oxygen-rich atmospheres, and hydrocarbon-rich atmospheres. We find that carbon has to be in the form of CO{sub 2} rather than CH{sub 4} or CO in a H{sub 2}-depleted water-dominated thick atmospheremore » and that the preferred loss of light elements from an oxygen-poor carbon-rich atmosphere leads to the formation of unsaturated hydrocarbons (C{sub 2}H{sub 2} and C{sub 2}H{sub 4}). We apply our self-consistent atmosphere models to compute spectra and diagnostic features for known transiting low-mass exoplanets GJ 1214 b, HD 97658 b, and 55 Cnc e. For GJ 1214 b, we find that (1) C{sub 2}H{sub 2} features at 1.0 and 1.5 μm in transmission and C{sub 2}H{sub 2} and C{sub 2}H{sub 4} features at 9-14 μm in thermal emission are diagnostic for hydrocarbon-rich atmospheres; (2) a detection of water-vapor features and a confirmation of the nonexistence of methane features would provide sufficient evidence for a water-dominated atmosphere. In general, our simulations show that chemical stability has to be taken into account when interpreting the spectrum of a super Earth/mini Neptune. Water-dominated atmospheres only exist for carbon to oxygen ratios much lower than the solar ratio, suggesting that this kind of atmospheres could be rare.« less

  15. Ground-based transit observations of the super-Earth GJ 1214 b

    NASA Astrophysics Data System (ADS)

    Cáceres, C.; Kabath, P.; Hoyer, S.; Ivanov, V. D.; Rojo, P.; Girard, J. H.; Miller-Ricci Kempton, E.; Fortney, J. J.; Minniti, D.

    2014-05-01

    Context. GJ 1214 b is one of the few known transiting super-Earth-sized exoplanets with a measured mass and radius. It orbits an M-dwarf, only 14.55 pc away, making it a favorable candidate for follow-up studies. However, the composition of GJ 1214 b's mysterious atmosphere has yet to be fully unveiled. Aims: Our goal is to distinguish between the various proposed atmospheric models to explain the properties of GJ 1214 b: hydrogen-rich or hydrogen-He mix, or a heavy molecular weight atmosphere with reflecting high clouds, as latest studies have suggested. Methods: Wavelength-dependent planetary radii measurements from the transit depths in the optical/NIR are the best tool to investigate the atmosphere of GJ 1214 b. We present here (i) photometric transit observations with a narrow-band filter centered on 2.14 μm and a broad-band I-Bessel filter centered on 0.8665 μm, and (ii) transmission spectroscopy in the H and K atmospheric windows that cover three transits. The photometric and spectrophotometric time series obtained were analyzed with MCMC simulations to measure the planetary radii as a function of wavelength. We determined radii ratios of 0.1173-0.0024+0.0022 for I-Bessel and 0.11735-0.00076+0.00072 at 2.14 μm. Results: Our measurements indicate a flat transmission spectrum, in agreement with the last atmospheric models that favor featureless spectra with clouds and high molecular weight compositions. Based on observations obtained at the Southern Astrophysical Research (SOAR) Telescope, which is a joint project of the Ministério da Ciência, Tecnologia, e Inovação (MCTI) da República Federativa do Brasil, the US National Optical Astronomy Observatory (NOAO), the University of North Carolina at Chapel Hill (UNC), and Michigan State University (MSU). SofI results are based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 087.C-0509.Tables of the lightcurve data are only available at the CDS via anonymous

  16. Project 1640 Observations of Brown Dwarf GJ 758 B: Near-infrared Spectrum and Atmospheric Modeling

    NASA Astrophysics Data System (ADS)

    Nilsson, R.; Veicht, A.; Giorla Godfrey, P. A.; Rice, E. L.; Aguilar, J.; Pueyo, L.; Roberts, L. C., Jr.; Oppenheimer, R.; Brenner, D.; Luszcz-Cook, S. H.; Bacchus, E.; Beichman, C.; Burruss, R.; Cady, E.; Dekany, R.; Fergus, R.; Hillenbrand, L.; Hinkley, S.; King, D.; Lockhart, T.; Parry, I. R.; Sivaramakrishnan, A.; Soummer, R.; Vasisht, G.; Zhai, C.; Zimmerman, N. T.

    2017-03-01

    The nearby Sun-like star GJ 758 hosts a cold substellar companion, GJ 758 B, at a projected separation of ≲30 au, previously detected in high-contrast multi-band photometric observations. In order to better constrain the companion’s physical characteristics, we acquired the first low-resolution (R ˜ 50) near-infrared spectrum of it using the high-contrast hyperspectral imaging instrument Project 1640 on Palomar Observatory’s 5 m Hale telescope. We obtained simultaneous images in 32 wavelength channels covering the Y, J, and H bands (˜952-1770 nm), and used data processing techniques based on principal component analysis to efficiently subtract chromatic background speckle-noise. GJ 758 B was detected in four epochs during 2013 and 2014. Basic astrometric measurements confirm its apparent northwest trajectory relative to the primary star, with no clear signs of orbital curvature. Spectra of SpeX/IRTF observed T dwarfs were compared to the combined spectrum of GJ 758 B, with χ 2 minimization suggesting a best fit for spectral type T7.0 ± 1.0, but with a shallow minimum over T5-T8. Fitting of synthetic spectra from the BT-Settl13 model atmospheres gives an effective temperature T eff = 741 ± 25 K and surface gravity {log}g=4.3+/- 0.5 dex (cgs). Our derived best-fit spectral type and effective temperature from modeling of the low-resolution spectrum suggest a slightly earlier and hotter companion than previous findings from photometric data, but do not rule out current results, and confirm GJ 758 B as one of the coolest sub-stellar companions to a Sun-like star to date.

  17. 16 CFR Appendix B to Part 436 - Sample Item 20(1) Table-Systemwide Outlet Summary

    Code of Federal Regulations, 2014 CFR

    2014-01-01

    ... 16 Commercial Practices 1 2014-01-01 2014-01-01 false Sample Item 20(1) Table-Systemwide Outlet Summary B Appendix B to Part 436 Commercial Practices FEDERAL TRADE COMMISSION TRADE REGULATION RULES DISCLOSURE REQUIREMENTS AND PROHIBITIONS CONCERNING FRANCHISING Pt. 436, App. B Appendix B to Part 436—Sample...

  18. 16 CFR Appendix B to Part 436 - Sample Item 20(1) Table-Systemwide Outlet Summary

    Code of Federal Regulations, 2010 CFR

    2010-01-01

    ... 16 Commercial Practices 1 2010-01-01 2010-01-01 false Sample Item 20(1) Table-Systemwide Outlet Summary B Appendix B to Part 436 Commercial Practices FEDERAL TRADE COMMISSION TRADE REGULATION RULES DISCLOSURE REQUIREMENTS AND PROHIBITIONS CONCERNING FRANCHISING Pt. 436, App. B Appendix B to Part 436—Sample...

  19. Direct Imaging Detection of Methane in the Atmosphere of GJ 504 b

    NASA Technical Reports Server (NTRS)

    Janson, Markus; Brandt, Timothy; Kuzuhara, Masayuki; Spiegel, David; Thalmann, Christian; Currie, Thayne; Bonnefoy, Mickael; Zimmerman, Neil; Sorahana, Satoko; Kotani, Takayuki; hide

    2013-01-01

    Most exoplanets detected by direct imaging so far have been characterized by relatively hot (approximately greater than1000 K) and cloudy atmospheres. A surprising feature in some of their atmospheres has been a distinct lack of methane, possibly implying non-equilibrium chemistry. Recently, we reported the discovery of a planetary companion to the Sun-like star GJ 504 using Subaru/HiCIAO within the SEEDS survey. The planet is substantially colder (less than 600 K) than previously imaged planets, and has indications of fewer clouds, which implies that it represents a new class of planetary atmospheres with expected similarities to late T-type brown dwarfs in the same temperature range. If so, one might also expect the presence of significant methane absorption, which is characteristic of such objects. Here, we report the detection of deep methane absorption in the atmosphere of GJ 504 b, using the Spectral Differential Imaging mode of HiCIAO to distinguish the absorption feature around 1.6 micrometers. We also report updated JHK photometry based on new K(sub s)-band data and a re-analysis of the existing data. The results support the notion that GJ 504 b has atmospheric properties distinct from other imaged exoplanets, and will become a useful reference object for future planets in the same temperature range.

  20. HAT-P-26b: A Neptune-mass Exoplanet with Primordial Solar Heavy Element Abundance

    NASA Astrophysics Data System (ADS)

    Wakeford, Hannah; Sing, David; Deming, Drake; Kataria, Tiffany; Lopez, Eric

    2016-10-01

    A trend in giant planet mass and atmospheric heavy elemental abundance was first noted last century from observations of planets in our own solar system. These four data points from Jupiter, Saturn, Uranus, and Neptune have served as a corner stone of planet formation theory. Here we add another point in the mass-metallicity trend from a detailed observational study of the extrasolar planet HAT-P-26b, which inhabits the critical mass regime near Neptune and Uranus. Neptune-sized worlds are among the most common planets in our galaxy and frequently exist in orbital periods very different from that of our own solar system ice giants. Atmospheric studies are the principal window into these worlds, and thereby into their formation and evolution, beyond those of our own solar system. Using the Hubble Space Telescope and Spitzer, from the optical to the infrared, we conducted a detailed atmospheric study of the Neptune-mass exoplanet HAT-P-26b over 0.5 to 4.5 μm. We detect prominent H2O absorption at 1.4 μm to 525 ppm in the atmospheric transmission spectrum. We determine that HAT-P-26b's atmosphere is not rich in heavy elements (≈1.8×solar), which goes distinctly against the solar system mass-metallicity trend. This likely indicates that HAT-P-26b's atmosphere is primordial and obtained its gaseous envelope late in its disk lifetime with little contamination from metal-rich planetesimals.

  1. In Pursuit of New Worlds: Searches for and Studies of Transiting Exoplanets from Three Space-Based Observatories

    NASA Astrophysics Data System (ADS)

    Ballard, Sarah Ashley

    2012-01-01

    This thesis presents studies of transiting exoplanets using observations gathered in large part from space, with the NASA EPOXI Mission, the Spitzer Space Telescope, and the Kepler Mission. The first part of this thesis describes searches for additional transiting planets in known exoplanet systems, using time series photometry gathered as part of the NASA EPOXI Mission. Using the EPOXI light curves spanning weeks for each star, we searched six exoplanetary systems for signatures of additional transiting planets. These six systems include five hosts to hot Jupiters: HAT-P-4, TrES-3, TrES-2, WASP-3, and HAT-P-7, and one host to a hot Neptune: GJ 436. We place upper limits on the presence of additional transiting planets in the super-Earth radius range for GJ 436 in Chapter 2, and in the Neptune-to-Saturn radius range for the other five systems in Chapter 4. Chapter 3 details a search for additional transits of a hypothesized planet smaller than the Earth, whose presence was suggested by the EPOXI observations of GJ 436. In that study, we demonstrate the sensitivity of Warm Spitzer observations to transits of a sub-Earth-sized planet. The fifth chapter details the characterization and validation of the Kepler-19 system, which hosts a transiting 2.2 R⊕ planet, Kepler-19b. We demonstrate the planetary nature of the transit signal with an analysis that combines information from high-resolution spectroscopy, the shape of the transit light curve, adaptive optics imaging, and near-infrared transits of the planet. The sinusoidal variation in the transit times of Kepler-19b indicates the presence of an additional perturbing body, and comprises the first definitive detection of a planet using the transit timing variation method. While we cannot uniquely determine the mass and orbital period of Kepler-19c, we establish that its mass must be less than 6 times the mass of Jupiter. The sixth chapter presents evidence for the validation of a 2.0 R ⊕ planet residing in the

  2. THE LEECH EXOPLANET IMAGING SURVEY: CHARACTERIZATION OF THE COLDEST DIRECTLY IMAGED EXOPLANET, GJ 504 b, AND EVIDENCE FOR SUPERSTELLAR METALLICITY

    DOE Office of Scientific and Technical Information (OSTI.GOV)

    Skemer, Andrew J.; Leisenring, Jarron; Bailey, Vanessa

    2016-02-01

    As gas giant planets and brown dwarfs radiate away the residual heat from their formation, they cool through a spectral type transition from L to T, which encompasses the dissipation of cloud opacity and the appearance of strong methane absorption. While there are hundreds of known T-type brown dwarfs, the first generation of directly imaged exoplanets were all L type. Recently, Kuzuhara et al. announced the discovery of GJ 504 b, the first T dwarf exoplanet. GJ 504 b provides a unique opportunity to study the atmosphere of a new type of exoplanet with a ∼500 K temperature that bridges themore » gap between the first directly imaged planets (∼1000 K) and our own solar system's Jupiter (∼130 K). We observed GJ 504 b in three narrow L-band filters (3.71, 3.88, and 4.00 μm), spanning the red end of the broad methane fundamental absorption feature (3.3 μm) as part of the LBTI Exozodi Exoplanet Common Hunt (LEECH) exoplanet imaging survey. By comparing our new photometry and literature photometry with a grid of custom model atmospheres, we were able to fit GJ 504 b's unusual spectral energy distribution for the first time. We find that GJ 504 b is well fit by models with the following parameters: T{sub eff} = 544 ± 10 K, g < 600 m s{sup −2}, [M/H] = 0.60 ± 0.12, cloud opacity parameter of f{sub sed} = 2–5, R = 0.96 ± 0.07 R{sub Jup}, and log(L) = −6.13 ± 0.03 L{sub ⊙}, implying a hot start mass of 3–30 M{sub jup} for a conservative age range of 0.1–6.5 Gyr. Of particular interest, our model fits suggest that GJ 504 b has a superstellar metallicity. Since planet formation can create objects with nonstellar metallicities, while binary star formation cannot, this result suggests that GJ 504 b formed like a planet, not like a binary companion.« less

  3. THEORETICAL TRANSIT SPECTRA FOR GJ 1214b AND OTHER 'SUPER-EARTHS'

    DOE Office of Scientific and Technical Information (OSTI.GOV)

    Howe, Alex R.; Burrows, Adam S., E-mail: arhowe@astro.princeton.edu, E-mail: burrows@astro.princeton.edu

    2012-09-10

    We present new calculations of transit spectra of super-Earths that allow for atmospheres with arbitrary proportions of common molecular species and haze. We test this method with generic spectra, reproducing the expected systematics and absorption features, then apply it to the nearby super-Earth GJ 1214b, which has produced conflicting observational data, leaving the questions of a hydrogen-rich versus hydrogen-poor atmosphere and the water content of the atmosphere ambiguous. We present representative transit spectra for a range of classes of atmosphere models for GJ 1214b. Our analysis supports a hydrogen-rich atmosphere with a cloud or haze layer, although a hydrogen-poor modelmore » with {approx}<10% water is not ruled out. Several classes of models are ruled out, however, including hydrogen-rich atmospheres with no haze, hydrogen-rich atmospheres with a haze of {approx}0.01 {mu}m tholin particles, and hydrogen-poor atmospheres with major sources of absorption other than water. We propose an observational test to distinguish hydrogen-rich from hydrogen-poor atmospheres. Finally, we provide a library of theoretical transit spectra for super-Earths with a broad range of parameters to facilitate future comparison with anticipated data.« less

  4. Lyman-alpha transit observations of the warm rocky exoplanet GJ1132b

    NASA Astrophysics Data System (ADS)

    Waalkes, William; Berta-Thompson, Zachory K.; Charbonneau, David; Irwin, Jonathan; Newton, Elisabeth; Dittmann, Jason; Bourrier, Vincent; Ehrenreich, David; Kempton, Eliza; Will

    2018-06-01

    GJ1132b is one of the few known Earth-sized planets, and at 12pc away it is also one of the closest known transiting planets. With an equilibrium temperature of 500 K, this planet is too hot to be habitable but we can use it to learn about the presence and volatile content of rocky planet atmospheres around M dwarf stars. Using Hubble STIS spectra obtained during primary transit, we search for a Lyman-α transit. If we were to observe a deep Lyman-α transit, that would indicate the presence of a neutral hydrogen envelope flowing from GJ1132b. On the other hand, ruling out deep absorption from neutral hydrogen may indicate that this planet has either retained its volatiles or lost them very early in the star’s life. We carry out this analysis by extracting 1D spectra from the STIS pipeline, splitting the time-tagged spectra into higher resolution samples, and producing light curves of the red and blue wings of the Lyman-α line. We fit for the baseline stellar flux and transit depths in order to constrain the characteristics of the cloud of neutral hydrogen gas that may surround the planet. We do not conclusively detect a transit but the results provide an upper limit for the transit depth. We also analyze the stellar variability and Lyman-α spectrum of GJ1132, a slowly-rotating 0.18 solar mass M dwarf with previously uncharacterized UV activity. Understanding the role that UV variability plays in planetary atmospheres and volatile retention is crucial to assess atmospheric evolution and the habitability of cooler rocky planets.

  5. The LEECH Exoplanet Imaging Survey: Characterization of the Coldest Directly Imaged Exoplanet, GJ 504 b, and Evidence for Superstellar Metallicity

    NASA Astrophysics Data System (ADS)

    Skemer, Andrew J.; Morley, Caroline V.; Zimmerman, Neil T.; Skrutskie, Michael F.; Leisenring, Jarron; Buenzli, Esther; Bonnefoy, Mickael; Bailey, Vanessa; Hinz, Philip; Defrére, Denis; Esposito, Simone; Apai, Dániel; Biller, Beth; Brandner, Wolfgang; Close, Laird; Crepp, Justin R.; De Rosa, Robert J.; Desidera, Silvano; Eisner, Josh; Fortney, Jonathan; Freedman, Richard; Henning, Thomas; Hofmann, Karl-Heinz; Kopytova, Taisiya; Lupu, Roxana; Maire, Anne-Lise; Males, Jared R.; Marley, Mark; Morzinski, Katie; Oza, Apurva; Patience, Jenny; Rajan, Abhijith; Rieke, George; Schertl, Dieter; Schlieder, Joshua; Stone, Jordan; Su, Kate; Vaz, Amali; Visscher, Channon; Ward-Duong, Kimberly; Weigelt, Gerd; Woodward, Charles E.

    2016-02-01

    As gas giant planets and brown dwarfs radiate away the residual heat from their formation, they cool through a spectral type transition from L to T, which encompasses the dissipation of cloud opacity and the appearance of strong methane absorption. While there are hundreds of known T-type brown dwarfs, the first generation of directly imaged exoplanets were all L type. Recently, Kuzuhara et al. announced the discovery of GJ 504 b, the first T dwarf exoplanet. GJ 504 b provides a unique opportunity to study the atmosphere of a new type of exoplanet with a ˜500 K temperature that bridges the gap between the first directly imaged planets (˜1000 K) and our own solar system's Jupiter (˜130 K). We observed GJ 504 b in three narrow L-band filters (3.71, 3.88, and 4.00 μm), spanning the red end of the broad methane fundamental absorption feature (3.3 μm) as part of the LBTI Exozodi Exoplanet Common Hunt (LEECH) exoplanet imaging survey. By comparing our new photometry and literature photometry with a grid of custom model atmospheres, we were able to fit GJ 504 b's unusual spectral energy distribution for the first time. We find that GJ 504 b is well fit by models with the following parameters: Teff = 544 ± 10 K, g < 600 m s-2, [M/H] = 0.60 ± 0.12, cloud opacity parameter of fsed = 2-5, R = 0.96 ± 0.07 RJup, and log(L) = -6.13 ± 0.03 L⊙, implying a hot start mass of 3-30 Mjup for a conservative age range of 0.1-6.5 Gyr. Of particular interest, our model fits suggest that GJ 504 b has a superstellar metallicity. Since planet formation can create objects with nonstellar metallicities, while binary star formation cannot, this result suggests that GJ 504 b formed like a planet, not like a binary companion. The LBT is an international collaboration among institutions in the United States, Italy, and Germany. LBT Corporation partners are the University of Arizona on behalf of the Arizona university system; Istituto Nazionale di Astrophisica, Italy; LBT

  6. HAT-P-26b: A Neptune-mass Exoplanet with Primordial Solar Heavy Element Abundance

    NASA Astrophysics Data System (ADS)

    Wakeford, Hannah R.; Sing, David K.; Kataria, Tiffany; Deming, Drake; Nikolov, Nikolay; Lopez, Eric; Tremblin, Pascal; Skalid Amundsen, David; Lewis, Nikole K.; Mandell, Avi; Fortney, Jonathan J.; Knutson, Heather; Benneke, Björn; Evans, Tom M.

    2017-01-01

    A trend in giant planet mass and atmospheric heavy elemental abundance was first noted last century from observations of planets in our own solar system. These four data points from Jupiter, Saturn, Uranus, and Neptune have served as a corner stone of planet formation theory. Here we add another point in the mass-metallicity trend from a detailed observational study of the extrasolar planet HAT-P-26b, which inhabits the critical mass regime near Neptune and Uranus. Neptune-sized worlds are among the most common planets in our galaxy and frequently exist in orbital periods very different from that of our own solar system ice giants. Atmospheric studies are the principal window into these worlds, and thereby into their formation and evolution, beyond those of our own solar system. Using the Hubble Space Telescope and Spitzer, from the optical to the infrared, we conducted a detailed atmospheric study of the Neptune-mass exoplanet HAT-P-26b over 0.5 to 4.5 μm. We detect prominent H2O absorption at 1.4 μm to 525 ppm in the atmospheric transmission spectrum. We determine that HAT-P-26b’s atmosphere is not rich in heavy elements (≈1.8×solar), which goes distinctly against the solar system mass-metallicity trend. This likely indicates that HAT-P-26b’s atmosphere is primordial and obtained its gaseous envelope late in its disk lifetime with little contamination from metal-rich planetesimals.

  7. The Global and Small-scale Magnetic Fields of Fully Convective, Rapidly Spinning M Dwarf Pair GJ65 A and B

    DOE Office of Scientific and Technical Information (OSTI.GOV)

    Kochukhov, Oleg; Lavail, Alexis

    2017-01-20

    The nearby M dwarf binary GJ65 AB, also known as BL Cet and UV Cet, is a unique benchmark for investigation of dynamo-driven activity of low-mass stars. Magnetic activity of GJ65 was repeatedly assessed by indirect means, such as studies of flares, photometric variability, X-ray, and radio emission. Here, we present a direct analysis of large-scale and local surface magnetic fields in both components. Interpreting high-resolution circular polarization spectra (sensitive to a large-scale field geometry) we uncovered a remarkable difference of the global stellar field topologies. Despite nearly identical masses and rotation rates, the secondary exhibits an axisymmetric, dipolar-like globalmore » field with an average strength of 1.3 kG while the primary has a much weaker, more complex, and non-axisymmetric 0.3 kG field. On the other hand, an analysis of the differential Zeeman intensification (sensitive to the total magnetic flux) shows the two stars having similar magnetic fluxes of 5.2 and 6.7 kG for GJ65 A and B, respectively, although there is evidence that the field strength distribution in GJ65 B is shifted toward a higher field strength compared to GJ65 A. Based on these complementary magnetic field diagnostic results, we suggest that the dissimilar radio and X-ray variability of GJ65 A and B is linked to their different global magnetic field topologies. However, this difference appears to be restricted to the upper atmospheric layers but does not encompass the bulk of the stars and has no influence on the fundamental stellar properties.« less

  8. Exploring an Earth-sized neighbor: ground-based transmission spectroscopy of GJ1132b, a rocky planet transiting a small nearby M-dwarf

    NASA Astrophysics Data System (ADS)

    Diamond-Lowe, Hannah; Berta-Thompson, Zachory K.; Charbonneau, David; Irwin, Jonathan; Newton, Elisabeth R.; Dittmann, Jason

    2017-01-01

    The terrestrial planets of the Solar System are rocky worlds that did not accrete envelopes of hydrogen and helium, but instead possess thin secondary atmospheres, or no atmosphere at all. Until recently, most exoplanet atmospheric studies have centered around hot Jupiters, for which high planet-to-star radius ratios and short orbital periods allowed for observable transmission spectra. Now we have the opportunity to probe the atmosphere of a small, rocky exoplanet. GJ1132b has a radius of 1.2 Earth radii and a mass of 1.6 Earth masses, and orbits an M-dwarf 12 parsecs away. Determining the composition of GJ1132b's atmosphere is essential to understanding the nature of atmospheric evolution on terrestrial planets. We observed five transits of GJ1132b using the Magellan Clay telescope with the LDSS3C multi-object spectrograph. We compare the transit depth of GJ1132b in wavelength bins ranging from 0.65 -- 1.04 microns to infer whether or not GJ1132b has maintained its primordial hydrogen-dominated atmosphere. Should we find evidence of a hydrogen-dominated atmosphere, this would imply that a terrestrial planet is able to accrete and retain a low mean-molecular weight atmosphere from the planetary nebula. Coupled with recent UV spectra of the host star, our results can clarify the process of atmospheric escape on terrestrial worlds, with implications for formation histories of M-dwarf planets and the potential for habitability in these systems. If instead GJ1132b possesses a low mean-molecular weight atmosphere, we look to future observations with JWST and the ground-based extremely large telescopes to characterize its atmosphere.This material is based upon work supported by the National Science Foundation Graduate Research Fellowship Program. This work was made possible by a grant from the John Templeton Foundation.

  9. The Magnetic Binary GJ 65: A Test of Magnetic Diffusivity Effects

    NASA Astrophysics Data System (ADS)

    MacDonald, James; Mullan, D. J.; Dieterich, Sergio

    2018-06-01

    GJ 65 is an M dwarf binary system consisting of the two flare stars BL Cet (GJ 65A) and UV Cet (GJ 65B). Two teams of investigators have recently reported total magnetic fluxes corresponding to fields of 4.5 and 5.2 kG for GJ 65A and 5.8 and 6.7 kG for GJ 65B: for each component, the magnetic results obtained by the two teams agree with each other to within 1σ. For the first time, we can directly compare the predictions of our magneto-convective models, based on fitting observed stellar parameters, with measured field strengths. We find that our models agree with the observed field strengths, provided the effects of finite conductivity are accounted for. Thus, GJ 65 provides us with an opportunity to use observations of field strengths to distinguish between the predictions of our models that assume perfect electrical conductivity and those that allow for finite conductivity.

  10. Possible formation pathways for the low-density Neptune-mass planet HAT-P-26b

    NASA Astrophysics Data System (ADS)

    Ali-Dib, Mohamad; Lakhlani, Gunjan

    2018-01-01

    We investigate possible pathways for the formation of the low-density Neptune-mass planet HAT-P-26b. We use two different formation models based on pebble and planetesimal accretion, and includes gas accretion, disc migration and simple photoevaporation. The models track the atmospheric oxygen abundance, in addition to the orbital period, and mass of the forming planets, which we compare to HAT-P-26b. We find that pebble accretion can explain this planet more naturally than planetesimal accretion that fails completely unless we artificially enhance the disc metallicity significantly. Pebble accretion models can reproduce HAT-P-26b with either a high initial core mass and low amount of envelope enrichment through core erosion or pebbles dissolution, or the opposite, with both scenarios being possible. Assuming a low envelope enrichment factor as expected from convection theory and comparable to the values we can infer from the D/H measurements in Uranus and Neptune, our most probable formation pathway for HAT-P-26b is through pebble accretion starting around 10 au early in the disc's lifetime.

  11. A Comparison of Simulated JWST Observations Derived from Equilibrium and Non-equilibrium Chemistry Models of Giant Exoplanets

    NASA Astrophysics Data System (ADS)

    Blumenthal, Sarah D.; Mandell, Avi M.; Hébrard, Eric; Batalha, Natasha E.; Cubillos, Patricio E.; Rugheimer, Sarah; Wakeford, Hannah R.

    2018-02-01

    We aim to see if the difference between equilibrium and disequilibrium chemistry is observable in the atmospheres of transiting planets by the James Webb Space Telescope (JWST). We perform a case study comparing the dayside emission spectra of three planets like HD 189733b, WASP-80b, and GJ 436b, in and out of chemical equilibrium at two metallicities each. These three planets were chosen because they span a large range of planetary masses and equilibrium temperatures, from hot and Jupiter-sized to warm and Neptune-sized. We link the one-dimensional disequilibrium chemistry model from Venot et al. (2012), in which thermochemical kinetics, vertical transport, and photochemistry are taken into account, to the one-dimensional, pseudo line-by-line radiative transfer model, Pyrat bay, developed especially for hot Jupiters, and then simulate JWST spectra using PandExo for comparing the effects of temperature, metallicity, and radius. We find the most significant differences from 4 to 5 μm due to disequilibrium from CO and CO2 abundances, and also H2O for select cases. Our case study shows a certain “sweet spot” of planetary mass, temperature, and metallicity where the difference between equilibrium and disequilibrium is observable. For a planet similar to WASP-80b, JWST’s NIRSpec G395M can detect differences due to disequilibrium chemistry with one eclipse event. For a planet similar to GJ 436b, the observability of differences due to disequilibrium chemistry is possible at low metallicity given five eclipse events, but not possible at the higher metallicity.

  12. Constraints on Neutral Hydrogen Outflow from the Warm Rocky Planet GJ1132b using Lyman-alpha Transit Observations

    NASA Astrophysics Data System (ADS)

    Waalkes, William; Berta-Thompson, Zachory; Charbonneau, David; Irwin, Jonathan; Newton, Elisabeth; Dittmann, Jason; Bourrier, Vincent; Ehrenreich, David; Kempton, Eliza

    2018-01-01

    GJ1132b is one of the few known Earth-sized planets, and at 12 pc away it is also one of the closest known transiting planets. With an equilibrium temperature of 500 K, this planet is too hot to be habitable but we can use it to learn about the presence and volatile content of rocky planet atmospheres around M dwarf stars. Using Hubble STIS spectra during primary transit, we explore the potential for UV transit detections of GJ1132b. If we were to observe a deep Lyman-α transit, that would indicate the presence of a neutral hydrogen envelope flowing from GJ1132b. On the other hand, ruling out deep absorption from neutral hydrogen may indicate that this planet has either retained its volatiles or lost them very early in the star’s life. We carry out this analysis by extracting 1D spectra from the STIS pipeline, splitting the time-tagged spectra into higher resolution samples, and producing light curves of the red and blue wings of the Lyman-α line. We fit for the baseline stellar flux and transit depths in order to constrain the characteristics of the cloud of neutral hydrogen gas that may surround the planet. Our work extends beyond the transit study into an analysis of the stellar variability and Lyman-α spectrum of GJ1132, a slowly-rotating 0.18 MSun M dwarf with previously uncharacterized UV activity. Understanding the role that UV variability plays in planetary atmospheres and volatile retention is crucial to assess atmospheric evolution and the habitability of cooler rocky planets.

  13. Magellan/PFS Radial Velocities of GJ 9827, a Late K dwarf at 30 pc with Three Transiting Super-Earths

    NASA Astrophysics Data System (ADS)

    Teske, Johanna K.; Wang, Sharon; Wolfgang, Angie; Dai, Fei; Shectman, Stephen A.; Butler, R. Paul; Crane, Jeffrey D.; Thompson, Ian B.

    2018-04-01

    The Kepler mission showed us that planets with sizes between that of Earth and Neptune appear to be the most common type in our Galaxy. These “super-Earths” continue to be of great interest for exoplanet formation, evolution, and composition studies. However, the number of super-Earths with well-constrained mass and radius measurements remains small (40 planets with σ mass < 25%), due in part to the faintness of their host stars causing ground-based mass measurements to be challenging. Recently, three transiting super-Earth planets were detected by the K2 mission around the nearby star GJ 9827/HIP 115752, at only 30 pc away. The radii of the planets span the “radius gap” detected by Fulton et al. (2017), and all orbit within ∼6.5 days, easing follow-up observations. Here, we report radial velocity (RV) observations of GJ 9827, taken between 2010 and 2016 with the Planet Finder Spectrograph on the Magellan II Telescope. We employ two different RV analysis packages, SYSTEMIC and RADVEL, to derive masses and thus densities of the GJ 9827 planets. We also test a Gaussian Process regression analysis but find the correlated stellar noise is not well constrained by the PFS data and that the GP tends to over-fit the RV semi-amplitudes resulting in a lower K value. Our RV observations are not able to place strong mass constraints on the two outer planets (c and d) but do indicate that planet b, at 1.64 R ⊕ and ∼8 M ⊕, is one of the most massive (and dense) super-Earth planets detected to date.

  14. Neptune encounter highlights

    NASA Astrophysics Data System (ADS)

    1989-11-01

    Voyager encounter data are presented in computer animation (CA) and real (R) animation. The highlights include a view of 2 full rotations of Neptune. It shows spacecraft trajectory 'diving' over Neptune and intercepting Triton's orbit, depicting radiation and occulation zones. Also shown are a renegade orbit of Triton and Voyager's encounter with Neptune's Magnetopause. A model of the spacecraft's complex maneuvers during close encounters of Neptune and Triton is presented. A view from Earth of Neptune's occulation experiment is is shown as well as a recreation of Voyager's final pass. There is detail of Voyager's Image Compensation technique which produces Voyager images. Eighteen images were produced on June 22 - 23, 1989, from 57 million miles away. A 68 day sequence which provides a stroboscopic view - colorization approximates what is seen by the human eye. Real time images recorded live from Voyager on 8/24/89 are presented. Photoclinometry produced the topography of Triton. Three images are used to create a sequence of Neptune's rings. The globe of Neptune and 2 views of the south pole are shown as well as Neptune rotating. The rotation of a scooter is frozen in images showing differential motion. There is a view of rotation of the Great Dark Spot about its own axis. Photoclinometry provides a 3-dimensional perspective using a color mosaic of Triton images. The globe is used to indicate the orientation of Neptune's crescent. The east and west plumes on Triton are shown.

  15. High-Contrast 3.8 Micron Imaging of the Brown Dwarf/Planet-Mass Companion to GJ 758

    NASA Technical Reports Server (NTRS)

    Currie, Thayne; Bailey, Vanessa; Fabrycky, Daniel; Murray-Clay, Ruth; Rodigas, Timothy; Hinz, Phil

    2010-01-01

    We present L' band (3.8 Micron) MMT/Clio high-contrast imaging data for the nearby star GJ 758, which was recently reported by Thalmann et al. (2009) to have one -- possibly two-- faint comoving companions (GJ 7588 and "C", respectively). GJ 758B is detected in two distinct datasets. Additionally, we report a \\textit(possible) detection of the object identified by Thalmann et al as "GJ 758C" in our more sensitive dataset, though it is likely a residual speckle. However, if it is the same object as that reported by Thalmann et al. it cannot be a companion in a bound orbit. GJ 758B has a H-L'color redder than nearly all known L--T8 dwarfs. Based on comparisons with the COND evolutionary models, GJ 758B has Te approx. 560 K (+150 K, -90 K) and a mass ranging from approx. 10-20 Mj if it is approx. 1 Gyr old to approx. 25-40 Mj if it is 8.7 Gyr old. GJ 758B is likely in a highly eccentric orbit, e approx. 0.73 (+0.12,-0.21), with a semimajor axis of approx. 44 AU (+32 AU, -14 AU). Though GJ 758B is sometimes discussed within the context of exoplanet direct imaging, its mass is likely greater than the deuterium-burning limit and its formation may resemble that of binary stars rather than that of jovian-mass planets.

  16. Voyager: Neptune Encounter Highlights

    NASA Technical Reports Server (NTRS)

    1989-01-01

    Voyager encounter data are presented in computer animation (CA) and real (R) animation. The highlights include a view of 2 full rotations of Neptune. It shows spacecraft trajectory 'diving' over Neptune and intercepting Triton's orbit, depicting radiation and occulation zones. Also shown are a renegade orbit of Triton and Voyager's encounter with Neptune's Magnetopause. A model of the spacecraft's complex maneuvers during close encounters of Neptune and Triton is presented. A view from Earth of Neptune's occulation experiment is is shown as well as a recreation of Voyager's final pass. There is detail of Voyager's Image Compensation technique which produces Voyager images. Eighteen images were produced on June 22 - 23, 1989, from 57 million miles away. A 68 day sequence which provides a stroboscopic view - colorization approximates what is seen by the human eye. Real time images recorded live from Voyager on 8/24/89 are presented. Photoclinometry produced the topography of Triton. Three images are used to create a sequence of Neptune's rings. The globe of Neptune and 2 views of the south pole are shown as well as Neptune rotating. The rotation of a scooter is frozen in images showing differential motion. There is a view of rotation of the Great Dark Spot about its own axis. Photoclinometry provides a 3-dimensional perspective using a color mosaic of Triton images. The globe is used to indicate the orientation of Neptune's crescent. The east and west plumes on Triton are shown.

  17. 40 CFR 436.183-436.184 - [Reserved

    Code of Federal Regulations, 2011 CFR

    2011-07-01

    ... 40 Protection of Environment 30 2011-07-01 2011-07-01 false [Reserved] 436.183-436.184 Section 436.183-436.184 Protection of Environment ENVIRONMENTAL PROTECTION AGENCY (CONTINUED) EFFLUENT GUIDELINES AND STANDARDS MINERAL MINING AND PROCESSING POINT SOURCE CATEGORY Phosphate Rock Subcategory §§ 436...

  18. 40 CFR 436.183-436.184 - [Reserved

    Code of Federal Regulations, 2010 CFR

    2010-07-01

    ... 40 Protection of Environment 29 2010-07-01 2010-07-01 false [Reserved] 436.183-436.184 Section 436.183-436.184 Protection of Environment ENVIRONMENTAL PROTECTION AGENCY (CONTINUED) EFFLUENT GUIDELINES AND STANDARDS MINERAL MINING AND PROCESSING POINT SOURCE CATEGORY Phosphate Rock Subcategory §§ 436...

  19. Neptune's Stormy Disposition

    NASA Technical Reports Server (NTRS)

    1998-01-01

    Using powerful ground-and space-based telescopes, scientists have obtained a moving look at some of the wildest, weirdest weather in the solar system.

    Combining simultaneous observations of Neptune made with the Hubble Space Telescope and NASA's Infrared Telescope Facility on Mauna Kea, Hawaii, a team of scientists led by Lawrence A. Sromovsky of the University of Wisconsin-Madison has captured the most insightful images to date of a planet whose blustery weather -- monster storms and equatorial winds of 900 miles per hour -- bewilders scientists.

    Blending a series of Hubble images, Sromovsky's team constructed a time-lapse rotation movie of Neptune, permitting scientists to watch the ebb and flow of the distant planet's weather. And while the observations, presented here at a meeting of the American Astronomical Society's Division of Planetary Science, are helping scientists tease out clues to the planet's stormy weather, they also are deepening some of Neptune's mysteries, said Sromovsky.

    The weather on Neptune, the eighth planet from the sun, is an enigma to begin with. The mechanism that drives its near-supersonic winds and giant storms has yet to be discerned.

    On Earth, weather is driven by energy from the sun as it heats the atmosphere and oceans. On Neptune, the sun is 900 times dimmer and scientists have yet to understand how Neptune's weather-generating machinery can be so efficient.

    'It's an efficient weather machine compared to Earth,' said Sromovsky. 'It seems to run on almost no energy.'

    In an effort to dissect the distant planet's atmosphere and monitor its bizarre weather, Sromovsky and his colleagues obtained a series of measurements and images over the span of three of Neptune's rotations.

    From those observations, Sromovsky said it is possible to measure Neptune's circulation and view a 'strange menagerie of variable, discrete cloud features and zonal bands' of weather. Moreover, the new observations enabled Sromovsky's team to

  20. The JPL Neptune Radiation Model (NMOD)

    NASA Technical Reports Server (NTRS)

    Garrett, Henry; Evans, Robin

    2017-01-01

    The objective of this study is the development of a comprehensive radiation model of the Neptunian environment for JPL mission planning. The ultimate goal is to provide a description of the high-energy electron and proton environments and the magnetic field at Neptune that can be used for engineering design. The JPL Neptune Radiation Model (NMOD) models the high-energy electrons and protons between 0.025 MeV and 5 MeV based on the California Institute of Technology's Cosmic Ray Subsystem and the Applied Physics Laboratory's Low Energy Charged Particle Detector on Voyager 2. As in previous JPL radiation models, the form of the Neptunian model is based on magnetic field coordinates and requires a conversion from spacecraft coordinates to Neptunian-centered magnetic "B-L" coordinates. Two types of magnetic field models have been developed for Neptune: 1) simple "offset, tilted dipoles" (OTD), and 2) a complex, multi-pole expansion model ("O8"). A review of the existing data on Neptune and a search of the NASA Planetary Data System (PDS) were completed to obtain the most current descriptions of the Neptunian high-energy particle environment. These data were fit in terms of the O8 B-L coordinates to develop the electron and proton flux models. The flux predictions of the new model were used to estimate the total ionizing dose (TID) rate along the Neptunian equator, meridional flux contours for the electrons and protons, and for flux and dose comparisons with the other radiation belts in the Solar System.

  1. 40 CFR 436.183-436.184 - [Reserved

    Code of Federal Regulations, 2013 CFR

    2013-07-01

    ... 40 Protection of Environment 31 2013-07-01 2013-07-01 false [Reserved] 436.183-436.184 Section 436.183-436.184 Protection of Environment ENVIRONMENTAL PROTECTION AGENCY (CONTINUED) EFFLUENT GUIDELINES AND STANDARDS (CONTINUED) MINERAL MINING AND PROCESSING POINT SOURCE CATEGORY Phosphate Rock...

  2. 40 CFR 436.183-436.184 - [Reserved

    Code of Federal Regulations, 2012 CFR

    2012-07-01

    ... 40 Protection of Environment 31 2012-07-01 2012-07-01 false [Reserved] 436.183-436.184 Section 436.183-436.184 Protection of Environment ENVIRONMENTAL PROTECTION AGENCY (CONTINUED) EFFLUENT GUIDELINES AND STANDARDS (CONTINUED) MINERAL MINING AND PROCESSING POINT SOURCE CATEGORY Phosphate Rock...

  3. 40 CFR 436.183-436.184 - [Reserved

    Code of Federal Regulations, 2014 CFR

    2014-07-01

    ... 40 Protection of Environment 30 2014-07-01 2014-07-01 false [Reserved] 436.183-436.184 Section 436.183-436.184 Protection of Environment ENVIRONMENTAL PROTECTION AGENCY (CONTINUED) EFFLUENT GUIDELINES AND STANDARDS (CONTINUED) MINERAL MINING AND PROCESSING POINT SOURCE CATEGORY Phosphate Rock...

  4. Clouds and hazes in exoplanets and brown dwarfs

    NASA Astrophysics Data System (ADS)

    Morley, Caroline Victoria

    The formation of clouds significantly alters the spectra of cool substellar atmospheres from terrestrial planets to brown dwarfs. In cool planets like Earth and Jupiter, volatile species like water and ammonia condense to form ice clouds. In hot planets and brown dwarfs, iron and silicates instead condense, forming dusty clouds. Irradiated methane-rich planets may have substantial hydrocarbon hazes. During my dissertation, I have studied the impact of clouds and hazes in a variety of substellar objects. First, I present results for cool brown dwarfs including clouds previously neglected in model atmospheres. Model spectra that include sulfide and salt clouds can match the spectra of T dwarf atmospheres; water ice clouds will alter the spectra of the newest and coldest brown dwarfs, the Y dwarfs. These sulfide/salt and ice clouds potentially drive spectroscopic variability in these cool objects, and this variability should be distinguishable from variability caused by hot spots. Next, I present results for small, cool exoplanets between the size of Earth and Neptune. They likely have sulfide and salt clouds and also have photochemical hazes caused by stellar irradiation. Vast resources have been dedicated to characterizing the handful of super Earths and Neptunes accessible to current telescopes, yet of the planets smaller than Neptune studied to date, all have radii in the near-infrared consistent with being constant in wavelength, likely showing that these small planets are consistently enshrouded in thick hazes and clouds. For the super Earth GJ 1214b, very thick, lofted clouds of salts or sulfides in high metallicity (1000x solar) atmospheres create featureless transmission spectra in the near-infrared. Photochemical hazes also create featureless transmission spectra at lower metallicities. For the Neptune-sized GJ 436b, its thermal emission and transmission spectra combine indicate a high metallicity atmosphere, potentially heated by tides and affected by

  5. Voyager at Neptune: 1989

    NASA Technical Reports Server (NTRS)

    1989-01-01

    The Voyager mission has taken advantage of a rare planetary alignment that occurs at intervals of about 175 years and affords an extraordinary opportunity: a grand tour by a single spacecraft of the outer planets Jupiter, Saturn, Uranus, and Neptune. Voyager 2 will fly past Nepture and its large moon Triton on August 24, 1989. The discovery of Neptune, along with its current history is discussed. The imaging challenges, tracking and data acquisition, and the Voyager spacecraft are explained. Data will be gathered on the ring arcs of Neptune, the atmosphere and surface of Neptune, Triton, and Nereid (the smaller moon).

  6. Helium-Shrouded Planets Artist Concept

    NASA Image and Video Library

    2015-06-11

    Planets having atmospheres rich in helium may be common in our galaxy, according to a new theory based on data from NASA's Spitzer Space Telescope. These planets would be around the mass of Neptune, or lighter, and would orbit close to their stars, basking in their searing heat. According to the new theory, radiation from the stars would boil off hydrogen in the planets' atmospheres. Both hydrogen and helium are common ingredients of gas planets like these. Hydrogen is lighter than helium and thus more likely to escape. After billions of years of losing hydrogen, the planet's atmosphere would become enriched with helium. Scientists predict the planets would appear covered in white or gray clouds. This is in contrast to our own Neptune, which is blue due to the presence of methane. Methane absorbs the color red, leaving blue. Neptune is far from our sun and hasn't lost its hydrogen. The hydrogen bonds with carbon to form methane. This artist's concept depicts a proposed helium-atmosphere planet called GJ 436b, which was found by Spitzer to lack in methane -- a first clue about its lack of hydrogen. The planet orbits every 2.6 days around its star, which is cooler than our sun and thus appears more yellow-orange in color. http://photojournal.jpl.nasa.gov/catalog/PIA19344

  7. From Hot Jupiters to Super-Earths: Characterizing the Atmospheres of Extrasolar Planets with the Spitzer Space Telescope

    NASA Astrophysics Data System (ADS)

    Knutson, Heather

    2009-05-01

    The Spitzer Space Telescope has been a remarkably successful platform for studies of exoplanet atmospheres, with notable results including the first detection of the light emitted by an extrasolar planet (Deming et al. 2005, Charbonneau et al. 2005), the first spectrum of an extrasolar planet (Richardson et al. 2007, Grillmair et al. 2007), and the first map of the flux distribution across the surface of an extrasolar planet (Knutson et al. 2007). These observations have allowed us to characterize the pressure-temperature profiles, chemistry, clouds, and circulation patterns of a select subset of the massive, close-in planets known as hot Jupiters, along with the hot Saturn HD 149026b and the cooler Neptune-mass planet GJ 436b. In my talk I will review the current status of Spitzer observations of transiting planets at the end of the cryogenic mission and look ahead to the observations planned for the two-year warm mission, which will begin this summer after the last of Spitzer's cryogen is exhausted.

  8. The mass of planet GJ 676A b from ground-based astrometry. A planetary system with two mature gas giants suitable for direct imaging

    NASA Astrophysics Data System (ADS)

    Sahlmann, J.; Lazorenko, P. F.; Ségransan, D.; Astudillo-Defru, N.; Bonfils, X.; Delfosse, X.; Forveille, T.; Hagelberg, J.; Lo Curto, G.; Pepe, F.; Queloz, D.; Udry, S.; Zimmerman, N. T.

    2016-11-01

    The star GJ 676A is an M0 dwarf hosting both gas-giant and super-Earth-type planets that were discovered with radial-velocity measurements. Using FORS2/VLT, we obtained position measurements of the star in the plane of the sky that tightly constrain its astrometric reflex motion caused by the super-Jupiter planet "b" in a 1052-day orbit. This allows us to determine the mass of this planet to be , which is 40% higher than the minimum mass inferred from the radial-velocity orbit. Using new HARPS radial-velocity measurements, we improve upon the orbital parameters of the inner low-mass planets "d" and "e" and we determine the orbital period of the outer giant planet "c" to be Pc = 7340 days under the assumption of a circular orbit. The preliminary minimum mass of planet "c" is Mcsini = 6.8 MJ with an upper limit of 39 MJ that we set using NACO/VLT high-contrast imaging. We also determine precise parallaxes and relative proper motions for both GJ 676A and its wide M3 companion GJ 676B. Although the system is probably quite mature, the masses and projected separations ( 0.̋1-0.̋4) of planets "b" and "c" make them promising targets for direct imaging with future instruments in space and on extremely large telescopes. In particular, we estimate that GJ 676A b and GJ 676A c are promising targets for directly detecting their reflected light with the WFIRST space mission. Our study demonstrates the synergy of radial-velocity and astrometric surveys that is necessary to identify the best targets for such a mission. Based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programmes 385.C-0416 (A,B), 086.C-0515(A), 089.C-0115(D,E), 072.C-0488(E), 180.C-0886(A), 183.C-0437(A), 085.C-0019(A), 091.C-0034(A), 095.C-0551(A), 096.C-0460(A).Full Table A.2 is only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (http://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/595/A77

  9. 42 CFR 455.436 - Federal database checks.

    Code of Federal Regulations, 2012 CFR

    2012-10-01

    ... 42 Public Health 4 2012-10-01 2012-10-01 false Federal database checks. 455.436 Section 455.436....436 Federal database checks. The State Medicaid agency must do all of the following: (a) Confirm the... databases. (b) Check the Social Security Administration's Death Master File, the National Plan and Provider...

  10. 42 CFR 455.436 - Federal database checks.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... 42 Public Health 4 2011-10-01 2011-10-01 false Federal database checks. 455.436 Section 455.436....436 Federal database checks. The State Medicaid agency must do all of the following: (a) Confirm the... databases. (b) Check the Social Security Administration's Death Master File, the National Plan and Provider...

  11. 42 CFR 455.436 - Federal database checks.

    Code of Federal Regulations, 2014 CFR

    2014-10-01

    ... 42 Public Health 4 2014-10-01 2014-10-01 false Federal database checks. 455.436 Section 455.436....436 Federal database checks. The State Medicaid agency must do all of the following: (a) Confirm the... databases. (b) Check the Social Security Administration's Death Master File, the National Plan and Provider...

  12. 42 CFR 455.436 - Federal database checks.

    Code of Federal Regulations, 2013 CFR

    2013-10-01

    ... 42 Public Health 4 2013-10-01 2013-10-01 false Federal database checks. 455.436 Section 455.436....436 Federal database checks. The State Medicaid agency must do all of the following: (a) Confirm the... databases. (b) Check the Social Security Administration's Death Master File, the National Plan and Provider...

  13. Triboelectrification of KCl and ZnS particles with applications to GJ1214b

    NASA Astrophysics Data System (ADS)

    Mendez, Joshua; Dufek, Josef

    2017-10-01

    When mobilized, granular materials become charged as individual grains undergo collisions and frictional interactions. On Earth, this process, known as triboelectrification, has been recognized in volcanic plumes and sandstorms (Kok & Lacks 2009 )(Cimarelli et al. 2014 ) (Méndez Harper & Dufek 2016 ). Yet, frictional charging almost certainly exists on other worlds in our own Solar System (such as Mars, the Moon, and Venus) as well as extra solar planets. Indeed, recent observations and numerical modeling have suggested that many exoplanets may have processes that lift large quantities of particles into their atmospheres (volcanic activity, for instance) (Hodosán et al. 2016 ) or maintain extensive condensed granular reservoirs in the form of clouds or hazes (Helling et al. 2013 )(Kreidberg et al. 2014 ) (Gao & Benneke 2016 ). On these worlds, triboelectric charging almost certainly contributes to their global electric circuits, providing a mechanism to generate lightning, to drive chemical processes in the atmospheres, and, perhaps, influence habitability. Yet, despite the high likelihood of granular electrification processes occurring on worlds beyond our Solar System, no experiments, to our knowledge, have been conducted to characterize the triboelectrification of materials expected to exist in the exoplanet atmospheres under appropriate conditions. To help close this knowledge-gap, we explore the electrification of potassium chloride and zinc sulfide, two substances possibly composing the clouds on super-Earth GJ1214b (Kreidberg et al. 2014 ) (Charnay et al. 2015 ) (Gao & Benneke 2016 ). We find that both materials become readily electrified when mobilized, attaining charge densities similar to those found on volcanic ash particles. Thus, if GJ1214b does indeed host salt clouds in its atmosphere, they are likely electrified and may be capable of producing lightning or corona discharge.

  14. 42 CFR 436.530 - Definition of blindness.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... 42 Public Health 4 2010-10-01 2010-10-01 false Definition of blindness. 436.530 Section 436.530... Requirements for Medicaid Eligibility Blindness § 436.530 Definition of blindness. (a) Definition. The agency must use the definition of blindness that is used in the State plan for AB or AABD. (b) State plan...

  15. 42 CFR 436.600 - Scope.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... 42 Public Health 4 2011-10-01 2011-10-01 false Scope. 436.600 Section 436.600 Public Health CENTERS FOR MEDICARE & MEDICAID SERVICES, DEPARTMENT OF HEALTH AND HUMAN SERVICES (CONTINUED) MEDICAL... specified in subparts B, C, and D of this part. Subparts H and I of this part prescribe additional financial...

  16. 42 CFR 436.600 - Scope.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... 42 Public Health 4 2010-10-01 2010-10-01 false Scope. 436.600 Section 436.600 Public Health CENTERS FOR MEDICARE & MEDICAID SERVICES, DEPARTMENT OF HEALTH AND HUMAN SERVICES (CONTINUED) MEDICAL... specified in subparts B, C, and D of this part. Subparts H and I of this part prescribe additional financial...

  17. First Atmosphere Characterization of the Benchmark Exo-Neptune WASP-107b

    NASA Astrophysics Data System (ADS)

    Kreidberg, Laura

    2016-10-01

    WASP-107b is a newly announced transiting planet that is the highest signal-to-noise target for transmission spectroscopy discovered in the last decade, thanks to its low surface gravity and small, bright host star. The planet is in the intriguing transition region between ice and gas giants, with a mass comparable to Neptune and a radius similar to Jupiter. Relative to other benchmark systems, WASP-107b has a cool equilibrium temperature (780 K), where methane and water are both expected to be abundant. The planet therefore provides a unique opportunity for spectroscopic characterization of carbon and oxygen chemistry. With its large expected signal, WASP-107b also provides an excellent laboratory to study aerosol formation. The features are so large that even if thick clouds/haze are present at very high altitudes (0.1 mbar), it will still be possible to detect absorption features peeking out above them. Here we propose a reconnaissance observation of a single transit of WASP-107b. This measurement will vet the planet's atmosphere composition and test for the presence of aerosols so that the community can decide on the best follow-up strategy for this exciting system.

  18. The Formation of Mini-Neptunes

    NASA Astrophysics Data System (ADS)

    Venturini, Julia; Helled, Ravit

    2017-10-01

    Mini-Neptunes seem to be common planets. In this work we investigate the possible formation histories and predicted occurrence rates of mini-Neptunes, assuming that the planets form beyond the iceline. We consider pebble and planetesimal accretion accounting for envelope enrichment and two different opacity conditions. We find that the formation of mini-Neptunes is a relatively frequent output when envelope enrichment by volatiles is included, and that there is a “sweet spot” for mini-Neptune formation with a relatively low solid accretion rate of ˜10-6 M ⊕ yr-1. This rate is typical for low/intermediate-mass protoplanetary disks and/or disks with low metallicities. With pebble accretion, envelope enrichment and high opacity favor the formation of mini-Neptunes, with more efficient formation at large semimajor axes (˜30 au) and low disk viscosities. For planetesimal accretion, such planets can also form without enrichment, with the opacity being a key aspect in the growth history and favorable formation location. Finally, we show that the formation of Neptune-like planets remains a challenge for planet formation theories.

  19. Neptune in Primary Colors

    NASA Image and Video Library

    1998-08-02

    These two NASA Hubble Space Telescope images provide views of weather on opposite hemispheres of Neptune. Taken Aug. 13, 1996; these composite images blend information from different wavelengths to bring out features of Neptune blustery weather.

  20. Neptune Polar Orbiter with Probes

    NASA Technical Reports Server (NTRS)

    Bienstock, Bernard; Atkinson, David; Baines, Kevin; Mahaffy, Paul; Steffes, Paul; Atreya, Sushil; Stern, Alan; Wright, Michael; Willenberg, Harvey; Smith, David; hide

    2005-01-01

    The giant planets of the outer solar system divide into two distinct classes: the gas giants Jupiter and Saturn, which consist mainly of hydrogen and helium; and the ice giants Uranus and Neptune, which are believed to contain significant amounts of the heavier elements oxygen, nitrogen, and carbon and sulfur. Detailed comparisons of the internal structures and compositions of the gas giants with those of the ice giants will yield valuable insights into the processes that formed the solar system and, perhaps, other planetary systems. By 2012, Galileo, Cassini and possibly a Jupiter Orbiter mission with microwave radiometers, Juno, in the New Frontiers program, will have yielded significant information on the chemical and physical properties of Jupiter and Saturn. A Neptune Orbiter with Probes (NOP) mission would deliver the corresponding key data for an ice giant planet. Such a mission would ideally study the deep Neptune atmosphere to pressures approaching and possibly exceeding 1000 bars, as well as the rings, Triton, Nereid, and Neptune s other icy satellites. A potential source of power would be nuclear electric propulsion (NEP). Such an ambitious mission requires that a number of technical issues be investigated, however, including: (1) atmospheric entry probe thermal protection system (TPS) design, (2) probe structural design including seals, windows, penetrations and pressure vessel, (3) digital, RF subsystem, and overall communication link design for long term operation in the very extreme environment of Neptune's deep atmosphere, (4) trajectory design allowing probe release on a trajectory to impact Neptune while allowing the spacecraft to achieve a polar orbit of Neptune, (5) and finally the suite of science instruments enabled by the probe technology to explore the depths of the Neptune atmosphere. Another driving factor in the design of the Orbiter and Probes is the necessity to maintain a fully operational flight system during the lengthy transit time

  1. Hubble View of Neptune

    NASA Image and Video Library

    1998-08-02

    These NASA Hubble Space Telescope views of the blue-green planet Neptune provide three snapshots of changing weather conditions. The images were taken in 1994 on 3 separate days when Neptune was 2.8 billion miles 4.5 billion kilometers from Earth.

  2. The Voyager encounter with Neptune

    NASA Technical Reports Server (NTRS)

    Stone, E. C.; Miner, E. D.

    1991-01-01

    The investigations carried out by the Voyager Neptune/Interstellar Mission are discussed. Attention is given to the location of the various science instruments and the spacecraft subsystems on the Voyager spacecraft and to the charactgeristics of eleven instruments used in the Voyager mission. The Voyager 1 and 2 trajectories from the launch through the Voyager-2 Neptune encounter are presented together with data for the Neptune encounter events.

  3. Recent Transits of the Super-Earth Exoplanet GJ 1214B

    NASA Technical Reports Server (NTRS)

    Sada, Pedro V.; Deming, Drake; Jackson, Brian; Jennings, Donald E.; Peterson, Steven W.; Haase, Flynn; Bays, Kevin; OGorman, Eamon; Lundsford, Alan

    2001-01-01

    We report recent ground-based photometry of the transiting super-Earth exoplanet GJ1214b at several wavelengths, including the infrared near 1.25 microns (J-band). We observed a J-band transit with the FLAMINGOS infrared imager and the 2.1-meter telescope on Kitt Peak, and we observed several optical transits using a 0.5-meter telescope on Kitt Peak and the 0.36-meter Universidad de Monterrey Observatory telescope. Our high-precision J-band observations exploit the brightness of the M-dwarf host star at this infrared wavelength as compared to the optical, as well as being significantly less affected by stellar activity and limb darkening. We fit the J-band transit to obtain an independent determination of the planetary and stellar radii. Our radius for the planet (2.61 +0.30 / -0.11 Earth radii) is in excellent agreement with the discovery value reported by Charbonneau et al. based on optical data. We demonstrate that the planetary radius is insensitive to degeneracies in the fitting process. We use all of our observations to improve the transit ephemeris, finding P=1.5804043 +/- 0.0000005 days, and T0=2454964.94390 +/- 0.00006 BJD.

  4. Recent Transits of the Super-Earth Exoplanet GJ 1214b

    NASA Astrophysics Data System (ADS)

    Sada, Pedro V.; Deming, Drake; Jackson, Brian; Jennings, Donald E.; Peterson, Steven W.; Haase, Flynn; Bays, Kevin; O'Gorman, Eamon; Lundsford, Alan

    2010-09-01

    We report recent ground-based photometry of the transiting super-Earth exoplanet GJ 1214b at several wavelengths, including the infrared near 1.25 μm (J band). We observed a J-band transit with the FLAMINGOS infrared imager and the 2.1 m telescope on Kitt Peak, and we observed several optical transits using a 0.5 m telescope on Kitt Peak and the 0.36 m Universidad de Monterrey Observatory telescope. Our high-precision J-band observations exploit the brightness of the M dwarf host star at this infrared wavelength as compared with the optical and are significantly less affected by stellar activity and limb darkening. We fit the J-band transit to obtain an independent determination of the planetary and stellar radii. Our radius for the planet (2.61+0.30 -0.11 R ⊕) is in excellent agreement with the discovery value reported by Charbonneau et al. based on optical data. We demonstrate that the planetary radius is insensitive to degeneracies in the fitting process. We use all of our observations to improve the transit ephemeris, finding P = 1.5804043 ± 0.0000005 days and T 0 = 2454964.94390 ± 0.00006 BJD.

  5. Spectroscopic Characterization of a Newborn Neptune-Sized Planet

    NASA Astrophysics Data System (ADS)

    Benneke, Bjoern

    2016-10-01

    The study of planet formation as it occurs has remained an elusive frontier, until now. Our team recently identified a newly-born planet orbiting a young, 5-10 Myr old, pre-main-sequence M star in the Upper Scorpius star-forming region. In its early stage, the close-in planet is about 50% larger than Neptune. Models predict that it will contract over the coming 100-1000 Myr to become a member of the intriguingly abundant class of close-in sub-Neptunes. Spectroscopic observations of this newborn planet will give us the unprecedented opportunity to probe the formation and evolution of low-mass, close-in planets at this early stage. Here, we propose to a reconnaissance study to probe the adolescent state of the gravitationally-bound atmosphere using near-infrared transit spectroscopy and the planet's hydrogen loss rate using far-UV transit spectroscopy. Together, our observations will give us unparalleled insights into the initial state of a young close-in planet as well as into the competing timescales of Kelvin-Helmholtz contraction and envelope mass-loss involved in the early evolution of close-in sub-Neptunes and Neptunes. If the proposed reconnaissance observations detect that molecular absorption in the atmosphere of USco 1610-1919b, then USco 1610-1919b will be one of the prime targets for the 200-hour JWST/NIRISS GTO program to probe the formation and evolution of exoplanets. Mid-cycle observations are required because the final target list for JWST/GTO programs must be locked in by June 2017 before the beginning of HST Cycle 25.

  6. Neptune

    NASA Image and Video Library

    1999-10-14

    This photograph of Neptune shows three of the features that NASA Voyager 2 has been photographing during recent weeks. At the north is the Great Dark Spot, accompanied by bright, white clouds that undergo rapid changes in appearance.

  7. Magnetic fields at neptune.

    PubMed

    Ness, N F; Acuña, M H; Burlaga, L F; Connerney, J E; Lepping, R P; Neubauer, F M

    1989-12-15

    The National Aeronautics and Space Administration Goddard Space Flight Center-University of Delaware Bartol Research Institute magnetic field experiment on the Voyager 2 spacecraft discovered a strong and complex intrinsic magnetic field of Neptune and an associated magnetosphere and magnetic tail. The detached bow shock wave in the supersonic solar wind flow was detected upstream at 34.9 Neptune radii (R(N)), and the magnetopause boundary was tentatively identified at 26.5 R(N) near the planet-sun line (1 R(N) = 24,765 kilometers). A maximum magnetic field of nearly 10,000 nanoteslas (1 nanotesla = 10(-5) gauss) was observed near closest approach, at a distance of 1.18 R(N). The planetary magnetic field between 4 and 15 R(N) can be well represented by an offset tilted magnetic dipole (OTD), displaced from the center of Neptune by the surprisingly large amount of 0.55 R(N) and inclined by 47 degrees with respect to the rotation axis. The OTD dipole moment is 0.133 gauss-R(N)(3). Within 4 R(N), the magnetic field representation must include localized sources or higher order magnetic multipoles, or both, which are not yet well determined. The obliquity of Neptune and the phase of its rotation at encounter combined serendipitously so that the spacecraft entered the magnetosphere at a time when the polar cusp region was directed almost precisely sunward. As the spacecraft exited the magnetosphere, the magnetic tail appeared to be monopolar, and no crossings of an imbedded magnetic field reversal or plasma neutral sheet were observed. The auroral zones are most likely located far from the rotation poles and may have a complicated geometry. The rings and all the known moons of Neptune are imbedded deep inside the magnetosphere, except for Nereid, which is outside when sunward of the planet. The radiation belts will have a complex structure owing to the absorption of energetic particles by the moons and rings of Neptune and losses associated with the significant changes

  8. RECENT TRANSITS OF THE SUPER-EARTH EXOPLANET GJ 1214b

    DOE Office of Scientific and Technical Information (OSTI.GOV)

    Sada, Pedro V.; Deming, Drake; Jackson, Brian

    We report recent ground-based photometry of the transiting super-Earth exoplanet GJ 1214b at several wavelengths, including the infrared near 1.25 {mu}m (J band). We observed a J-band transit with the FLAMINGOS infrared imager and the 2.1 m telescope on Kitt Peak, and we observed several optical transits using a 0.5 m telescope on Kitt Peak and the 0.36 m Universidad de Monterrey Observatory telescope. Our high-precision J-band observations exploit the brightness of the M dwarf host star at this infrared wavelength as compared with the optical and are significantly less affected by stellar activity and limb darkening. We fit themore » J-band transit to obtain an independent determination of the planetary and stellar radii. Our radius for the planet (2.61{sup +0.30} {sub -0.11} R {sub +}) is in excellent agreement with the discovery value reported by Charbonneau et al. based on optical data. We demonstrate that the planetary radius is insensitive to degeneracies in the fitting process. We use all of our observations to improve the transit ephemeris, finding P = 1.5804043 {+-} 0.0000005 days and T {sub 0} = 2454964.94390 {+-} 0.00006 BJD.« less

  9. Voyager 2 Neptune targeting strategy

    NASA Technical Reports Server (NTRS)

    Potts, C. L.; Francis, K.; Matousek, S. E.; Cesarone, R. J.; Gray, D. L.

    1989-01-01

    The success of the Voyager 2 flybys of Neptune and Triton depends upon the ability to correct the spacecraft's trajectory. Accurate spacecraft delivery to the desired encounter conditions will promote the maximum science return. However, Neptune's great distance causes large a priori uncertainties in Neptune and Triton ephemerides and planetary system parameters. Consequently, the 'ideal' trajectory is unknown beforehand. The targeting challenge is to utilize the gradually improving knowledge as the spacecraft approaches Neptune to meet the science objectives, but with an overriding concern for spacecraft safety and a desire to limit propellant expenditure. A unique targeting strategy has been developed in response to this challenge. Through the use of a Monte Carlo simulation, candidate strategies are evaluated by the degree to which they meet these objectives and are compared against each other in determining the targeting strategy to be adopted.

  10. Uranus and Neptune

    NASA Technical Reports Server (NTRS)

    Bergstralh, J. T. (Editor)

    1984-01-01

    A scientific framework within which to plan the Voyager encounters with Uranus and Neptune was sought. Specific objectives were: (1) to assess the current state of knowledge of Uranus and Neptune, their magnetospheres, and their respective systems of satellites and rings (if any), (2) to identify important scientific issues that can be addressed effectively by Voyager, and (3) to provide an opportunity for Voyager investigators to interact with other scientists knowledgeable in the field of physical studies of the Uranian and Neptunian systems.

  11. 1981N1 - A Neptune arc?

    NASA Technical Reports Server (NTRS)

    Hubbard, W. B.

    1986-01-01

    An object in the vicinity of Neptune detected in 1981 by simultaneous stellar occultation measurements at observatories near Tucson, Arizona, was interpreted as a new Neptune satellite. A reinterpretation suggests that it may have instead been a Neptune arc similar to one observed in 1984. The 1981 object, however, did not occult the star during simultaneous observations at Flagstaff, Arizona. This result constrains possible arc geometries.

  12. No hydrogen exosphere detected around the super-Earth HD 97658 b

    NASA Astrophysics Data System (ADS)

    Bourrier, V.; Ehrenreich, D.; King, G.; Lecavelier des Etangs, A.; Wheatley, P. J.; Vidal-Madjar, A.; Pepe, F.; Udry, S.

    2017-01-01

    The exoplanet HD 97658 b provides a rare opportunity to probe the atmospheric composition and evolution of moderately irradiated super-Earths. It transits a bright K star at a moderate orbital distance of 0.08 au. Its low density is compatible with a massive steam envelope that could photodissociate at high altitudes and become observable as escaping neutral hydrogen. Our analysis of three transits with HST/STIS at Lyman-α reveals no such signature, suggesting that the thermosphere of HD 97658 b is not hydrodynamically expanding and is subjected to a low escape of neutral hydrogen (<108 g s-1 at 3σ). Using HST/STIS Lyman-α observations and Chandra/ACIS-S and XMM-Newton/EPIC X-ray observations at different epochs, we find that HD 97658 is in fact a weak and soft X-ray source with signs of chromospheric variability in the Lyman-α line core. We determine an average reference for the intrinsic Lyman-α line and X-EUV (XUV) spectrum of the star, and show that HD 97658 b is in mild conditions of irradiation compared to other known evaporating exoplanets with an XUV irradiation about three times lower than the evaporating warm Neptune GJ436 b. This could be the reason why the thermosphere of HD 97658 b is not expanding: the low XUV irradiation prevents an efficient photodissociation of any putative steam envelope. Alternatively, it could be linked to a low hydrogen content or inefficient conversion of the stellar energy input. The HD 97658 system provides clues for understanding the stability of low-mass planet atmospheres in terms of composition, planetary density, and irradiation. Our study of HD 97658 b can be seen as a control experiment of our methodology, confirming that it does not bias detections of atmospheric escape and underlining its strength and reliability. Our results show that stellar activity can be efficiently discriminated from absorption signatures by a transiting exospheric cloud. They also highlight the potential of observing the upper atmosphere

  13. Neptune Through a Clear Filter

    NASA Image and Video Library

    1999-07-25

    On July 23, 1989, NASA Voyager 2 spacecraft took this picture of Neptune through a clear filter on its narrow-angle camera. The image on the right has a latitude and longitude grid added for reference. Neptune Great Dark Spot is visible on the left.

  14. High-Contrast 3.8 Micron Imaging of the Brown Dwarf/Planet-Mass Companion to GJ 758

    NASA Technical Reports Server (NTRS)

    Currie, Thayne M.; Bailey, Vanessa; Fabrycky, Daniel; Murray-Clay, Ruth; Rodigas, Timothy; Hinz, Phil

    2011-01-01

    We present L' band (3.8 Micron) MMT/Clio high-contrast imaging data for the nearby star GJ 758, which was recently reported by Thalmann et al. (2009) to have one - possibly two - faint comoving companions (GJ 7588 and "C", respectively). GJ 758B is detected in two distinct datasets. Additionally, we report a \\textit{possible} detection of the object identified by Thalmann et al as "GJ 758C" in our more sensitive dataset, though it is likely a residual speckle. However, if it is the same object as that reported by Thalmann et al. it cannot be a companion in a bound orbit. GJ 7588 has a H-L' color redder than nearly all known L-T8 dwarfs. 8ased on comparisons with the COND evolutionary models, GJ 7588 has Te approx. 560 K (+150 K, -90 K) and a mass ranging from approx.10-20 Mj if it is approx.1 Gyr old to approx. 25-40 Mj if it is 8.7 Gyr old. GJ 7588 is likely in a highly eccentric orbit, e approx. 0.73 (+0.12,-0.21), with a semimajor axis of approx. 44 AU (+32 AU, -14 AU). Though GJ 7588 is sometimes discussed within the context of exoplanet direct imaging, its mass is likely greater than the deuterium-burning limit and its formation may resemble that of binary stars rather than that of jovian-mass planets.

  15. Did Triton Destroy Neptune's First Moons?

    NASA Astrophysics Data System (ADS)

    Kohler, Susanna

    2017-11-01

    Neptunes moon system is not what we would expect for a gas giant in our solar system. Scientists have now explored the possibility that Neptune started its life with an ordinary system of moons that was later destroyed by the capture of its current giant moon, Triton.An Odd SystemOur current understanding of giant-planet formation predicts a period of gas accretion to build up the large size of these planets. According to models, the circumplanetary gas disks that surround the planets during this time then become the birthplaces of the giant planets satellite systems, producing systems of co-planar and prograde (i.e., orbiting in the same direction as the planets rotation) satellites similar to the many-moon systems of Jupiter or Saturn.Tritons orbit is tilted relative to the inner Neptunian satellite orbits. [NASA, ESA, and A. Feild (STScI)]Neptune, however, is quirky. This gas giant has surprisingly few satellites only 14 compared to, say, the nearly 70 moons of Jupiter and most of them are extremely small. One of Neptunes moons is an exception to this, however: Triton, which contains 99.7% of the mass of Neptunes entire satellite system!Tritons orbit has a number of unusual properties. The orbit is retrograde Triton orbits in the opposite direction as Neptunes rotation which is unique behavior among large moons in our solar system. Tritons orbit is also highly inclined, and yet the moons path is nearly circular and lies very close to Neptune.The distribution of impact velocities in the authors simulations for primordial satellite interactions with Triton, in three cases of different satellite mass ratios. In the low-mass case a third of the mass ratio of the Uranian satellite system 88% of simulations ended with Triton surviving on its high-inclination orbit. The survival rate was only 12% in the high-mass case. [Adapted from Rufu et al. 2017]How did this monster of a satellite get its strange properties, and why is Neptunes system so odd compared to what we

  16. Neptune

    NASA Image and Video Library

    1999-07-25

    This image of Neptune was taken through the clear filter of the narrow-angle camera on July 16, 1989 by NASA Voyager 2 spacecraft. The image was processed by computer to show the newly resolved dark oval feature embedded in the middle of the dusky south

  17. Neptune Aerocapture Systems Analysis

    NASA Technical Reports Server (NTRS)

    Lockwood, Mary Kae

    2004-01-01

    A Neptune Aerocapture Systems Analysis is completed to determine the feasibility, benefit and risk of an aeroshell aerocapture system for Neptune and to identify technology gaps and technology performance goals. The high fidelity systems analysis is completed by a five center NASA team and includes the following disciplines and analyses: science; mission design; aeroshell configuration screening and definition; interplanetary navigation analyses; atmosphere modeling; computational fluid dynamics for aerodynamic performance and database definition; initial stability analyses; guidance development; atmospheric flight simulation; computational fluid dynamics and radiation analyses for aeroheating environment definition; thermal protection system design, concepts and sizing; mass properties; structures; spacecraft design and packaging; and mass sensitivities. Results show that aerocapture can deliver 1.4 times more mass to Neptune orbit than an all-propulsive system for the same launch vehicle. In addition aerocapture results in a 3-4 year reduction in trip time compared to all-propulsive systems. Aerocapture is feasible and performance is adequate for the Neptune aerocapture mission. Monte Carlo simulation results show 100% successful capture for all cases including conservative assumptions on atmosphere and navigation. Enabling technologies for this mission include TPS manufacturing; and aerothermodynamic methods and validation for determining coupled 3-D convection, radiation and ablation aeroheating rates and loads, and the effects on surface recession.

  18. Neptune's Eccentricity and the Nature of the Kuiper Belt

    NASA Technical Reports Server (NTRS)

    Ward, William R.; Hahn, Joseph M.

    1998-01-01

    The small eccentricity of Neptune may be a direct consequence of apsidal wave interaction with the trans-Neptune population of debris called the Kuiper belt. The Kuiper belt is subject to resonant perturbations from Neptune, so that the transport of angular momentum by density waves can result in orbital evolution of Neptune as well as changes in the structure of the Kuiper belt. In particular, for a belt eroded out to the vicinity of Neptune's 2:1 resonance at about 48 astronomical units, Neptune's eccentricity can damp to its current value over the age of the solar system if the belt contains slightly more than an earth mass of material out to about 75 astronomical units.

  19. Neptune aerocapture mission and spacecraft design overview

    NASA Technical Reports Server (NTRS)

    Bailey, Robert W.; Hall, Jeff L.; Spliker, Tom R.; O'Kongo, Nora

    2004-01-01

    A detailed Neptune aerocapture systems analysis and spacecraft design study was performed as part of NASA's In-Space Propulsion Program. The primary objectives were to assess the feasibility of a spacecraft point design for a Neptune/Triton science mission. That uses aerocapture as the Neptune orbit insertion mechanism. This paper provides an overview of the science, mission and spacecraft design resulting from that study.

  20. 30 CFR 43.6 - Notice of negative finding.

    Code of Federal Regulations, 2010 CFR

    2010-07-01

    ... 30 Mineral Resources 1 2010-07-01 2010-07-01 false Notice of negative finding. 43.6 Section 43.6... Notice of negative finding. (a) If it is determined that a special inspection is not warranted, a written notice of negative finding shall be issued as soon as possible following such determination. (b) If it is...

  1. HAT-P-26b: A Neptune-mass exoplanet with a well-constrained heavy element abundance.

    PubMed

    Wakeford, Hannah R; Sing, David K; Kataria, Tiffany; Deming, Drake; Nikolov, Nikolay; Lopez, Eric D; Tremblin, Pascal; Amundsen, David S; Lewis, Nikole K; Mandell, Avi M; Fortney, Jonathan J; Knutson, Heather; Benneke, Björn; Evans, Thomas M

    2017-05-12

    A correlation between giant-planet mass and atmospheric heavy elemental abundance was first noted in the past century from observations of planets in our own Solar System and has served as a cornerstone of planet-formation theory. Using data from the Hubble and Spitzer Space Telescopes from 0.5 to 5 micrometers, we conducted a detailed atmospheric study of the transiting Neptune-mass exoplanet HAT-P-26b. We detected prominent H 2 O absorption bands with a maximum base-to-peak amplitude of 525 parts per million in the transmission spectrum. Using the water abundance as a proxy for metallicity, we measured HAT-P-26b's atmospheric heavy element content ([Formula: see text] times solar). This likely indicates that HAT-P-26b's atmosphere is primordial and obtained its gaseous envelope late in its disk lifetime, with little contamination from metal-rich planetesimals. Copyright © 2017, American Association for the Advancement of Science.

  2. The First Neptune Analog or Super-Earth with a Neptune-Like Orbit: MOA-2013-BLG-605Lb

    NASA Technical Reports Server (NTRS)

    Sumi, T.; Bennett, D. P.; Udalski, A.; Gould, A.; Poleski, R.; Bond, I. A.; Skowron, J.; Rattenbury, N.; Pogge, R. W.; Bensby, T.

    2016-01-01

    We present the discovery of the first Neptune analog exoplanet or super-Earth with a Neptune-like orbit, MOA- 2013-BLG-605Lb. This planet has a mass similar to that of Neptune or a super-Earth and it orbits at 9 approximately 14 times the expected position of the snow line, a(sub snow), which is similar to Neptune's separation of 11 a(sub snow) from the Sun. The planet/host-star mass ratio is q = (3.6 +/- 0.7) × 10(exp -4) and the projected separation normalized by the Einstein radius is s = 2.39 +/- 0.05. There are three degenerate physical solutions and two of these are due to a new type of degeneracy in the microlensing parallax parameters, which we designate "the wide degeneracy." The three models have (i) a Neptune-mass planet with a mass of M(sub p) = 21(+6/-7)(M) orbiting a low-mass M-dwarf with a mass of M(sub h) = 0.19(+0.05/-0.06 (solar mass)), (ii) a mini-Neptune with M(sub p) = 7.9(+1.8/-1.5)(M)) orbiting a brown dwarf host with M(sub h) = 0.068(+0.019/-0.011(solar mass)), and (iii) a super-Earth with M(sub p) = 3.2(+0.5/-0.3(M)) orbiting a low-mass brown dwarf host with M(sub h) = 0.025(+0.005/-0.004)(solar mass)), which is slightly favored. The 3D planet-host separations are 4.6(+4.7/-1.2)au, 2.1(+1.0/-0.2)au, and 0.94(+0.67/-0.02)au, which are 8.9(+10.5/-1.4)m 12(+7/-1), or 14(+11/-1) times larger than a(sub snow) for these models, respectively. Keck adaptive optics observations confirm that the lens is faint. This discovery suggests that low-mass planets with Neptune-like orbits are common. Therefore processes similar to the one that formed Neptune in our own solar system or cold super-Earths may be common in other solar systems.

  3. Neptune and Triton: A Study in Future Exploration

    NASA Astrophysics Data System (ADS)

    Day, M. D.; Malaska, M. J.; Hosseini, S.; Mcgranaghan, R.; Fernandes, P. A.; Fougere, N.; Clegg, R. N.; Scully, J.; Alibay, F.; Ries, P.; Craig, P. L.; Hutchins, M. L.; Leonard, J.; Uckert, K.; Patthoff, A.; Girazian, Z.

    2013-12-01

    Neptune provides a unique natural laboratory for studying the dynamics of ice giants. Last visited by Voyager 2 in 1989, Neptune and its moon Triton hold important clues to the evolution of the solar system. The Voyager 2 flyby revealed Neptune to be a dynamic world with large storms, unparalleled wind speeds, and an unusual magnetic field. Triton, Neptune's largest satellite, is believed to be a captured Kuiper Belt Object with a thin atmosphere and possible sub-surface ocean. Further study of the farthest planet in our solar system could offer new insights into the dynamics of ice-giant exoplanets, and help us understand their complex atmospheres. The diverse science questions associated with Neptune and Triton motivate the complex and exciting mission proposed in this study. The proposed mission follows the guidelines of the 2013-2022 Planetary Science Decadal Survey, and optimizes the number of high priority science goals achieved, while still maintaining low mission costs. High priority science goals include understanding the structure, composition, and dynamics of Neptune's atmosphere and magnetosphere, as well as analyzing the surface of Triton. With a budget of $1.5 billion, the mission hosts an atmospheric probe and suite of instruments equipped with technologies significantly more advanced than those carried by Voyager 2. Additionally, the mission offers improved spatial coverage and higher resolution measurements than any previously achieved at Neptune. The proposed spacecraft would complete an orbital tour of Neptune and execute several close flybys of Triton. Further study of Neptune and Triton will provide exciting insights into what lies on the edge of our solar system and beyond. This study was prepared in conjunction with Jet Propulsion Laboratory's 2013 Planetary Science Summer School.

  4. The GTC exoplanet transit spectroscopy survey. V. A spectrally-resolved Rayleigh scattering slope in GJ 3470b

    NASA Astrophysics Data System (ADS)

    Chen, G.; Guenther, E. W.; Pallé, E.; Nortmann, L.; Nowak, G.; Kunz, S.; Parviainen, H.; Murgas, F.

    2017-04-01

    Aims: As a sub-Uranus-mass low-density planet, GJ 3470b has been found to show a flat featureless transmission spectrum in the infrared and a tentative Rayleigh scattering slope in the optical. We conducted an optical transmission spectroscopy project to assess the impacts of stellar activity and to determine whether or not GJ 3470b hosts a hydrogen-rich gas envelop. Methods: We observed three transits with the low-resolution Optical System for Imaging and low-Intermediate-Resolution Integrated Spectroscopy (OSIRIS) at the 10.4 m Gran Telescopio Canarias, and one transit with the high-resolution Ultraviolet and Visual Echelle Spectrograph (UVES) at the 8.2 m Very Large Telescope. Results: From the high-resolution data, we find that the difference of the Ca II H+K lines in- and out-of-transit is only 0.67 ± 0.22%, and determine a magnetic filling factor of about 10-15%. From the low-resolution data, we present the first optical transmission spectrum in the 435-755 nm band, which shows a slope consistent with Rayleigh scattering. Conclusions: After exploring the potential impacts of stellar activity in our observations, we confirm that Rayleigh scattering in an extended hydrogen-helium atmosphere is currently the best explanation. Further high-precision observations that simultaneously cover optical and infrared bands are required to answer whether or not clouds and hazes exist at high-altitude. Based on observations made with the Gran Telescopio Canarias (GTC), at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias, on the island of La Palma, as well as observations obtained at the European Southern Observatory at Paranal, Chile in program 096.C-0258(A).

  5. Aerocapture Guidance Performance for the Neptune Orbiter

    NASA Technical Reports Server (NTRS)

    Masciarelli, James P.; Westhelle, Carlos H.; Graves, Claude A.

    2004-01-01

    A performance evaluation of the Hybrid Predictor corrector Aerocapture Scheme (HYPAS) guidance algorithm for aerocapture at Neptune is presented in this paper for a Mission to Neptune and the Neptune moon Triton'. This mission has several challenges not experienced in previous aerocapture guidance assessments. These challengers are a very high Neptune arrival speed, atmospheric exit into a high energy orbit about Neptune, and a very high ballistic coefficient that results in a low altitude acceleration capability when combined with the aeroshell LD. The evaluation includes a definition of the entry corridor, a comparison to the theoretical optimum performance, and guidance responses to variations in atmospheric density, aerodynamic coefficients and flight path angle for various vehicle configurations (ballistic numbers). The benefits of utilizing angle-of-attack modulation in addition to bank angle modulation to improve flight performance is also discussed. The results show that despite large sensitivities in apoapsis targeting, the algorithm performs within the allocated AV budget for the Neptune mission bank angle only modulation. The addition of angle-of-attack modulation with as little as 5 degrees of amplitude significantly improves the scatter in final orbit apoapsis. Although the angle-of-attack modulation complicates the vehicle design, the performance enhancement reduces aerocapture risk and reduces the propellant consumption needed to reach the high energy target orbit for a conventional propulsion system.

  6. CONSTRAINTS ON PLANET OCCURRENCE AROUND NEARBY MID-TO-LATE M DWARFS FROM THE MEARTH PROJECT

    DOE Office of Scientific and Technical Information (OSTI.GOV)

    Berta, Zachory K.; Irwin, Jonathan; Charbonneau, David, E-mail: zberta@cfa.harvard.edu

    The MEarth Project is a ground-based photometric survey intended to find planets transiting the closest and smallest main-sequence stars. In its first four years, MEarth discovered one transiting exoplanet, the 2.7 R{sub ⊕} planet GJ1214b. Here, we answer an outstanding question: in light of the bounty of small planets transiting small stars uncovered by the Kepler mission, should MEarth have found more than just one planet so far? We estimate MEarth's ensemble sensitivity to exoplanets by performing end-to-end simulations of 1.25 × 10{sup 6} observations of 988 nearby mid-to-late M dwarfs, gathered by MEarth between 2008 October and 2012 June.more » For 2-4 R{sub ⊕} planets, we compare this sensitivity to results from Kepler and find that MEarth should have found planets at a rate of 0.05-0.36 planets yr{sup –1} in its first four years. As part of this analysis, we provide new analytic fits to the Kepler early M dwarf planet occurrence distribution. When extrapolating between Kepler's early M dwarfs and MEarth's mid-to-late M dwarfs, we find that assuming the planet occurrence distribution stays fixed with respect to planetary equilibrium temperature provides a good match to our detection of a planet with GJ1214b's observed properties. For larger planets, we find that the warm (600-700 K), Neptune-sized (4 R{sub ⊕}) exoplanets that transit early M dwarfs like Gl436 and GJ3470 occur at a rate of <0.15 star{sup –1} (at 95% confidence) around MEarth's later M dwarf targets. We describe a strategy with which MEarth can increase its expected planet yield by 2.5 × without new telescopes by shifting its sensitivity toward the smaller and cooler exoplanets that Kepler has demonstrated to be abundant.« less

  7. Dynamics of a Probable Earth-mass Planet in the GJ 832 System

    NASA Astrophysics Data System (ADS)

    Satyal, S.; Griffith, J.; Musielak, Z. E.

    2017-08-01

    The stability of planetary orbits around the GJ 832 star system, which contains inner (GJ 832c) and outer (GJ 832b) planets, is investigated numerically and a detailed phase-space analysis is performed. Special attention is given to the existence of stable orbits for a planet less than 15 M ⊕ that is injected between the inner and outer planets. Thus, numerical simulations are performed for three and four bodies in elliptical orbits (or circular for special cases) by using a large number of initial conditions that cover the selected phase-spaces of the planet’s orbital parameters. The results presented in the phase-space maps for GJ 832c indicate the least deviation of eccentricity from its nominal value, which is then used to determine its inclination regime relative to the star-outer planet plane. Also, the injected planet is found to display stable orbital configurations for at least one billion years. Then, the radial velocity curves based on the signature from the Keplerian motion are generated for the injected planets with masses 1 M ⊕ to 15 M ⊕ in order to estimate their semimajor axes and mass limits. The synthetic RV signal suggests that an additional planet of mass ≤15 M ⊕ with a dynamically stable configuration may be residing between 0.25 and 2.0 au from the star. We have provided an estimated number of RV observations for the additional planet that is required for further observational verification.

  8. The origin of carbon monoxide in Neptunes's atmosphere

    NASA Technical Reports Server (NTRS)

    Lodders, K.; Fegley, B., Jr.

    1994-01-01

    The CO abundance in the observable atmosphere of Neptune can be plausibly explained by rapid vertical mixing from the deeper atmosphere if Neptune has a greater complement of water than Uranus. Thermochemical equilibrium and kinetic calculations reveal that Neptune must and Uranus may have about 10 times more oxygen than carbon, whereas for Jupiter and Saturn equal enrichments of carbon and oxygen are satifactory to explain the observed CO abundances by deep vertical mixing. Relative to hydrogen and solar composition, the respective enrichment factors for carbon and oxygen are 41, 440 (Neptune); 32, less than or equal 260 (Uranus); 6.6, 6.6 (Saturn); and 2.8, 2.8 (Jupiter). Because water ice is the most refractory ice among the ices assumed to be present in the outer solar nebula, the most massive H2O enrichment is expected for the outermost planet of this group. Thus, Neptune can indeed be regarded as the 'god of the seas.'

  9. Surprisingly different star-spot distributions on the near equal-mass equal-rotation-rate stars in the M dwarf binary GJ 65 AB

    NASA Astrophysics Data System (ADS)

    Barnes, J. R.; Jeffers, S. V.; Haswell, C. A.; Jones, H. R. A.; Shulyak, D.; Pavlenko, Ya. V.; Jenkins, J. S.

    2017-10-01

    We aim to understand how stellar parameters such as mass and rotation impact the distribution of star-spots on the stellar surface. To this purpose, we have used Doppler imaging to reconstruct the surface brightness distributions of three fully convective M dwarfs with similar rotation rates. We secured high cadence spectral time series observations of the 5.5 au separation binary GJ 65, comprising GJ 65A (M5.5V, Prot = 0.24 d) and GJ 65B (M6V, Prot = 0.23 d). We also present new observations of GJ 791.2A (M4.5V, Prot = 0.31 d). Observations of each star were made on two nights with UVES, covering a wavelength range from 0.64 - 1.03μm. The time series spectra reveal multiple line distortions that we interpret as cool star-spots and which are persistent on both nights suggesting stability on the time-scale of 3 d. Spots are recovered with resolutions down to 8.3° at the equator. The global spot distributions for GJ 791.2A are similar to observations made a year earlier. Similar high latitude and circumpolar spot structure is seen on GJ 791.2A and GJ 65A. However, they are surprisingly absent on GJ 65B, which instead reveals more extensive, larger, spots concentrated at intermediate latitudes. All three stars show small amplitude latitude-dependent rotation that is consistent with solid body rotation. We compare our measurements of differential rotation with previous Doppler imaging studies and discuss the results in the wider context of other observational estimates and recent theoretical predictions.

  10. 10 CFR 436.42 - Evaluation of Life-Cycle Cost Effectiveness.

    Code of Federal Regulations, 2014 CFR

    2014-01-01

    ... 10 Energy 3 2014-01-01 2014-01-01 false Evaluation of Life-Cycle Cost Effectiveness. 436.42... PROGRAMS Agency Procurement of Energy Efficient Products § 436.42 Evaluation of Life-Cycle Cost...) ENERGY STAR qualified and FEMP designated products may be assumed to be life-cycle cost-effective. (b) In...

  11. 10 CFR 436.42 - Evaluation of Life-Cycle Cost Effectiveness.

    Code of Federal Regulations, 2012 CFR

    2012-01-01

    ... 10 Energy 3 2012-01-01 2012-01-01 false Evaluation of Life-Cycle Cost Effectiveness. 436.42... PROGRAMS Agency Procurement of Energy Efficient Products § 436.42 Evaluation of Life-Cycle Cost...) ENERGY STAR qualified and FEMP designated products may be assumed to be life-cycle cost-effective. (b) In...

  12. 10 CFR 436.42 - Evaluation of Life-Cycle Cost Effectiveness.

    Code of Federal Regulations, 2013 CFR

    2013-01-01

    ... 10 Energy 3 2013-01-01 2013-01-01 false Evaluation of Life-Cycle Cost Effectiveness. 436.42... PROGRAMS Agency Procurement of Energy Efficient Products § 436.42 Evaluation of Life-Cycle Cost...) ENERGY STAR qualified and FEMP designated products may be assumed to be life-cycle cost-effective. (b) In...

  13. 10 CFR 436.42 - Evaluation of Life-Cycle Cost Effectiveness.

    Code of Federal Regulations, 2010 CFR

    2010-01-01

    ... 10 Energy 3 2010-01-01 2010-01-01 false Evaluation of Life-Cycle Cost Effectiveness. 436.42... PROGRAMS Agency Procurement of Energy Efficient Products § 436.42 Evaluation of Life-Cycle Cost...) ENERGY STAR qualified and FEMP designated products may be assumed to be life-cycle cost-effective. (b) In...

  14. The naming of Neptune

    NASA Astrophysics Data System (ADS)

    Kollerstrom, Nicholas

    2009-03-01

    Le Verrier chose the name of Neptune immediately after hearing of the correctness of his prediction. This fact soon became obscured by François Arago's pledge made before the French Académie des Sciences, claiming that Le Verrier had entrusted him with the naming of the new planet. Then, British and German sources weighed in with differing names, and Britain's claim to co-prediction of the planet's position was expressed by their proposal of the name, `Oceanus'. Eventually in February of 1847 Airy urged upon Le Verrier that the name he had originally proposed, namely `Neptune' should be accepted, because it was the only one that could secure consensus.

  15. The Voyager encounter with Uranus and Neptune

    NASA Technical Reports Server (NTRS)

    Miner, Ellis D.

    1986-01-01

    Voyager 2 approaches Uranus at a relative low phase angle and high southerly latitude. Only when the spacecraft is very close to Uranus does the geometry change appreciably. Most of the important observations occur within six hours of closest approach. Voyager flies through an Earth and solar occulation zone and leaves Uranus at a relatively high phase angle of about 145 degrees. There isn't much of an opportunity to look at the equatorial region of the planet. At Neptune, on the other hand, the approach is more nearly equatorial (about 35 deg S lat). Voyager 2 will come much closer to Nepture than to any of the other gas giants as it skims within about 2000 km of Neptune's cloudtops. It will pass through earth and solar occultation zones at both Neptune and its satellite, Triton. Again, Voyager 2 will leave Neptune at about 35 deg S latitude. Voyager operational instrument, interplanetary trajectories and planetary encounters are briefly discussed.

  16. Optical navigation during the Voyager Neptune encounter

    NASA Technical Reports Server (NTRS)

    Riedel, J. E.; Owen, W. M., Jr.; Stuve, J. A.; Synnott, S. P.; Vaughan, R. M.

    1990-01-01

    Optical navigation techniques were required to successfully complete the planetary exploration phase of the NASA deep-space Voyager mission. The last of Voyager's planetary encounters, with Neptune, posed unique problems from an optical navigation standpoint. In this paper we briefly review general aspects of the optical navigation process as practiced during the Voyager mission, and discuss in detail particular features of the Neptune encounter which affected optical navigation. New approaches to the centerfinding problem were developed for both stars and extended bodies, and these are described. Results of the optical navigation data analysis are presented, as well as a description of the optical orbit determination system and results of its use during encounter. Partially as a result of the optical navigation processing, results of scientific significance were obtained. These results include the discovery and orbit determination of several new satellites of Neptune and the determination of the size of Triton, Neptune's largest moon.

  17. Global magnetic anomaly and aurora of Neptune

    NASA Technical Reports Server (NTRS)

    Cheng, Andrew F.

    1990-01-01

    The large offset and tilt of Neptune's dipole magnetic field combine to create a global magnetic anomaly, analogous to but much more important than earth's South Atlantic Anomaly. Energetic particle precipitation loss within the Neptune anomaly creates 'atmospheric drift shadows' within which particle fluxes are greatly reduced. The energetic particle dropout observed by Voyager near closest approach occurred near the predicted times when Voyager passed within the atmospheric drift shadow. Extremely soft, structured bursts of ions and electrons within the drift shadow may result from plasma wave-induced pitch angle scattering of trapped particles confined near the magnetic equator. The dropout does not necessarily imply that Voyager passed through an earth-like discrete auroral zone, as earlier reported. The ion and electron fluxes observed within the dropout period correspond to particles that must precipitate to Neptune's atmosphere within the anomaly region. This anomaly precipitation can account for a major portion of the ultraviolet emissions previously identified as Neptune aurora.

  18. GJ 832c: A Super-Earth in the Habitable Zone

    NASA Astrophysics Data System (ADS)

    Wittenmyer, Robert A.; Tuomi, Mikko; Butler, R. P.; Jones, H. R. A.; Anglada-Escudé, Guillem; Horner, Jonathan; Tinney, C. G.; Marshall, J. P.; Carter, B. D.; Bailey, J.; Salter, G. S.; O'Toole, S. J.; Wright, D.; Crane, J. D.; Schectman, S. A.; Arriagada, P.; Thompson, I.; Minniti, D.; Jenkins, J. S.; Diaz, M.

    2014-08-01

    We report the detection of GJ 832c, a super-Earth orbiting near the inner edge of the habitable zone of GJ 832, an M dwarf previously known to host a Jupiter analog in a nearly circular 9.4 yr orbit. The combination of precise radial-velocity measurements from three telescopes reveals the presence of a planet with a period of 35.68 ± 0.03 days and minimum mass (m sin i) of 5.4 ± 1.0 Earth masses. GJ 832c moves on a low-eccentricity orbit (e = 0.18 ± 0.13) toward the inner edge of the habitable zone. However, given the large mass of the planet, it seems likely that it would possess a massive atmosphere, which may well render the planet inhospitable. Indeed, it is perhaps more likely that GJ 832c is a "super-Venus," featuring significant greenhouse forcing. With an outer giant planet and an interior, potentially rocky planet, the GJ 832 planetary system can be thought of as a miniature version of our own solar system. This paper includes data gathered with the 6.5 m Magellan Telescopes located at the Las Campanas Observatory, Chile.

  19. Methane photochemistry and methane production on Neptune

    NASA Technical Reports Server (NTRS)

    Romani, P. N.; Atreya, S. K.

    1988-01-01

    The Neptune stratosphere's methane photochemistry is presently studied by means of a numerical model in which the observed mixing ratio of methane prompts photolysis near the CH4 homopause. Haze generation by methane photochemistry has its basis in the formation of hydrocarbon ices and polyacetylenes; the hazes can furnish the requisite aerosol haze at the appropriate pressure levels required by observations of Neptune in the visible and near-IR. Comparisons of model predictions with Uranus data indicate a lower ratio of polyacetylene production to hydrocarbon ice, as well as a lower likelihood of UV postprocessing of the acetylene ice to polymers on Neptune, compared to Uranus.

  20. Neptune and Titan Observed with Keck Telescope Adaptive Optics

    DOE Office of Scientific and Technical Information (OSTI.GOV)

    Max, C.E.; Macintosh, B.A.; Gibbard, S.

    2000-05-05

    The authors report on observations taken during engineering science validation time using the new adaptive optics system at the 10-m Keck II Telescope. They observe Neptune and Titan at near-infrared wavelengths. These objects are ideal for adaptive optics imaging because they are bright and small, yet have many diffraction-limited resolution elements across their disks. In addition Neptune and Titan have prominent physical features, some of which change markedly with time. They have observed infrared-bright storms on Neptune, and very low-albedo surface regions on Titan, Saturn's largest moon, Spatial resolution on Neptune and Titan was 0.05-0.06 and 0.04-0.05 arc sec, respectively.

  1. The K2-ESPRINT project. VI. K2-105 b, a hot Neptune around a metal-rich G-dwarf

    NASA Astrophysics Data System (ADS)

    Narita, Norio; Hirano, Teruyuki; Fukui, Akihiko; Hori, Yasunori; Dai, Fei; Yu, Liang; Livingston, John; Ryu, Tsuguru; Nowak, Grzegorz; Kuzuhara, Masayuki; Sato, Bun'ei; Takeda, Yoichi; Albrecht, Simon; Kudo, Tomoyuki; Kusakabe, Nobuhiko; Palle, Enric; Ribas, Ignasi; Tamura, Motohide; Van Eylen, Vincent; Winn, Joshua N.

    2017-04-01

    We report on the confirmation that the candidate transits observed for the star EPIC 211525389 are due to a short-period Neptune-sized planet. The host star, located in K2 campaign field 5, is a metal-rich ([Fe/H] = 0.26 ± 0.05) G-dwarf (Teff = 5430 ± 70 K and log g = 4.48 ± 0.09), based on observations with the High Dispersion Spectrograph (HDS) on the Subaru 8.2 m telescope. High spatial resolution AO imaging with HiCIAO on the Subaru telescope excludes faint companions near the host star, and the false positive probability of this target is found to be <10-6 using the open source vespa code. A joint analysis of transit light curves from K2 and additional ground-based multi-color transit photometry with MuSCAT on the Okayama 1.88 m telescope gives an orbital period of P = 8.266902 ± 0.000070 d and consistent transit depths of Rp/R⋆ ∼ 0.035 or (Rp/R⋆)2 ∼ 0.0012. The transit depth corresponds to a planetary radius of R_p = 3.59_{-0.39}^{+0.44} R_{\\oplus }, indicating that EPIC 211525389 b is a short-period Neptune-sized planet. Radial velocities of the host star, obtained with the Subaru HDS, lead to a 3 σ upper limit of 90 M⊕ (0.00027 M⊙) on the mass of EPIC 211525389 b, confirming its planetary nature. We expect this planet, newly named K2-105 b, to be the subject of future studies to characterize its mass, atmosphere, and spin-orbit (mis)alignment, as well as investigate the possibility of additional planets in the system.

  2. Engineering-Level Model Atmospheres for Titan and Neptune

    NASA Technical Reports Server (NTRS)

    Justus, C. G.; Duvall, Aleta; Johnson, D. L.

    2003-01-01

    Engineering-level atmospheric models for Titan and Neptune have been developed for use in NASA s systems analysis studies of aerocapture applications in missions to the outer planets. Analogous to highly successful Global Reference Atmospheric Models for Earth (GRAM, Justus et al., 2000) and Mars (Mars-GRAM, Justus and Johnson, 2001, Justus et al., 2002) the new models are called Titan-GRAM and Neptune-GRAM. Like GRAM and Mars-GRAM, an important feature of Titan-GRAM and Neptune-GRAM is their ability to simulate quasi-random perturbations for Monte- Carlo analyses in developing guidance, navigation and control algorithms, and for thermal systems design.

  3. The Tropospheres of Uranus and Neptune as seen at Microwave Wavelengths

    NASA Astrophysics Data System (ADS)

    Hofstadter, Mark D.; Butler, B. J.; Gurwell, M. A.; Hesman, B. E.; Devaraj, K.

    2008-09-01

    Brightness patterns seen at centimeter wavelengths are used to study the deep tropospheres of Uranus and Neptune (pressures from 1 to 50 bars). Early examples are Briggs and Andrew 1980 for Uranus (Icarus 41, 269-277) and Hofstadter et al. 1993 for Neptune (BAAS 25, 1077). We recently collected high-resolution Neptune data with the VLA at 1.3 and 2 cm under excellent conditions, allowing us to make a better comparison of the two ice-giants. As was known, the planets are grossly similar. The polar regions are the brightest (by tens of Kelvin, 20% brighter than the disk average), and both planets have less prominent, bright, mid-latitude bands. We can now say with confidence that Neptune's polar brightening covers a much smaller area than Uranus’ (at least in the south---Neptune's far north is not currently visible). Neptune's bright spot extends from -90 to about -75 degrees latitude, while Uranus’ extends down to -45 degrees at all times of the year. This, combined with Neptune's atmosphere being more opaque than Uranus', supports the idea that Neptune's deep troposphere is more convectively active. Convection brings absorbers (H2O, NH3, H2S) up to high altitudes, making some regions appear dim. Cloud formation in rising air depletes absorbers, changing the vertical opacity structure and making regions of subsidence absorber-free and bright. On Neptune, convective activity extends further towards the poles than it does on Uranus. We will discuss our results in light of recent observations of both planets at shorter wavelengths, and will present a re-analysis of older Neptune data in a search for temporal variability. This work was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. We acknowledge the support of NASA's Planetary Astronomy program, and of the VLA observatory.

  4. On the oblateness and rotation rate of Neptune's atmosphere

    NASA Technical Reports Server (NTRS)

    Hubbard, W. B.

    1986-01-01

    Recent observations of a stellar occultation by Neptune give an oblateness of 0.022 + or - 0.004 for Neptune's atmosphere at the 1-microbar pressure level. This results is consistent with hydrostatic equilibrium at a uniform atmospheric rotation period of 15 hours, although the error bars on quantities used in the calculation are such that an 18-hour period is not excluded. The oblateness of a planetary atmosphere is determined from stellar occultations by measuring the times at which a specified point on immersion or emersion occultation profiles is reached. Whether this standard procedure for deriving the shape of the atmosphere is consistent with what is known about vertical and horizontal temperature gradients in Neptune's atmosphere is evaluated. The nature of the constraint placed on the interior mass distribution by an oblateness determined in this manner is consided, as is the effects of possible differential rotation. A 15-hour Neptune internal mass distribution is approximately homologous to Uranus', but an 18-hour period is not. The implications for Neptune's interior structure if its body rotation period is actually 18 hours are discussed.

  5. Structure and evolution of Uranus and Neptune

    NASA Technical Reports Server (NTRS)

    Hubbard, W. B.; Macfarlane, J. J.

    1980-01-01

    Three-layer interior models of Uranus and Neptune with central rocky cores, mantles of water, methane, and ammonia (the 'ices'), and outer envelopes primarily composed of hydrogen and helium are presented. The models incorporate a new H2O equation of state based on experimental data which is considerably 'softer' than previous H2O equations of state. Corrections for interior temperatures approximately 5000 K are included in the models, and the thermal evolution of both planets is investigated using recent heat flow measurements. It is found that the evolutionary considerations are consistent with gravitational field data in supporting models with approximately solar abundances of 'ice' and 'rock'. Evolutionary considerations indicate that initial temperatures and luminosities for Uranus and Neptune were not substantially higher than the present value. Both planets apparently have relatively small approximately 1-2 earth masses) hydrogen-helium envelopes, with Neptune's envelope smaller than Uranus'. A monotonic trend is evident among the Jovian planets: all have central rock-ice cores of approximately 15 earth masses, but with hydrogen-helium envelopes which decrease in mass from Jupiter to Saturn to Uranus to Neptune.

  6. Voyager radio science observations of neptune and triton.

    PubMed

    Tyler, G L; Sweetnam, D N; Anderson, J D; Borutzki, S E; Campbell, J K; Eshleman, V R; Gresh, D L; Gurrola, E M; Hinson, D P; Kawashima, N; Kursinski, E R; Levy, G S; Lindal, G F; Lyons, J R; Marouf, E A; Rosen, P A; Simpson, R A; Wood, G E

    1989-12-15

    The Voyager 2 encounter with the Neptune system included radio science investigations of the masses and densities of Neptune and Triton, the low-order gravitational harmonics of Neptune, the vertical structures of the atmospheres and ionospheres of Neptune and Triton, the composition of the atmosphere of Neptune, and characteristics of ring material. Demanding experimental requirements were met successfully, and study of the large store of collected data has begun. The initial search of the data revealed no detectable effects of ring material with optical depth tau [unknown] 0.01. Preliminary representative results include the following: 1.0243 x 10(26) and 2.141 x 10(22) kilograms for the masses of Neptune and Triton; 1640 and 2054 kilograms per cubic meter for their respective densities; 1355 +/- 7 kilometers, provisionally, for the radius of Triton; and J(2) = 3411 +/- 10(x 10(-6)) and J(4) = -26(+12)(-20)(x10(-6)) for Neptune's gravity field (J>(2) and J(4) are harmonic coefficients of the gravity field). The equatorial and polar radii of Neptune are 24,764 +/- 20 and 24,340 +/- 30 kllometers, respectively, at the 10(5)-pascal (1 bar) pressure level. Neptune's atmosphere was probed to a pressure level of about 5 x 10(5) pascals, and effects of a methane cloud region and probable ammonia absorption below the cloud are evident in the data. Results for the mixing ratios of helium and ammonia are still being investigated; the methane abundance below the clouds is at least 1 percent by volume. Derived temperature-pressure profiles to 1.2 x 10(5) pascals and 78 kelvins (K) show a lapse rate corresponding to "frozen" equilibrium of the para- and ortho-hydrogen states. Neptune's ionosphere exhibits an extended topside at a temperature of 950 +/- 160 K if H(+) is the dominant ion, and narrow ionization layers of the type previously seen at the other three giant planets. Triton has a dense ionosphere with a peak electron concentration of 46 x 10(9) per cubic meter at an

  7. 16 CFR 436.11 - Severability.

    Code of Federal Regulations, 2010 CFR

    2010-01-01

    ... 16 Commercial Practices 1 2010-01-01 2010-01-01 false Severability. 436.11 Section 436.11 Commercial Practices FEDERAL TRADE COMMISSION TRADE REGULATION RULES DISCLOSURE REQUIREMENTS AND PROHIBITIONS CONCERNING FRANCHISING Other Provisions § 436.11 Severability. If any provision of this part is stayed or...

  8. The clouds and winds of Neptune

    NASA Astrophysics Data System (ADS)

    Beebe, R.

    1992-04-01

    The atmospheric features of Neptune are described based on the images from Voyager 2 with comparisons made to the atmosphere of Uranus. Specific attention is given to the clear atmosphere's methane content and lack of the smog associated with Uranus. Neptune absorbs only a small amount of energy from sunlight and radiates about 2.7 times as much as it absorbs. The mechanisms that keep Neptune's atmosphere free of smog are thought to be upwelling enhanced by an outward heat flow and melting ice. The Voyager photographs show streaks of white clouds indicating strong winds and probably white ice in the upper atmosphere. The Great Dark Spot and a small triangular cloud are described in terms of their periods of rotation, and the wind speed is discussed in terms of cloud variations. The Great Dark Spot drifted equatorward during the observational period, and the drift yields some important clues regarding the nature of the Neptunian atmosphere and climate.

  9. NEPTUNE Canada-status and planning

    NASA Astrophysics Data System (ADS)

    Bornhold, Brian D.

    2005-04-01

    Stage 1 of the joint Canada-U.S. NEPTUNE seafloor observatory has been funded by the Canada Foundation for Innovation and the British Columbia Knowledge Development Fund with an overall budget of $62.4 million. The network is designed to provide as close to real-time data and images as possible to be distributed to the research community, government agencies, educational institutions and the public via the Internet. Covering much of the northern segment of the Juan de Fuca Plate, this first phase of the NEPTUNE project is scheduled to be installed, with an initial suite of ``community experiments'', in 2008. As part of the planning, NEPTUNE Canada held a series of three workshops to develop the science plans for these ``community experiments'' these experiments have a budget of approximately $13 million. The experiments will cover the gamut of oceanographic science themes including various aspects of: ocean climate and marine productivity, seabed environments and biological communities, fluids at ocean ridges, gas hydrates and fluids on continental margins, plate tectonics processes, associated earthquakes and tsunamis. The next three years will be spent developing and testing the necessary instrumentation for deployment on the network.

  10. GJ 3236 - radial velocity determination

    NASA Astrophysics Data System (ADS)

    Kára, J.; Wolf, M.; Zharikov, S.

    2018-04-01

    We present a new study of low-mass red-dwarf eclipsing binary GJ 3236 using spectroscopic data obtained by the 2.12-m telescope at the San Pedro Mártir Observatory. We resolved radial velocities of both components of the binary and improved determination of the physical parameters of the binary.

  11. A Phase 2, Double-Blind, Placebo-Controlled Randomized Trial Assessing the Efficacy of ABT-436, a Novel V1b Receptor Antagonist, for Alcohol Dependence

    PubMed Central

    Ryan, Megan L; Falk, Daniel E; Fertig, Joanne B; Rendenbach-Mueller, Beatrice; Katz, David A; Tracy, Katherine A; Strain, Eric C; Dunn, Kelly E; Kampman, Kyle; Mahoney, Elizabeth; Ciraulo, Domenic A; Sickles-Colaneri, Laurie; Ait-Daoud, Nassima; Johnson, Bankole A; Ransom, Janet; Scott, Charles; Koob, George F; Litten, Raye Z

    2017-01-01

    Alcohol use disorder has been linked to dysregulation of the brain stress systems, producing a negative emotional state leading to chronic relapsing behavior. Vasopressin receptors appear to have a regulatory role in stress, anxiety, and alcohol. This study evaluated the novel compound, ABT-436, a V1b receptor antagonist, in alcohol-dependent participants in a 12-week clinical trial. Men and women (n=150) who met criteria for DSM–IV alcohol dependence were recruited across four sites. Participants received double-blind ABT-436 or placebo, and a computerized behavioral intervention. ABT-436 was titrated to 800 mg/day during weeks 2–12. Although the primary outcome, percentage of heavy drinking days, was lower in participants receiving ABT-436 compared with placebo, this difference was not statistically significant (31.3 vs 37.6, respectively; p=0.172; d=0.20). However, participants receiving ABT-436 had significantly greater percentage of days abstinent than those receiving placebo (51.2 vs 41.6, respectively; p=0.037; d=0.31). No significant differences were found between treatment groups on any other measures of drinking, alcohol craving, or alcohol-related consequences. Smokers receiving ABT-436 smoked significantly fewer cigarettes per week than those receiving placebo (p=0.046). ABT-436 was well tolerated, with diarrhea (mild-to-moderate severity) being the most common side effect. In subgroup analyses, participants with relatively higher baseline levels of stress responded better to ABT-436 than placebo on select drinking outcomes, suggesting there may be value in testing medications targeting the vasopressin receptor in high stress, alcohol-dependent patients. PMID:27658483

  12. 10 CFR 436.108 - Waivers.

    Code of Federal Regulations, 2010 CFR

    2010-01-01

    ... 10 Energy 3 2010-01-01 2010-01-01 false Waivers. 436.108 Section 436.108 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS Guidelines for General Operations Plans § 436.108 Waivers. (a) Any Federal agency may submit a written request to the Under...

  13. 42 CFR 436.300 - Scope.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... 42 Public Health 4 2010-10-01 2010-10-01 false Scope. 436.300 Section 436.300 Public Health CENTERS FOR MEDICARE & MEDICAID SERVICES, DEPARTMENT OF HEALTH AND HUMAN SERVICES (CONTINUED) MEDICAL... Medically Needy § 436.300 Scope. This subpart specifies the option for coverage of medically needy...

  14. 10 CFR 436.1 - Scope.

    Code of Federal Regulations, 2010 CFR

    2010-01-01

    ... 10 Energy 3 2010-01-01 2010-01-01 false Scope. 436.1 Section 436.1 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS § 436.1 Scope. This part sets forth the rules for Federal energy management and planning programs to reduce Federal energy consumption and...

  15. 10 CFR 436.1 - Scope.

    Code of Federal Regulations, 2013 CFR

    2013-01-01

    ... 10 Energy 3 2013-01-01 2013-01-01 false Scope. 436.1 Section 436.1 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS § 436.1 Scope. This part sets forth the rules for Federal energy management and planning programs to reduce Federal energy consumption and...

  16. 10 CFR 436.1 - Scope.

    Code of Federal Regulations, 2012 CFR

    2012-01-01

    ... 10 Energy 3 2012-01-01 2012-01-01 false Scope. 436.1 Section 436.1 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS § 436.1 Scope. This part sets forth the rules for Federal energy management and planning programs to reduce Federal energy consumption and...

  17. 10 CFR 436.1 - Scope.

    Code of Federal Regulations, 2014 CFR

    2014-01-01

    ... 10 Energy 3 2014-01-01 2014-01-01 false Scope. 436.1 Section 436.1 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS § 436.1 Scope. This part sets forth the rules for Federal energy management and planning programs to reduce Federal energy consumption and...

  18. 10 CFR 436.1 - Scope.

    Code of Federal Regulations, 2011 CFR

    2011-01-01

    ... 10 Energy 3 2011-01-01 2011-01-01 false Scope. 436.1 Section 436.1 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS § 436.1 Scope. This part sets forth the rules for Federal energy management and planning programs to reduce Federal energy consumption and...

  19. Characterizing the UV environment of GJ1214b

    NASA Astrophysics Data System (ADS)

    Desert, Jean-Michel

    2010-09-01

    The recent detection of a super-Earth transiting a nearby low-mass star GJ1214 {Charbonneau et al., 2009} has opened the door to testing the predictions of low mass planet atmosphere theories. Theoretical models predict that low mass planets are likely to exist with atmospheres that can vary widely in their composition and structure. Some super-Earths may be able to retain massive hydrogen-rich atmospheres. Others might never accumulate hydrogen or experience significant escape of lightweight elements, resulting in atmospheres more like those of the terrestrial planets in our Solar System. Planets which orbit close to their parent stars, such as close-in hot-Jupiters and super-Earths, are exposed to strong XEUV flux that influence their atmospheres and may trigger atmospheric escape processes. This phenomenon, which shapes planetary atmospheres, determines the evolution of the planet. This can also dramatically enhance the detectability of a heavily irradiated hydrogen atmosphere when the planet transits in front of its parent star. We propose to use HST/STIS/G140M to determine the intensity and variability of the Lyman-alpha chromospheric emission line and provide observational constraints to super-Earth atmospheric models. We propose to coordinate this measurement with a planetary transit in order to detect large upper atmospheric signatures if present. This short measurement also enables us to determine whether a larger program dedicated to upper atmospheric study is feasible for a following cycle.

  20. Uranus and Neptune orbiter missions via solar electric propulsion

    NASA Technical Reports Server (NTRS)

    Friedlander, A. L.; Brandenburg, R. K.

    1971-01-01

    The characteristics and capabilities of solar electric propulsion for performing orbiter missions at the planets Uranus and Neptune are described. An assessment of the scientific objectives and instrumentation requirements, their relation to orbit size selection, and parametric analysis of solar electric propulsion trajectory/payload performance are included. Utilizing the Titan 3D/Centaur launch vehicle, minimum flight times of about 3400 days to Uranus and 5300 days to Neptune are required to place the TOPS spacecraft into the nominal orbits. It has been shown that solar electric propulsion can be used effectively to accomplish elliptical orbiter missions at Uranus and Neptune. However, because of the very long flight time required, these mission profiles are not too attractive. Previous studies have shown that nuclear electric propulsion, if developed, would allow much faster trips; 5 years to Uranus and 8 years to Neptune.

  1. A thick cloud of Neptune Trojans and their colors.

    PubMed

    Sheppard, Scott S; Trujillo, Chadwick A

    2006-07-28

    The dynamical and physical properties of asteroids offer one of the few constraints on the formation, evolution, and migration of the giant planets. Trojan asteroids share a planet's semimajor axis but lead or follow it by about 60 degrees near the two triangular Lagrangian points of gravitational equilibrium. Here we report the discovery of a high-inclination Neptune Trojan, 2005 TN(53). This discovery demonstrates that the Neptune Trojan population occupies a thick disk, which is indicative of "freeze-in" capture instead of in situ or collisional formation. The Neptune Trojans appear to have a population that is several times larger than the Jupiter Trojans. Our color measurements show that Neptune Trojans have statistically indistinguishable slightly red colors, which suggests that they had a common formation and evolutionary history and are distinct from the classical Kuiper Belt objects.

  2. Long-term safety and efficacy of single-tablet combinations of solifenacin and tamsulosin oral controlled absorption system in men with storage and voiding lower urinary tract symptoms: results from the NEPTUNE Study and NEPTUNE II open-label extension.

    PubMed

    Drake, Marcus J; Chapple, Christopher; Sokol, Roman; Oelke, Matthias; Traudtner, Klaudia; Klaver, Monique; Drogendijk, Ted; Van Kerrebroeck, Philip

    2015-02-01

    Short-term trials have demonstrated the efficacy and safety of combination therapy using antimuscarinics and α-blockers in men with lower urinary tract symptoms (LUTS). The Study of Solifenacin Succinate and Tamsulosin Hydrochloride OCAS (oral controlled absorption system) in Males with Lower Urinary Tract Symptoms (NEPTUNE) II is the first long-term study using solifenacin (Soli) and the oral controlled absorption system formulation of tamsulosin (TOCAS). To evaluate long-term (up to 52 wk) safety and efficacy of flexible dosing of two fixed-dose combinations (FDC) of Soli plus TOCAS in men with moderate to severe storage symptoms and voiding symptoms. Patients with both storage and voiding LUTS, maximum urinary flow rate of 4.0-12.0 ml/s, prostate size <75 ml, and postvoid residuals ≤ 150 ml, who completed the 12-wk, double-blind NEPTUNE study could continue in the 40-wk, open-label NEPTUNE II study. FDC of Soli 6 mg plus TOCAS 0.4 mg, or Soli 9 mg plus TOCAS 0.4mg; patients could switch between doses in NEPTUNE II. Safety and efficacy data from NEPTUNE and NEPTUNE II were combined to cover a 52-wk period. Primary efficacy end points were total International Prostate Symptom Score (IPSS) and total urgency and frequency score (TUFS); secondary end points included IPSS storage and voiding subscores, micturition diary variables, and quality of life parameters. In all, 1066 men completed NEPTUNE and received one dose or more of study medication in NEPTUNE II. Treatment-emergent adverse events were reported in 499 (46.8%) patients who participated in NEPTUNE II; most were mild or moderate. Urinary retention occurred in 13 of 1208 (1.1%) patients receiving one or more FDCs in NEPTUNE and/or NEPTUNE II; 8 (0.7%) required catheterisation (acute urinary retention [AUR]). Reductions in total IPSS and TUFS during NEPTUNE were maintained for up to 52 wk of FDC treatment, with mean reductions of 9.0 (standard deviation [SD]: 5.7) and 10.1 (SD: 9.2), respectively, from

  3. 42 CFR 436.2 - Basis.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... 42 Public Health 4 2011-10-01 2011-10-01 false Basis. 436.2 Section 436.2 Public Health CENTERS FOR MEDICARE & MEDICAID SERVICES, DEPARTMENT OF HEALTH AND HUMAN SERVICES (CONTINUED) MEDICAL ASSISTANCE PROGRAMS ELIGIBILITY IN GUAM, PUERTO RICO, AND THE VIRGIN ISLANDS General Provisions and Definitions § 436.2 Basis. This part implements the...

  4. 42 CFR 436.2 - Basis.

    Code of Federal Regulations, 2014 CFR

    2014-10-01

    ... 42 Public Health 4 2014-10-01 2014-10-01 false Basis. 436.2 Section 436.2 Public Health CENTERS FOR MEDICARE & MEDICAID SERVICES, DEPARTMENT OF HEALTH AND HUMAN SERVICES (CONTINUED) MEDICAL ASSISTANCE PROGRAMS ELIGIBILITY IN GUAM, PUERTO RICO, AND THE VIRGIN ISLANDS General Provisions and Definitions § 436.2 Basis. This part implements the...

  5. 42 CFR 436.2 - Basis.

    Code of Federal Regulations, 2013 CFR

    2013-10-01

    ... 42 Public Health 4 2013-10-01 2013-10-01 false Basis. 436.2 Section 436.2 Public Health CENTERS FOR MEDICARE & MEDICAID SERVICES, DEPARTMENT OF HEALTH AND HUMAN SERVICES (CONTINUED) MEDICAL ASSISTANCE PROGRAMS ELIGIBILITY IN GUAM, PUERTO RICO, AND THE VIRGIN ISLANDS General Provisions and Definitions § 436.2 Basis. This part implements the...

  6. 42 CFR 436.2 - Basis.

    Code of Federal Regulations, 2012 CFR

    2012-10-01

    ... 42 Public Health 4 2012-10-01 2012-10-01 false Basis. 436.2 Section 436.2 Public Health CENTERS FOR MEDICARE & MEDICAID SERVICES, DEPARTMENT OF HEALTH AND HUMAN SERVICES (CONTINUED) MEDICAL ASSISTANCE PROGRAMS ELIGIBILITY IN GUAM, PUERTO RICO, AND THE VIRGIN ISLANDS General Provisions and Definitions § 436.2 Basis. This part implements the...

  7. 42 CFR 436.2 - Basis.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... 42 Public Health 4 2010-10-01 2010-10-01 false Basis. 436.2 Section 436.2 Public Health CENTERS FOR MEDICARE & MEDICAID SERVICES, DEPARTMENT OF HEALTH AND HUMAN SERVICES (CONTINUED) MEDICAL ASSISTANCE PROGRAMS ELIGIBILITY IN GUAM, PUERTO RICO, AND THE VIRGIN ISLANDS General Provisions and Definitions § 436.2 Basis. This part implements the...

  8. The discoveries of Neptune and Triton.

    NASA Astrophysics Data System (ADS)

    Moore, P.

    The story of the tracking-down of Neptune has been told many times, but even today there are still discrepancies in the various accounts, to say nothing of conflicting opinions. To some people, John Couch Adams is a shining hero and George Biddell Airy a black villain; to others it is Le Verrier who is the hero, and Adams an unimportant member of the supporting cast. Of course, all this is absurd. In the author's view, the true discoverers of Neptune were Johann Gottfried Galle and Heinrich D'Arrest.

  9. Voyager 2 Uranus and Neptune targeting

    NASA Technical Reports Server (NTRS)

    Gray, D. L.; Cesarone, R. J.; Van Allen, R. E.

    1982-01-01

    Targeting strategies are developed for the Voyager 2 flybys of Uranus and Neptune/Triton. The need to maximize science return, conserve propellant, and maintain spacecraft safety presents a challenge, given the difficulty in estimating the spacecraft orbit relative to these outer planets. Expected propellant usage, science return, and targeting complexity are presented for each targeting strategy. For the dual encounter of Neptune and its satellite Triton, split targeting conditions are proposed to fix the most important conditions at each body, and thus minimize science losses resulting from Triton ephemeris uncertainties.

  10. Theory for planetary exospheres: III. Radiation pressure effect on the Circular Restricted Three Body Problem and its implication on planetary atmospheres

    NASA Astrophysics Data System (ADS)

    Beth, A.; Garnier, P.; Toublanc, D.; Dandouras, I.; Mazelle, C.

    2016-12-01

    The planetary exospheres are poorly known in their outer parts, since the neutral densities are low compared with the instruments detection capabilities. The exospheric models are thus often the main source of information at such high altitudes. We present a new way to take into account analytically the additional effect of the stellar radiation pressure on planetary exospheres. In a series of papers, we present with a Hamiltonian approach the effect of the radiation pressure on dynamical trajectories, density profiles and escaping thermal flux. Our work is a generalization of the study by Bishop and Chamberlain [1989] Icarus, 81, 145-163. In this third paper, we investigate the effect of the stellar radiation pressure on the Circular Restricted Three Body Problem (CR3BP), called also the photogravitational CR3BP, and its implication on the escape and the stability of planetary exospheres, especially for hot Jupiters. In particular, we describe the transformation of the equipotentials and the location of the Lagrange points, and we provide a modified equation for the Hill sphere radius that includes the influence of the radiation pressure. Finally, an application to the hot Jupiter HD 209458b and hot Neptune GJ 436b reveals the existence of a blow-off escape regime induced by the stellar radiation pressure.

  11. First Earth-based observations of Neptune's satellite Proteus

    NASA Astrophysics Data System (ADS)

    Colas, F.; Buil, C.

    1992-08-01

    Proteus (Neptune III) was discovered from Voyager Spacecraft images in 1989 (Smith, 1989). It was never observed from ground-based observatories because of its magnitude (m = 20.3) and closeness to Neptune (maximum elongation = 6 arcsec). In October 1991, we used the 2.2 m telescope at the European Southern Observatory (La Silla, Chile) to look for it. The observation success is mainly due to the use of an anti blooming CCD and to good seeing conditions (less than 1 arcsec). We give the differential positions of Proteus referred to Neptune and we compare with theoretical positions issued from Voyager's data (Owen et al., 1991). We found that the rms orbital residual was about 0.1 arcsec.

  12. Orbits of the inner satellites of Neptune

    NASA Astrophysics Data System (ADS)

    Brozovic, Marina; Showalter, Mark R.; Jacobson, Robert Arthur; French, Robert S.; de Pater, Imke; Lissauer, Jack

    2018-04-01

    We report on the numerically integrated orbits of seven inner satellites of Neptune, including S/2004 N1, the last moon of Neptune to be discovered by the Hubble Space Telescope (HST). The dataset includes Voyager imaging data as well as the HST and Earth-based astrometric data. The observations span time period from 1989 to 2016. Our orbital model accounts for the equatorial bulge of Neptune, perturbations from the Sun and the planets, and perturbations from Triton. The initial orbital integration assumed that the satellites are massless, but the residuals improved significantly as the masses adjusted toward values that implied that the density of the satellites is in the realm of 1 g/cm3. We will discuss how the integrated orbits compare to the precessing ellipses fits, mean orbital elements, current orbital uncertainties, and the need for future observations.

  13. HAT-P-26b: A Neptune-mass exoplanet with a well-constrained heavy element abundance

    NASA Astrophysics Data System (ADS)

    Wakeford, Hannah R.; Sing, David K.; Kataria, Tiffany; Deming, Drake; Nikolov, Nikolay; Lopez, Eric D.; Tremblin, Pascal; Amundsen, David S.; Lewis, Nikole K.; Mandell, Avi M.; Fortney, Jonathan J.; Knutson, Heather; Benneke, Björn; Evans, Thomas M.

    2017-05-01

    A correlation between giant-planet mass and atmospheric heavy elemental abundance was first noted in the past century from observations of planets in our own Solar System and has served as a cornerstone of planet-formation theory. Using data from the Hubble and Spitzer Space Telescopes from 0.5 to 5 micrometers, we conducted a detailed atmospheric study of the transiting Neptune-mass exoplanet HAT-P-26b. We detected prominent H2O absorption bands with a maximum base-to-peak amplitude of 525 parts per million in the transmission spectrum. Using the water abundance as a proxy for metallicity, we measured HAT-P-26b’s atmospheric heavy element content (4.8-4.0+21.5 times solar). This likely indicates that HAT-P-26b’s atmosphere is primordial and obtained its gaseous envelope late in its disk lifetime, with little contamination from metal-rich planetesimals.

  14. HADES RV Programme with HARPS-N at TNG. VI. GJ 3942 b behind dominant activity signals

    NASA Astrophysics Data System (ADS)

    Perger, M.; Ribas, I.; Damasso, M.; Morales, J. C.; Affer, L.; Suárez Mascareño, A.; Micela, G.; Maldonado, J.; González Hernández, J. I.; Rebolo, R.; Scandariato, G.; Leto, G.; Zanmar Sanchez, R.; Benatti, S.; Bignamini, A.; Borsa, F.; Carbognani, A.; Claudi, R.; Desidera, S.; Esposito, M.; Lafarga, M.; Martinez Fiorenzano, A. F.; Herrero, E.; Molinari, E.; Nascimbeni, V.; Pagano, I.; Pedani, M.; Poretti, E.; Rainer, M.; Rosich, A.; Sozzetti, A.; Toledo-Padrón, B.

    2017-12-01

    Context. Short- to mid-term magnetic phenomena on the stellar surface of M-type stars can resemble the effects of planets in radial velocity data, and may also hide them. Aims: We analyze 145 spectroscopic HARPS-N observations of GJ 3942 taken over the past five years and additional photometry in order to disentangle stellar activity effects from genuine Doppler signals as a result of the orbital motion of the star around the common barycenter with its planet. Methods: To achieve this, we use the common methods of pre-whitening, and treat the correlated red noise by a first-order moving average term and by Gaussian-process regression following an MCMC analysis. Results: We identify the rotational period of the star at 16.3 days and discover a new super-Earth, GJ 3942 b, with an orbital period of 6.9 days and a minimum mass of 7.1 M⊕. An additional signal in the periodogram of the residuals is present, but at this point we cannot claim with sufficient significance that it is related to a second planet. If confirmed, this planet candidate would have a minimum mass of 6.3 M⊕ and a period of 10.4 days, which might indicate a 3:2 mean-motion resonance with the inner planet. Based on observations made with the Italian Telescopio Nazionale Galileo (TNG), operated on the island of La Palma by the INAF - Fundación Galileo Galilei at the Roque de los Muchachos Observatory of the Instituto de Astrofísica de Canarias (IAC); photometric observations from the APACHE array located at the Astronomical Observatory of the Aosta Valley; photometric observations made with the robotic APT2 (within the EXORAP program) located at Serra La Nave on Mt. Etna.Table 9 is only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (http://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/608/A63

  15. Detection of CS in Neptune's atmosphere from ALMA observations

    NASA Astrophysics Data System (ADS)

    Moreno, R.; Lellouch, E.; Cavalié, T.; Moullet, A.

    2017-12-01

    Context. The large and vertically non-uniform abundance of CO in Neptune's atmosphere has been interpreted as the result of past cometary impact(s), either single or distributed in size and time, which could also be at the origin of Neptune's HCN. Aims: We aim to provide observational support for this scenario by searching for other comet-induced species, in particular carbon sulfide (CS) which has been observed continuously in Jupiter since the 1994 Shoemaker-Levy 9 impacts. Methods: In April 2016 we used the ALMA interferometer to search for CS(7-6) at 342.883 GHz in Neptune. Results: We report on the detection of CS in Neptune's atmosphere, the first unambiguous observation of a sulfur-bearing species in a giant planet beyond Jupiter. Carbon sulfide appears to be present only at submillibar levels, with a column density of (2.0-3.1) × 1012 cm-2, and a typical mixing ratio of (2-20) × 10-11 that depends on its precise vertical location. The favoured origin of CS is deposition by a putative large comet impact several centuries ago, and the strong depletion of CS with respect to CO - compared to the Jupiter case - is likely due to the CS sticking to aerosols or clustering to form polymers in Neptune's lower stratosphere. Conclusions: The CS detection, along with recent analyses of the CO profile, reinforces the presumption of a large comet impact into Neptune 1000 yr ago, that delivered CO, CS, and HCN at the same time.

  16. The Atmospheric Diversity of Mini-Neptunes in Multi-planet Systems

    NASA Astrophysics Data System (ADS)

    Crossfield, Ian

    2017-08-01

    Mini-Neptunes, planets 2-4 times the size of the Earth, are anintriguing population. They are an abundant outcome of planetformation and occur around more than a quarter of all stars -- yetthey are absent in the Solar System. Mini-Neptunes bridge the gapbetween terrestrial planets and gas giants, and atmospherecharacterization of these planets has much to reveal about their currentproperties, origins, and evolutionary histories. However, only a handful of mini-Neptunes have been amenable to atmospheric study so far.We propose a survey of four mini-Neptunes recently discovered by ourteam around bright, nearby stars. These observations will nearlydouble the number of planets in this size range with measuredtransmission spectra. Our observations will yield high-precisionconstraints on the planets' atmospheric metallicities, elementalabundances, C/O ratios, and aerosol content. With a greatly expandedmini-Neptune sample, we will identify trends in planet properties as afunction of equilibrium temperature, UV irradiation, planet mass, andstellar spectral type. These trends will also identify specificpromising targets for further study with JWST, and will help usprioritize follow-up and atmospheric characterization of themany small planets expected from the TESS survey.

  17. Aerocapture Systems Analysis for a Neptune Mission

    NASA Technical Reports Server (NTRS)

    Lockwood, Mary Kae; Edquist, Karl T.; Starr, Brett R.; Hollis, Brian R.; Hrinda, Glenn A.; Bailey, Robert W.; Hall, Jeffery L.; Spilker, Thomas R.; Noca, Muriel A.; O'Kongo, N.

    2006-01-01

    A Systems Analysis was completed to determine the feasibility, benefit and risk of an aeroshell aerocapture system for Neptune and to identify technology gaps and technology performance goals. The systems analysis includes the following disciplines: science; mission design; aeroshell configuration; interplanetary navigation analyses; atmosphere modeling; computational fluid dynamics for aerodynamic performance and aeroheating environment; stability analyses; guidance development; atmospheric flight simulation; thermal protection system design; mass properties; structures; spacecraft design and packaging; and mass sensitivities. Results show that aerocapture is feasible and performance is adequate for the Neptune mission. Aerocapture can deliver 1.4 times more mass to Neptune orbit than an all-propulsive system for the same launch vehicle and results in a 3-4 year reduction in trip time compared to all-propulsive systems. Enabling technologies for this mission include TPS manufacturing; and aerothermodynamic methods for determining coupled 3-D convection, radiation and ablation aeroheating rates and loads.

  18. Neptune Hot South Pole

    NASA Image and Video Library

    2007-09-18

    These thermal images show a hot south pole on the planet Neptune. These warmer temperatures provide an avenue for methane to escape out of the deep atmosphere. The images were obtained with the Very Large Telescope in Chile Sept. 1 and 2, 2006.

  19. HUBBLE FINDS NEW DARK SPOT ON NEPTUNE

    NASA Technical Reports Server (NTRS)

    2002-01-01

    NASA's Hubble Space Telescope has discovered a new great dark spot, located in the northern hemisphere of the planet Neptune. Because the planet's northern hemisphere is now tilted away from Earth, the new feature appears near the limb of the planet. The spot is a near mirror-image to a similar southern hemisphere dark spot that was discovered in 1989 by the Voyager 2 probe. In 1994, Hubble showed that the southern dark spot had disappeared. Like its predecessor, the new spot has high altitude clouds along its edge, caused by gasses that have been pushed to higher altitudes where they cool to form methane ice crystal clouds. The dark spot may be a zone of clear gas that is a window to a cloud deck lower in the atmosphere. Planetary scientists don t know how long lived this new feature might be. Hubble's high resolution will allow astronomers to follow the spot's evolution and other unexpected changes in Neptune's dynamic atmosphere. The image was taken on November 2, 1994 with Hubble's Wide Field Planetary Camera 2, when Neptune was 2.8 billion miles (4.5 billion kilometers) from Earth. Hubble can resolve features as small as 625 miles (1,000 kilometers) across in Neptune's cloud tops. Credit: H. Hammel (Massachusetts Institute of Technology) and NASA

  20. From dense hot Jupiter to low-density Neptune: The discovery of WASP-127b, WASP-136b, and WASP-138b

    NASA Astrophysics Data System (ADS)

    Lam, K. W. F.; Faedi, F.; Brown, D. J. A.; Anderson, D. R.; Delrez, L.; Gillon, M.; Hébrard, G.; Lendl, M.; Mancini, L.; Southworth, J.; Smalley, B.; Triaud, A. H. M.; Turner, O. D.; Hay, K. L.; Armstrong, D. J.; Barros, S. C. C.; Bonomo, A. S.; Bouchy, F.; Boumis, P.; Collier Cameron, A.; Doyle, A. P.; Hellier, C.; Henning, T.; Jehin, E.; King, G.; Kirk, J.; Louden, T.; Maxted, P. F. L.; McCormac, J. J.; Osborn, H. P.; Palle, E.; Pepe, F.; Pollacco, D.; Prieto-Arranz, J.; Queloz, D.; Rey, J.; Ségransan, D.; Udry, S.; Walker, S.; West, R. G.; Wheatley, P. J.

    2017-03-01

    We report three newly discovered exoplanets from the SuperWASP survey. WASP-127b is a heavily inflated super-Neptune of mass 0.18±0.02 MJ and radius 1.37±0.04 RJ. This is one of the least massive planets discovered by the WASP project. It orbits a bright host star (Vmag = 10.16) of spectral type G5 with a period of 4.17 days. WASP-127b is a low-density planet that has an extended atmosphere with a scale height of 2500 ± 400 km, making it an ideal candidate for transmission spectroscopy. WASP-136b and WASP-138b are both hot Jupiters with mass and radii of 1.51 ± 0.08 MJ and 1.38 ± 0.16 RJ, and 1.22 ± 0.08 MJ and 1.09 ± 0.05 RJ, respectively. WASP-136b is in a 5.22-day orbit around an F9 subgiant star with a mass of 1.41 ± 0.07 M⊙ and a radius of 2.21 ± 0.22 R⊙. The discovery of WASP-136b could help constrain the characteristics of the giant planet population around evolved stars. WASP-138b orbits an F7 star with a period of 3.63 days. Its radius agrees with theoretical values from standard models, suggesting the presence of a heavy element core with a mass of 10 M⊕. The discovery of these new planets helps in exploring the diverse compositional range of short-period planets, and will aid our understanding of the physical characteristics of both gas giants and low-density planets. Radial velocity and photometry tables are only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (http://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/599/A3

  1. Discovery of a Bright Equatorial Storm on Neptune

    NASA Astrophysics Data System (ADS)

    Molter, E. M.; De Pater, I.; Alvarez, C.; Tollefson, J.; Luszcz-Cook, S.

    2017-12-01

    Images of Neptune, taken with the NIRC2 instrument during testing of the new Twilight Zone observing program at Keck Observatory, revealed an extremely large bright storm system near Neptune's equator. The storm complex is ≈9,000 km across and brightened considerably between June 26 and July 2. Historically, very bright clouds have occasionally been seen on Neptune, but always in the midlatitude regions between ≈15° and ≈60° North or South. Voyager and HST observations have shown that cloud features large enough to dominate near-IR photometry are often "companion" clouds of dark anti-cyclonic vortices similar to Jupiter's Great Red Spot, interpreted as orographic clouds. In the past such clouds and their coincident dark vortices often persisted for one up to several years. However, the cloud complex we detect is unique: never before has a bright cloud been seen at, or so close to, the equator. The discovery points to a drastic departure in the dynamics of Neptune's atmosphere from what has been observed for the past several decades. Detections of the complex in multiple NIRC2 filters allows radiative transfer modeling to constrain the cloud's altitude and vertical extent.

  2. The Volatility of Far-Ultraviolet Radiation from Low-Mass Stars and Planetary Implications

    NASA Astrophysics Data System (ADS)

    Loyd, R. O. Parke

    A low-mass star emits only 0.001-0.01% of its electromagnetic energy in the ultraviolet (100 - 1700 A), yet the implications for planets are profound. Radiation at the short-wavelength end of this range, the extreme ultraviolet (100 - 912 A), powers planetary atmospheric escape that can be observed through transit spectroscopy in the far ultraviolet (FUV; 912 - 1700 A). In addition, FUV light that penetrates further into a planet's atmosphere photolyzes molecules, driving nonthermal chemistry capable of producing O2 and O3 abiotically. I present results from extensive Hubble Space Telescope (HST) observations of the FUV emission from low-mass stars, focusing on its variability in time. Using all available archival data, I determined an astrophysical noise floor on detectable absorption in the C II, Si III, and Si IV FUV lines due to a transiting evaporating planet. I analyzed such a transit of the evaporating hot-Neptune GJ 436b, finding no detectable absorption in C II or Si III despite a large (>50%) transit in Lyalpha, but placing upper limits that agree with a photochemical-hydrodynamical model of the planetary outflow. These observations of GJ 436 were part of the MUSCLES Treasury Survey, a much larger dataset covering 7 M and 4 K dwarf stars. A time series analysis of all of these data constrained FUV flares on the surveyed M dwarfs, which I augmented with archival data on well-studied flare stars. The analysis confirmed that M dwarf flares are ubiquitous. In relative units, the FUV flares of the "inactive" MUSCLES M dwarfs are equally as energetic and frequent as those of the M dwarf flare stars. Both flare 3 orders of magnitude more frequently than the sun. Indeed, flares possibly (if not probably) dominate the energy budget of FUV emission from M dwarf stars. Highly energetic flares occurring roughly yearly could annihilate most of the ozone from an Earth-like atmosphere. However, the effect is short-lived, unless additional reactions not accounted for or

  3. 40 CFR 436.381 - Specialized definitions.

    Code of Federal Regulations, 2011 CFR

    2011-07-01

    ... 40 Protection of Environment 30 2011-07-01 2011-07-01 false Specialized definitions. 436.381 Section 436.381 Protection of Environment ENVIRONMENTAL PROTECTION AGENCY (CONTINUED) EFFLUENT GUIDELINES AND STANDARDS MINERAL MINING AND PROCESSING POINT SOURCE CATEGORY Graphite Subcategory § 436.381...

  4. 40 CFR 436.181 - Specialized definitions.

    Code of Federal Regulations, 2011 CFR

    2011-07-01

    ... 40 Protection of Environment 30 2011-07-01 2011-07-01 false Specialized definitions. 436.181 Section 436.181 Protection of Environment ENVIRONMENTAL PROTECTION AGENCY (CONTINUED) EFFLUENT GUIDELINES AND STANDARDS MINERAL MINING AND PROCESSING POINT SOURCE CATEGORY Phosphate Rock Subcategory § 436.181...

  5. 40 CFR 436.131 - Specialized definitions.

    Code of Federal Regulations, 2010 CFR

    2010-07-01

    ... 40 Protection of Environment 29 2010-07-01 2010-07-01 false Specialized definitions. 436.131 Section 436.131 Protection of Environment ENVIRONMENTAL PROTECTION AGENCY (CONTINUED) EFFLUENT GUIDELINES AND STANDARDS MINERAL MINING AND PROCESSING POINT SOURCE CATEGORY Borax Subcategory § 436.131...

  6. 40 CFR 436.131 - Specialized definitions.

    Code of Federal Regulations, 2013 CFR

    2013-07-01

    ... 40 Protection of Environment 31 2013-07-01 2013-07-01 false Specialized definitions. 436.131 Section 436.131 Protection of Environment ENVIRONMENTAL PROTECTION AGENCY (CONTINUED) EFFLUENT GUIDELINES AND STANDARDS (CONTINUED) MINERAL MINING AND PROCESSING POINT SOURCE CATEGORY Borax Subcategory § 436...

  7. 40 CFR 436.131 - Specialized definitions.

    Code of Federal Regulations, 2011 CFR

    2011-07-01

    ... 40 Protection of Environment 30 2011-07-01 2011-07-01 false Specialized definitions. 436.131 Section 436.131 Protection of Environment ENVIRONMENTAL PROTECTION AGENCY (CONTINUED) EFFLUENT GUIDELINES AND STANDARDS MINERAL MINING AND PROCESSING POINT SOURCE CATEGORY Borax Subcategory § 436.131...

  8. 40 CFR 436.131 - Specialized definitions.

    Code of Federal Regulations, 2012 CFR

    2012-07-01

    ... 40 Protection of Environment 31 2012-07-01 2012-07-01 false Specialized definitions. 436.131 Section 436.131 Protection of Environment ENVIRONMENTAL PROTECTION AGENCY (CONTINUED) EFFLUENT GUIDELINES AND STANDARDS (CONTINUED) MINERAL MINING AND PROCESSING POINT SOURCE CATEGORY Borax Subcategory § 436...

  9. 40 CFR 436.131 - Specialized definitions.

    Code of Federal Regulations, 2014 CFR

    2014-07-01

    ... 40 Protection of Environment 30 2014-07-01 2014-07-01 false Specialized definitions. 436.131 Section 436.131 Protection of Environment ENVIRONMENTAL PROTECTION AGENCY (CONTINUED) EFFLUENT GUIDELINES AND STANDARDS (CONTINUED) MINERAL MINING AND PROCESSING POINT SOURCE CATEGORY Borax Subcategory § 436...

  10. 40 CFR 436.241 - Specialized definitions.

    Code of Federal Regulations, 2011 CFR

    2011-07-01

    ... 40 Protection of Environment 30 2011-07-01 2011-07-01 false Specialized definitions. 436.241 Section 436.241 Protection of Environment ENVIRONMENTAL PROTECTION AGENCY (CONTINUED) EFFLUENT GUIDELINES AND STANDARDS MINERAL MINING AND PROCESSING POINT SOURCE CATEGORY Diatomite Subcategory § 436.241...

  11. 40 CFR 436.241 - Specialized definitions.

    Code of Federal Regulations, 2010 CFR

    2010-07-01

    ... 40 Protection of Environment 29 2010-07-01 2010-07-01 false Specialized definitions. 436.241 Section 436.241 Protection of Environment ENVIRONMENTAL PROTECTION AGENCY (CONTINUED) EFFLUENT GUIDELINES AND STANDARDS MINERAL MINING AND PROCESSING POINT SOURCE CATEGORY Diatomite Subcategory § 436.241...

  12. 40 CFR 436.381 - Specialized definitions.

    Code of Federal Regulations, 2010 CFR

    2010-07-01

    ... 40 Protection of Environment 29 2010-07-01 2010-07-01 false Specialized definitions. 436.381 Section 436.381 Protection of Environment ENVIRONMENTAL PROTECTION AGENCY (CONTINUED) EFFLUENT GUIDELINES AND STANDARDS MINERAL MINING AND PROCESSING POINT SOURCE CATEGORY Graphite Subcategory § 436.381...

  13. 10 CFR 436.43 - Procurement planning.

    Code of Federal Regulations, 2010 CFR

    2010-01-01

    ... 10 Energy 3 2010-01-01 2010-01-01 false Procurement planning. 436.43 Section 436.43 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS Agency Procurement of Energy Efficient Products § 436.43 Procurement planning. (a) Agencies should consider the...

  14. 78 FR 42587 - Deepwater Port License: Amendment of the Neptune LNG LLC Deepwater Port License and Temporary...

    Federal Register 2010, 2011, 2012, 2013, 2014

    2013-07-16

    ... Neptune LNG LLC Deepwater Port License and Temporary Suspension of Operations at the Neptune LNG Deepwater... decision to approve the request of Neptune LNG LLC (Neptune) for a temporary five-year suspension of port operations at the Neptune Deepwater Port by amending the Neptune Deepwater Port License. ADDRESSES: The...

  15. 48 CFR 436.602-4 - Selection authority.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... 48 Federal Acquisition Regulations System 4 2010-10-01 2010-10-01 false Selection authority. 436... Selection authority. (a) The HCA shall serve as the selection authority in accordance with FAR 36.602-4. The... selection authority. (b) A copy of the final selection, inclusive of the supporting documents, shall be...

  16. An Empirically Derived Three-Dimensional Laplace Resonance in the GJ 876 Planetary System

    NASA Astrophysics Data System (ADS)

    Nelson, Benjamin Earl; Robertson, Paul; Pritchard, Seth

    2015-08-01

    We report constraints on the three-dimensional orbital architecture for all four planets known to orbit the nearby M dwarf Gliese 876 (=GJ 876) based solely on Doppler measurements and demanding long-term orbital stability. Our dataset incorporates publicly available radial velocities taken with the ELODIE and CORALIE spectrographs, HARPS, and Keck HIRES as well as previously unpublished HIRES RVs. We first quantitatively assess the validity of the planets thought to orbit GJ 876 by computing the Bayes factors for a variety of different coplanar models using an importance sampling algorithm. We confirm that a four-planet model is indeed preferred over a three-planet model. Next, we apply a Newtonian MCMC algorithm (RUN DMC, B. Nelson et al. 2014) to perform a Bayesian analysis of the planet masses and orbits using an n-body model that allows each planet to take on its own orbit in three-dimensional space. Based on the radial velocities alone, the mutual inclinations for the outer three resonant planets are constrained to Φcb = 2.8±1.71.3 degrees for the "c" and "b" pair and Φbe = 10.3±6.35.1 degrees for the "b" and "e" pair. We integrate the equations of motion of a sample of initial conditions drawn from our posterior for 107 years. We identify dynamically unstable models and find that the GJ 876 planets must be roughly coplanar (Φcb = 1.41±0.620.57 degrees) and (Φbe = 3.9±2.01.9 degrees), indicating the amount of planet-planet scattering in the system has been low. We investigate the distribution of the respective resonant arguments of each planet pair and find that at least one resonant argument for each planet pair and the Laplace argument librate. The libration amplitudes in our three-dimensional orbital model supports the idea of the outer-three planets having undergone significant past disk migration.

  17. 10 CFR 436.14 - Methodological assumptions.

    Code of Federal Regulations, 2011 CFR

    2011-01-01

    ... 10 Energy 3 2011-01-01 2011-01-01 false Methodological assumptions. 436.14 Section 436.14 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS Methodology and Procedures for Life Cycle Cost Analyses § 436.14 Methodological assumptions. (a) Each Federal Agency shall...

  18. 10 CFR 436.14 - Methodological assumptions.

    Code of Federal Regulations, 2013 CFR

    2013-01-01

    ... 10 Energy 3 2013-01-01 2013-01-01 false Methodological assumptions. 436.14 Section 436.14 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS Methodology and Procedures for Life Cycle Cost Analyses § 436.14 Methodological assumptions. (a) Each Federal Agency shall...

  19. 10 CFR 436.14 - Methodological assumptions.

    Code of Federal Regulations, 2012 CFR

    2012-01-01

    ... 10 Energy 3 2012-01-01 2012-01-01 false Methodological assumptions. 436.14 Section 436.14 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS Methodology and Procedures for Life Cycle Cost Analyses § 436.14 Methodological assumptions. (a) Each Federal Agency shall...

  20. 10 CFR 436.14 - Methodological assumptions.

    Code of Federal Regulations, 2010 CFR

    2010-01-01

    ... 10 Energy 3 2010-01-01 2010-01-01 false Methodological assumptions. 436.14 Section 436.14 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS Methodology and Procedures for Life Cycle Cost Analyses § 436.14 Methodological assumptions. (a) Each Federal Agency shall...

  1. 10 CFR 436.14 - Methodological assumptions.

    Code of Federal Regulations, 2014 CFR

    2014-01-01

    ... 10 Energy 3 2014-01-01 2014-01-01 false Methodological assumptions. 436.14 Section 436.14 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS Methodology and Procedures for Life Cycle Cost Analyses § 436.14 Methodological assumptions. (a) Each Federal Agency shall...

  2. 42 CFR 436.121 - Qualified family members.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... 42 Public Health 4 2011-10-01 2011-10-01 false Qualified family members. 436.121 Section 436.121... Coverage of the Categorically Needy § 436.121 Qualified family members. (a) Definition. A qualified family member is any member of a family, including pregnant women and children eligible for Medicaid under § 436...

  3. 42 CFR 436.121 - Qualified family members.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... 42 Public Health 4 2010-10-01 2010-10-01 false Qualified family members. 436.121 Section 436.121... Coverage of the Categorically Needy § 436.121 Qualified family members. (a) Definition. A qualified family member is any member of a family, including pregnant women and children eligible for Medicaid under § 436...

  4. 10 CFR 436.15 - Formatting cost data.

    Code of Federal Regulations, 2011 CFR

    2011-01-01

    ... Procedures for Life Cycle Cost Analyses § 436.15 Formatting cost data. In establishing cost data under §§ 436.16 and 436.17 and measuring cost effectiveness by the modes of analysis described by § 436.19 through... software referenced in the Life Cycle Cost Manual for the Federal Energy Management Program. ...

  5. Uranus and Neptune: internal heat flow

    NASA Astrophysics Data System (ADS)

    Hofstadter, M. D.; Simon, A. A.; Banfield, D. J.; Fortney, J. J.; Hayes, A. G., Jr.; Hedman, M.; Hospodarsky, G. B.; Mandt, K.; Showalter, G. M.; Soderlund, K. M.; Turtle, E. P.; Hofstadter, M. D.; Sayanagi, K. M.; Simon, A. A.; Banfield, D. J.; Fortney, J. J.; Hayes, A.; Hedman, M.; Hospodarsky, G. B.; Mandt, K.; Showalter, G. M.; Soderlund, K. M.; Turtle, E. P.; Nettelmann, N.; Scheibe, L.; Redmer, R.

    2017-12-01

    Uranus and Neptune offer unique possibilities to study the behavior of gas-ice-rock mixtures at high pressures, the formation of planets, planetary magnetic field generation [1], and planetary atmospheres. While Uranus and Neptune interior models have been constructed that satisfy some of the observational constraints, so far there are no physically motivated models that are consistent with all of them. Especially the observed intrinsic heat fluxes pose challenges [2]. Here I present the thermal boundary layer approach [3] to explain both the extraordinary low heat flux of Uranus and the high heat flux of Neptune, and discuss implications. In particular, current models suggest miscibility of ices with rocks at P>1 Mbar and super-solar ice-to-rock ratios, for Uranus an irradiated exoplanet-like evolution in equilibrium with the stellar incident flux, and fully convective deep interiors. The Figure illustrates such an ice giant interior model.[1] Soderlund K.M., Heimpel, M.H., King E.M. Aurnou J.M. (2013), Icarus 224, 97 [2] Guillot T. (2005), Annu. Rev. Earth Planet. Sci. 33, 493 [3] Nettelmann N., Wang K., Fortney J.J. et al (2016), Icarus 275, 107

  6. 40 CFR 436.381 - Specialized definitions.

    Code of Federal Regulations, 2014 CFR

    2014-07-01

    ... 40 Protection of Environment 30 2014-07-01 2014-07-01 false Specialized definitions. 436.381 Section 436.381 Protection of Environment ENVIRONMENTAL PROTECTION AGENCY (CONTINUED) EFFLUENT GUIDELINES AND STANDARDS (CONTINUED) MINERAL MINING AND PROCESSING POINT SOURCE CATEGORY Graphite Subcategory § 436.381 Specialized definitions. For the purpos...

  7. 40 CFR 436.381 - Specialized definitions.

    Code of Federal Regulations, 2013 CFR

    2013-07-01

    ... 40 Protection of Environment 31 2013-07-01 2013-07-01 false Specialized definitions. 436.381 Section 436.381 Protection of Environment ENVIRONMENTAL PROTECTION AGENCY (CONTINUED) EFFLUENT GUIDELINES AND STANDARDS (CONTINUED) MINERAL MINING AND PROCESSING POINT SOURCE CATEGORY Graphite Subcategory § 436.381 Specialized definitions. For the purpos...

  8. 43 CFR 4.436 - Reporter's fees.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... 43 Public Lands: Interior 1 2010-10-01 2010-10-01 false Reporter's fees. 4.436 Section 4.436 Public Lands: Interior Office of the Secretary of the Interior DEPARTMENT HEARINGS AND APPEALS PROCEDURES... Fact § 4.436 Reporter's fees. Reporter's fees shall be borne by the Bureau. ...

  9. The NEPTUNE Canada Seismograph Network

    NASA Astrophysics Data System (ADS)

    Rogers, G. C.; Meldrum, R.; Baldwin, R.; Rosenberger, A.; Mulder, T.

    2009-12-01

    NEPTUNE Canada is the world’s first large regional cable-linked, multi-disciplinary scientific seafloor observatory. In the fall of 2007 an 800 kilometer ring of powered fibre optic cable was laid on the seafloor over the northern part of the Juan de Fuca plate and connected to a shore facility near Port Alberni on Vancouver Island. Five nodes were attached to the cable in the early in the summer of 2009 paving the way for junction boxes and scientific instruments installed in the late summer and fall. The NEPTUNE Canada Seismograph Network will consist initially of four broadband and four short period seismic systems. In the summer of 2009, three broadband OBS packages were deployed forming a large triangle with apexes at ODP 1027 in mid plate and two sites on the continental slope, ODP 889 and Barkley Canyon. In summer 2010 an additional broadband package will be installed on the Endeavour segment of the Juan de Fuca Ridge, and four short period instruments will be installed nearby forming a small array, 6 km in maximum dimension, to record earthquake activity in the vicinity of the many multidisciplinary ridge experiments. The broadband systems comprise a broadband seismometer and strong motion accelerometer in a surficially buried spherical titanium case, with a current meter, hydrophone and differential pressure gauge deployed nearby. The short period systems will include 3-component corehole seismometers on long term loan from the Monterey Bay Aquarium Research Institute (MBARI). All systems will have backup capacity for modest cable outages. The NEPTUNE Canada Seismograph Network relies heavily on knowledge gained from the previous seismographs temporarily deployed in the region by MBARI and the University of Washington and will re-occupy the broadband site and three short period sites at the ridge. NEPTUNE Canada seismic data will be archived by, and available from, both the Geological Survey of Canada and IRIS.

  10. 42 CFR 436.124 - Newborn children.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... 42 Public Health 4 2010-10-01 2010-10-01 false Newborn children. 436.124 Section 436.124 Public... the Categorically Needy § 436.124 Newborn children. (a) The agency must provide Medicaid eligibility to a child born to a woman who has applied for, has been determined eligible and is receiving...

  11. 42 CFR 436.124 - Newborn children.

    Code of Federal Regulations, 2013 CFR

    2013-10-01

    ... 42 Public Health 4 2013-10-01 2013-10-01 false Newborn children. 436.124 Section 436.124 Public... the Categorically Needy § 436.124 Newborn children. (a) The agency must provide Medicaid eligibility to a child born to a woman who has applied for, has been determined eligible and is receiving...

  12. 42 CFR 436.124 - Newborn children.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... 42 Public Health 4 2011-10-01 2011-10-01 false Newborn children. 436.124 Section 436.124 Public... the Categorically Needy § 436.124 Newborn children. (a) The agency must provide Medicaid eligibility to a child born to a woman who has applied for, has been determined eligible and is receiving...

  13. 42 CFR 436.124 - Newborn children.

    Code of Federal Regulations, 2012 CFR

    2012-10-01

    ... 42 Public Health 4 2012-10-01 2012-10-01 false Newborn children. 436.124 Section 436.124 Public... the Categorically Needy § 436.124 Newborn children. (a) The agency must provide Medicaid eligibility to a child born to a woman who has applied for, has been determined eligible and is receiving...

  14. 42 CFR 436.124 - Newborn children.

    Code of Federal Regulations, 2014 CFR

    2014-10-01

    ... 42 Public Health 4 2014-10-01 2014-10-01 false Newborn children. 436.124 Section 436.124 Public... the Categorically Needy § 436.124 Newborn children. (a) The agency must provide Medicaid eligibility to a child born to a woman who has applied for, has been determined eligible and is receiving...

  15. 42 CFR 488.436 - Civil money penalties: Waiver of hearing, reduction of penalty amount.

    Code of Federal Regulations, 2012 CFR

    2012-10-01

    ... 42 Public Health 5 2012-10-01 2012-10-01 false Civil money penalties: Waiver of hearing, reduction of penalty amount. 488.436 Section 488.436 Public Health CENTERS FOR MEDICARE & MEDICAID SERVICES... the civil money penalty. (b) Reduction of penalty amount. (1) If the facility waives its right to a...

  16. 42 CFR 488.436 - Civil money penalties: Waiver of hearing, reduction of penalty amount.

    Code of Federal Regulations, 2014 CFR

    2014-10-01

    ... 42 Public Health 5 2014-10-01 2014-10-01 false Civil money penalties: Waiver of hearing, reduction of penalty amount. 488.436 Section 488.436 Public Health CENTERS FOR MEDICARE & MEDICAID SERVICES... the civil money penalty. (b) Reduction of penalty amount. (1) If the facility waives its right to a...

  17. 42 CFR 488.436 - Civil money penalties: Waiver of hearing, reduction of penalty amount.

    Code of Federal Regulations, 2013 CFR

    2013-10-01

    ... 42 Public Health 5 2013-10-01 2013-10-01 false Civil money penalties: Waiver of hearing, reduction of penalty amount. 488.436 Section 488.436 Public Health CENTERS FOR MEDICARE & MEDICAID SERVICES... the civil money penalty. (b) Reduction of penalty amount. (1) If the facility waives its right to a...

  18. Spitzer Space Telescope Mid-IR Light Curves of Neptune

    NASA Technical Reports Server (NTRS)

    Stauffer, John; Marley, Mark S.; Gizis, John E.; Rebull, Luisa; Carey, Sean J.; Krick, Jessica; Ingalls, James G.; Lowrance, Patrick; Glaccum, William; Kirkpatrick, J. Davy; hide

    2016-01-01

    We have used the Spitzer Space Telescope in 2016 February to obtain high cadence, high signal-to-noise, 17 hr duration light curves of Neptune at 3.6 and 4.5 microns. The light curve duration was chosen to correspond to the rotation period of Neptune. Both light curves are slowly varying with time, with full amplitudes of 1.1 mag at 3.6 microns and 0.6 mag at 4.5 microns. We have also extracted sparsely sampled 18 hr light curves of Neptune at W1 (3.4 microns) and W2 (4.6 microns) from the Wide-field Infrared Survey Explorer (WISE)/NEOWISE archive at six epochs in 2010-2015. These light curves all show similar shapes and amplitudes compared to the Spitzer light curves but with considerable variation from epoch to epoch. These amplitudes are much larger than those observed with Kepler/K2 in the visible (amplitude approximately 0.02 mag) or at 845 nm with the Hubble Space Telescope (HST) in 2015 and at 763 nm in 2016 (amplitude approximately 0.2 mag). We interpret the Spitzer and WISE light curves as arising entirely from reflected solar photons, from higher levels in Neptune's atmosphere than for K2. Methane gas is the dominant opacity source in Neptune's atmosphere, and methane absorption bands are present in the HST 763 and 845 nm, WISE W1, and Spitzer 3.6 micron filters.

  19. Neptune in False Color

    NASA Image and Video Library

    1996-01-29

    In this false color image of Neptune, objects that are deep in the atmosphere are blue, while those at higher altitudes are white. The image was taken by Voyager 2 wide-angle camera through an orange filter and two different methane filters. http://photojournal.jpl.nasa.gov/catalog/PIA00051

  20. 27 CFR 4.36 - Alcoholic content.

    Code of Federal Regulations, 2013 CFR

    2013-04-01

    ... 27 Alcohol, Tobacco Products and Firearms 1 2013-04-01 2013-04-01 false Alcoholic content. 4.36 Section 4.36 Alcohol, Tobacco Products and Firearms ALCOHOL AND TOBACCO TAX AND TRADE BUREAU, DEPARTMENT OF THE TREASURY ALCOHOL LABELING AND ADVERTISING OF WINE Labeling Requirements for Wine § 4.36 Alcoholic content. (a) Alcoholic content shall be...

  1. 27 CFR 4.36 - Alcoholic content.

    Code of Federal Regulations, 2014 CFR

    2014-04-01

    ... 27 Alcohol, Tobacco Products and Firearms 1 2014-04-01 2014-04-01 false Alcoholic content. 4.36 Section 4.36 Alcohol, Tobacco Products and Firearms ALCOHOL AND TOBACCO TAX AND TRADE BUREAU, DEPARTMENT OF THE TREASURY ALCOHOL LABELING AND ADVERTISING OF WINE Labeling Requirements for Wine § 4.36 Alcoholic content. (a) Alcoholic content shall be...

  2. 27 CFR 4.36 - Alcoholic content.

    Code of Federal Regulations, 2012 CFR

    2012-04-01

    ... 27 Alcohol, Tobacco Products and Firearms 1 2012-04-01 2012-04-01 false Alcoholic content. 4.36 Section 4.36 Alcohol, Tobacco Products and Firearms ALCOHOL AND TOBACCO TAX AND TRADE BUREAU, DEPARTMENT OF THE TREASURY LIQUORS LABELING AND ADVERTISING OF WINE Labeling Requirements for Wine § 4.36 Alcoholic content. (a) Alcoholic content shall be...

  3. 27 CFR 4.36 - Alcoholic content.

    Code of Federal Regulations, 2010 CFR

    2010-04-01

    ... 27 Alcohol, Tobacco Products and Firearms 1 2010-04-01 2010-04-01 false Alcoholic content. 4.36 Section 4.36 Alcohol, Tobacco Products and Firearms ALCOHOL AND TOBACCO TAX AND TRADE BUREAU, DEPARTMENT OF THE TREASURY LIQUORS LABELING AND ADVERTISING OF WINE Labeling Requirements for Wine § 4.36 Alcoholic content. (a) Alcoholic content shall be...

  4. 27 CFR 4.36 - Alcoholic content.

    Code of Federal Regulations, 2011 CFR

    2011-04-01

    ... 27 Alcohol, Tobacco Products and Firearms 1 2011-04-01 2011-04-01 false Alcoholic content. 4.36 Section 4.36 Alcohol, Tobacco Products and Firearms ALCOHOL AND TOBACCO TAX AND TRADE BUREAU, DEPARTMENT OF THE TREASURY LIQUORS LABELING AND ADVERTISING OF WINE Labeling Requirements for Wine § 4.36 Alcoholic content. (a) Alcoholic content shall be...

  5. NEPTUNE'S WILD DAYS: CONSTRAINTS FROM THE ECCENTRICITY DISTRIBUTION OF THE CLASSICAL KUIPER BELT

    DOE Office of Scientific and Technical Information (OSTI.GOV)

    Dawson, Rebekah I.; Murray-Clay, Ruth, E-mail: rdawson@cfa.harvard.edu

    2012-05-01

    Neptune's dynamical history shaped the current orbits of Kuiper Belt objects (KBOs), leaving clues to the planet's orbital evolution. In the 'classical' region, a population of dynamically 'hot' high-inclination KBOs overlies a flat 'cold' population with distinct physical properties. Simulations of qualitatively different histories for Neptune, including smooth migration on a circular orbit or scattering by other planets to a high eccentricity, have not simultaneously produced both populations. We explore a general Kuiper Belt assembly model that forms hot classical KBOs interior to Neptune and delivers them to the classical region, where the cold population forms in situ. First, wemore » present evidence that the cold population is confined to eccentricities well below the limit dictated by long-term survival. Therefore, Neptune must deliver hot KBOs into the long-term survival region without excessively exciting the eccentricities of the cold population. Imposing this constraint, we explore the parameter space of Neptune's eccentricity and eccentricity damping, migration, and apsidal precession. We rule out much of parameter space, except where Neptune is scattered to a moderately eccentric orbit (e > 0.15) and subsequently migrates a distance {Delta}a{sub N} = 1-6 AU. Neptune's moderate eccentricity must either damp quickly or be accompanied by fast apsidal precession. We find that Neptune's high eccentricity alone does not generate a chaotic sea in the classical region. Chaos can result from Neptune's interactions with Uranus, exciting the cold KBOs and placing additional constraints. Finally, we discuss how to interpret our constraints in the context of the full, complex dynamical history of the solar system.« less

  6. Stratospheric ethane on Neptune - Comparison of groundbased and Voyager IRIS retrievals

    NASA Technical Reports Server (NTRS)

    Kostiuk, Theodor; Romani, Paul; Espenak, Fred; Bezard, Bruno

    1992-01-01

    Near-simultaneous ground and spacecraft measurements of 12-micron ethane emission spectra during the Voyager encounter with Neptune have furnished bases for the determination of stratospheric ethane abundance and the testing and constraining of Neptune methane-photochemistry models. The ethane retrievals were sensitive to the thermal profile used. Contribution functions for warm thermal profiles peaked at higher altitudes, as expected, with the heterodyne functions covering lower-pressure regions. Both constant- and nonconstant-with-height profiles remain candidate distributions for Neptune's stratospheric ethane.

  7. Magnetostrophic balance in planetary dynamos - Predictions for Neptune's magnetosphere

    NASA Technical Reports Server (NTRS)

    Curtis, S. A.; Ness, N. F.

    1986-01-01

    With the purpose of estimating Neptune's magnetic field and its implications for nonthermal Neptune radio emissions, a new scaling law for planetary magnetic fields was developed in terms of externally observable parameters (the planet's mean density, radius, mass, rotation rate, and internal heat source luminosity). From a comparison of theory and observations by Voyager it was concluded that planetary dynamos are two-state systems with either zero intrinsic magnetic field (for planets with low internal heat source) or (for planets with the internal heat source sufficiently strong to drive convection) a magnetic field near the upper bound determined from magnetostrophic balance. It is noted that mass loading of the Neptune magnetosphere by Triton may play an important role in the generation of nonthermal radio emissions.

  8. Seasonal stratospheric photochemistry on Uranus and Neptune

    NASA Astrophysics Data System (ADS)

    Moses, Julianne I.; Fletcher, Leigh N.; Greathouse, Thomas K.; Orton, Glenn S.; Hue, Vincent

    2018-06-01

    A time-variable 1D photochemical model is used to study the distribution of stratospheric hydrocarbons as a function of altitude, latitude, and season on Uranus and Neptune. The results for Neptune indicate that in the absence of stratospheric circulation or other meridional transport processes, the hydrocarbon abundances exhibit strong seasonal and meridional variations in the upper stratosphere, but that these variations become increasingly damped with depth due to increasing dynamical and chemical time scales. At high altitudes, hydrocarbon mixing ratios are typically largest where the solar insolation is the greatest, leading to strong hemispheric dichotomies between the summer-to-fall hemisphere and winter-to-spring hemisphere. At mbar pressures and deeper, slower chemistry and diffusion lead to latitude variations that become more symmetric about the equator. On Uranus, the stagnant, poorly mixed stratosphere confines methane and its photochemical products to higher pressures, where chemistry and diffusion time scales remain large. Seasonal variations in hydrocarbons are therefore predicted to be more muted on Uranus, despite the planet's very large obliquity. Radiative-transfer simulations demonstrate that latitude variations in hydrocarbons on both planets are potentially observable with future JWST mid-infrared spectral imaging. Our seasonal model predictions for Neptune compare well with retrieved C2H2 and C2H6 abundances from spatially resolved ground-based observations (no such observations currently exist for Uranus), suggesting that stratospheric circulation - which was not included in these models - may have little influence on the large-scale meridional hydrocarbon distributions on Neptune, unlike the situation on Jupiter and Saturn.

  9. The vertical distribution and origin of HCN in Neptune's atmosphere

    NASA Technical Reports Server (NTRS)

    Lellouch, Emmanuel; Romani, Paul N.; Rosenqvist, Jan

    1994-01-01

    Measurements and modeling of the (3-2) rotational line of hydrogen cyanide at 265.9 GHz in Neptune's atmosphere are presented. High signal-to-noise observations provide information on the HCN vertical distribution in Neptune's stratosphere. The HCN mixing ratio is found to be nearly uniform with height above the condensation level. Best fits occur for HCN distributions that have a slight increase with altitude. A least-squares analysis yields a mixing ratio of (3.2 +/- 0.8)10(exp -10) at 2 mbar and a mean mixing ratio scale height of 250(sup 750)(sub -110) km in the 0.1-3 mbar region. To interpret these results, we developed a photochemical model of HCN. HCN formation is initiated by the reaction between CH3 radicals, produced from methane photochemistry, and N atoms. The primary sink for HCN is condensation, with minor contributions from photolysis and chemical losses. Two possible sources of N atoms are investigated: (1) infall of N escaped from Triton's upper atmosphere, and (2) galactic cosmic ray (GCR) impact on internal N2. Given the uncertainties on (i) the transport and possible ionization of N in Neptune's magnetosphere, and the fate of N(+) reaching Neptune's upper atmosphere and (ii) the N2 mixing ratio in Neptune's deep atmosphere, we suggest that both sources of N atoms may significantly contibute to the formation of HCN.

  10. 10 CFR 436.13 - Presuming cost-effectiveness results.

    Code of Federal Regulations, 2010 CFR

    2010-01-01

    ... Methodology and Procedures for Life Cycle Cost Analyses § 436.13 Presuming cost-effectiveness results. (a) If... life cycle cost-effective without further analysis. (b) A Federal agency may presume that an investment in an energy or water conservation measure retrofit to an existing Federal building is not life cycle...

  11. Featured Image: A New Dark Vortex on Neptune

    NASA Astrophysics Data System (ADS)

    Kohler, Susanna

    2018-03-01

    This remarkable series of images by the Hubble Space Telescope (click for the full view) track a dark vortex only the fifth ever observed on Neptune as it evolves in Neptunes atmosphere. These Hubble images, presented in a recent study led by Michael Wong (University of California, Berkeley), were taken in 2015 September, 2016 May, 2016 October, and 2017 October; the observations have monitored the evolution of the vortex as it has gradually weakened and drifted polewards. Confirmation of the vortex solved a puzzle that arose in 2015, when astronomers spotted an unexplained outburst of cloud activity on Neptune. This outburst was likely a group of bright companion clouds that form as air flows over high-pressure dark vortices, causing gases to freeze into methane ice crystals. To learn more about what the authors have since learned by studying this vortex, check out the paper below.CitationMichael H. Wong et al 2018 AJ 155 117. doi:10.3847/1538-3881/aaa6d6

  12. The Voyager Neptune travel guide

    NASA Technical Reports Server (NTRS)

    Kohlhase, Charles (Editor)

    1989-01-01

    The Voyager mission to the giant outer planets of our solar system is described. Scientific highlights include interplanetary cruise, Jupiter, Saturn, Uranus, and their vast satellite and ring systems. Detailed plans are provided for the August 1989 Neptune encounter and subsequent interstellar journey to reach the heliopause. As background, the elements of an unmanned space mission are explained, with emphasis on the capabilities of the spacecraft and the scientific sensors. Other topics include the Voyager Grand Tour trajectory design, deep-space navigation, and gravity-assist concepts. The Neptune flyby is animated through the use of computer-generated, flip-page movie frames that appear in the corners of the publication. Useful historical information is also presented, including facts associated with the Voyager mission. Finally, short summaries are provided to describe the major objectives and schedules for several space missions planned for the remainder of the 20th century.

  13. Direct Imaging of a Cold Jovian Exoplanet in Orbit around the Sun-Like Star GJ 504

    NASA Technical Reports Server (NTRS)

    Kuzuhara, M.; Tamura, M.; Kudo, T.; Janson, M; Kandori, R.; Brandt, T. D.; Thalmann, C.; Spiegel, D.; Biller, B.; Carson, J.; hide

    2013-01-01

    Several exoplanets have recently been imaged at wide separations of >10 AU from their parent stars. These span a limited range of ages (<50 Myr) and atmospheric properties, with temperatures of 800-1800 K and very red colors (J -H > 0.5 mag), implying thick cloud covers. Furthermore, substantial model uncertainties exist at these young ages due to the unknown initial conditions at formation, which can lead to an order of magnitude of uncertainty in the modeled planet mass. Here, we report the direct imaging discovery of a Jovian exoplanet around the Sun-like star GJ 504, detected as part of the SEEDS survey. The system is older than all other known directly-imaged planets; as a result, its estimated mass remains in the planetary regime independent of uncertainties related to choices of initial conditions in the exoplanet modeling. Using the most common exoplanet cooling model, and given the system age of 160(+350/-60) Myr, GJ 504 b has an estimated mass of 4(+4.5/-1.0) Jupiter masses, among the lowest of directly imaged planets. Its projected separation of 43.5 AU exceeds the typical outer boundary of approx.. 30 AU predicted for the core accretion mechanism. GJ 504 b is also significantly cooler (510(+30/-20) K)) and has a bluer color (J - H = -0.23 mag) than previously imaged exoplanets, suggesting a largely cloud-free atmosphere accessible to spectroscopic characterization. Thus, it has the potential of providing novel insights into the origins of giant planets, as well as their atmospheric properties.

  14. 42 CFR 436.510 - Determination of dependency.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... 42 Public Health 4 2011-10-01 2011-10-01 false Determination of dependency. 436.510 Section 436.510 Public Health CENTERS FOR MEDICARE & MEDICAID SERVICES, DEPARTMENT OF HEALTH AND HUMAN SERVICES... Requirements for Medicaid Eligibility Dependency § 436.510 Determination of dependency. For families with...

  15. 42 CFR 436.510 - Determination of dependency.

    Code of Federal Regulations, 2012 CFR

    2012-10-01

    ... 42 Public Health 4 2012-10-01 2012-10-01 false Determination of dependency. 436.510 Section 436.510 Public Health CENTERS FOR MEDICARE & MEDICAID SERVICES, DEPARTMENT OF HEALTH AND HUMAN SERVICES... Requirements for Medicaid Eligibility Dependency § 436.510 Determination of dependency. For families with...

  16. 42 CFR 436.510 - Determination of dependency.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... 42 Public Health 4 2010-10-01 2010-10-01 false Determination of dependency. 436.510 Section 436.510 Public Health CENTERS FOR MEDICARE & MEDICAID SERVICES, DEPARTMENT OF HEALTH AND HUMAN SERVICES... Requirements for Medicaid Eligibility Dependency § 436.510 Determination of dependency. For families with...

  17. 42 CFR 436.510 - Determination of dependency.

    Code of Federal Regulations, 2013 CFR

    2013-10-01

    ... 42 Public Health 4 2013-10-01 2013-10-01 false Determination of dependency. 436.510 Section 436.510 Public Health CENTERS FOR MEDICARE & MEDICAID SERVICES, DEPARTMENT OF HEALTH AND HUMAN SERVICES... Requirements for Medicaid Eligibility Dependency § 436.510 Determination of dependency. For families with...

  18. 42 CFR 436.510 - Determination of dependency.

    Code of Federal Regulations, 2014 CFR

    2014-10-01

    ... 42 Public Health 4 2014-10-01 2014-10-01 false Determination of dependency. 436.510 Section 436.510 Public Health CENTERS FOR MEDICARE & MEDICAID SERVICES, DEPARTMENT OF HEALTH AND HUMAN SERVICES... Requirements for Medicaid Eligibility Dependency § 436.510 Determination of dependency. For families with...

  19. 10 CFR 436.36 - Conditions of payment.

    Code of Federal Regulations, 2010 CFR

    2010-01-01

    ... baseline under the energy savings performance contract (adjusted if appropriate under § 436.37), multiplied... 10 Energy 3 2010-01-01 2010-01-01 false Conditions of payment. 436.36 Section 436.36 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS Methods and...

  20. 16 CFR 436.4 - Table of contents.

    Code of Federal Regulations, 2010 CFR

    2010-01-01

    ... 16 Commercial Practices 1 2010-01-01 2010-01-01 false Table of contents. 436.4 Section 436.4 Commercial Practices FEDERAL TRADE COMMISSION TRADE REGULATION RULES DISCLOSURE REQUIREMENTS AND PROHIBITIONS CONCERNING FRANCHISING Contents of a Disclosure Document § 436.4 Table of contents. Include the following...

  1. 10 CFR 436.37 - Annual energy audits.

    Code of Federal Regulations, 2012 CFR

    2012-01-01

    ... 10 Energy 3 2012-01-01 2012-01-01 false Annual energy audits. 436.37 Section 436.37 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS Methods and Procedures for Energy Savings Performance Contracting § 436.37 Annual energy audits. (a) After contractor...

  2. 10 CFR 436.37 - Annual energy audits.

    Code of Federal Regulations, 2014 CFR

    2014-01-01

    ... 10 Energy 3 2014-01-01 2014-01-01 false Annual energy audits. 436.37 Section 436.37 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS Methods and Procedures for Energy Savings Performance Contracting § 436.37 Annual energy audits. (a) After contractor...

  3. 10 CFR 436.37 - Annual energy audits.

    Code of Federal Regulations, 2013 CFR

    2013-01-01

    ... 10 Energy 3 2013-01-01 2013-01-01 false Annual energy audits. 436.37 Section 436.37 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS Methods and Procedures for Energy Savings Performance Contracting § 436.37 Annual energy audits. (a) After contractor...

  4. 10 CFR 436.37 - Annual energy audits.

    Code of Federal Regulations, 2011 CFR

    2011-01-01

    ... 10 Energy 3 2011-01-01 2011-01-01 false Annual energy audits. 436.37 Section 436.37 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS Methods and Procedures for Energy Savings Performance Contracting § 436.37 Annual energy audits. (a) After contractor...

  5. 10 CFR 436.37 - Annual energy audits.

    Code of Federal Regulations, 2010 CFR

    2010-01-01

    ... 10 Energy 3 2010-01-01 2010-01-01 false Annual energy audits. 436.37 Section 436.37 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS Methods and Procedures for Energy Savings Performance Contracting § 436.37 Annual energy audits. (a) After contractor...

  6. 42 CFR 436.300 - Scope.

    Code of Federal Regulations, 2014 CFR

    2014-10-01

    ... 42 Public Health 4 2014-10-01 2014-10-01 false Scope. 436.300 Section 436.300 Public Health CENTERS FOR MEDICARE & MEDICAID SERVICES, DEPARTMENT OF HEALTH AND HUMAN SERVICES (CONTINUED) MEDICAL ASSISTANCE PROGRAMS ELIGIBILITY IN GUAM, PUERTO RICO, AND THE VIRGIN ISLANDS Optional Coverage of the...

  7. 42 CFR 436.200 - Scope.

    Code of Federal Regulations, 2014 CFR

    2014-10-01

    ... 42 Public Health 4 2014-10-01 2014-10-01 false Scope. 436.200 Section 436.200 Public Health CENTERS FOR MEDICARE & MEDICAID SERVICES, DEPARTMENT OF HEALTH AND HUMAN SERVICES (CONTINUED) MEDICAL ASSISTANCE PROGRAMS ELIGIBILITY IN GUAM, PUERTO RICO, AND THE VIRGIN ISLANDS Options for Coverage as...

  8. 42 CFR 436.100 - Scope.

    Code of Federal Regulations, 2014 CFR

    2014-10-01

    ... 42 Public Health 4 2014-10-01 2014-10-01 false Scope. 436.100 Section 436.100 Public Health CENTERS FOR MEDICARE & MEDICAID SERVICES, DEPARTMENT OF HEALTH AND HUMAN SERVICES (CONTINUED) MEDICAL ASSISTANCE PROGRAMS ELIGIBILITY IN GUAM, PUERTO RICO, AND THE VIRGIN ISLANDS Mandatory Coverage of the...

  9. 42 CFR 436.330 - Coverage for certain aliens.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... 42 Public Health 4 2011-10-01 2011-10-01 false Coverage for certain aliens. 436.330 Section 436... Coverage of the Medically Needy § 436.330 Coverage for certain aliens. If an agency provides Medicaid to... condition, as defined in § 440.255(c) of this chapter to those aliens described in § 436.406(c) of this...

  10. 42 CFR 436.330 - Coverage for certain aliens.

    Code of Federal Regulations, 2013 CFR

    2013-10-01

    ... 42 Public Health 4 2013-10-01 2013-10-01 false Coverage for certain aliens. 436.330 Section 436... Coverage of the Medically Needy § 436.330 Coverage for certain aliens. If an agency provides Medicaid to... condition, as defined in § 440.255(c) of this chapter to those aliens described in § 436.406(c) of this...

  11. 42 CFR 436.330 - Coverage for certain aliens.

    Code of Federal Regulations, 2012 CFR

    2012-10-01

    ... 42 Public Health 4 2012-10-01 2012-10-01 false Coverage for certain aliens. 436.330 Section 436... Coverage of the Medically Needy § 436.330 Coverage for certain aliens. If an agency provides Medicaid to... condition, as defined in § 440.255(c) of this chapter to those aliens described in § 436.406(c) of this...

  12. 42 CFR 436.330 - Coverage for certain aliens.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... 42 Public Health 4 2010-10-01 2010-10-01 false Coverage for certain aliens. 436.330 Section 436... Coverage of the Medically Needy § 436.330 Coverage for certain aliens. If an agency provides Medicaid to... condition, as defined in § 440.255(c) of this chapter to those aliens described in § 436.406(c) of this...

  13. 42 CFR 436.330 - Coverage for certain aliens.

    Code of Federal Regulations, 2014 CFR

    2014-10-01

    ... 42 Public Health 4 2014-10-01 2014-10-01 false Coverage for certain aliens. 436.330 Section 436... Coverage of the Medically Needy § 436.330 Coverage for certain aliens. If an agency provides Medicaid to... condition, as defined in § 440.255(c) of this chapter to those aliens described in § 436.406(c) of this...

  14. 49 CFR 195.436 - Security of facilities.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... 49 Transportation 3 2011-10-01 2011-10-01 false Security of facilities. 195.436 Section 195.436... PIPELINE Operation and Maintenance § 195.436 Security of facilities. Each operator shall provide protection for each pumping station and breakout tank area and other exposed facility (such as scraper traps...

  15. 42 CFR 436.1002 - FFP for services.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... 42 Public Health 4 2011-10-01 2011-10-01 false FFP for services. 436.1002 Section 436.1002 Public Health CENTERS FOR MEDICARE & MEDICAID SERVICES, DEPARTMENT OF HEALTH AND HUMAN SERVICES (CONTINUED... Participation (FFP) Ffp for Expenditures for Determining Eligibility and Providing Services § 436.1002 FFP for...

  16. 42 CFR 436.1002 - FFP for services.

    Code of Federal Regulations, 2013 CFR

    2013-10-01

    ... 42 Public Health 4 2013-10-01 2013-10-01 false FFP for services. 436.1002 Section 436.1002 Public Health CENTERS FOR MEDICARE & MEDICAID SERVICES, DEPARTMENT OF HEALTH AND HUMAN SERVICES (CONTINUED... Participation (FFP) Ffp for Expenditures for Determining Eligibility and Providing Services § 436.1002 FFP for...

  17. 42 CFR 436.1002 - FFP for services.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... 42 Public Health 4 2010-10-01 2010-10-01 false FFP for services. 436.1002 Section 436.1002 Public Health CENTERS FOR MEDICARE & MEDICAID SERVICES, DEPARTMENT OF HEALTH AND HUMAN SERVICES (CONTINUED... Participation (FFP) Ffp for Expenditures for Determining Eligibility and Providing Services § 436.1002 FFP for...

  18. 42 CFR 436.1002 - FFP for services.

    Code of Federal Regulations, 2012 CFR

    2012-10-01

    ... 42 Public Health 4 2012-10-01 2012-10-01 false FFP for services. 436.1002 Section 436.1002 Public Health CENTERS FOR MEDICARE & MEDICAID SERVICES, DEPARTMENT OF HEALTH AND HUMAN SERVICES (CONTINUED... Participation (FFP) Ffp for Expenditures for Determining Eligibility and Providing Services § 436.1002 FFP for...

  19. 42 CFR 436.1002 - FFP for services.

    Code of Federal Regulations, 2014 CFR

    2014-10-01

    ... 42 Public Health 4 2014-10-01 2014-10-01 false FFP for services. 436.1002 Section 436.1002 Public Health CENTERS FOR MEDICARE & MEDICAID SERVICES, DEPARTMENT OF HEALTH AND HUMAN SERVICES (CONTINUED... Participation (FFP) Ffp for Expenditures for Determining Eligibility and Providing Services § 436.1002 FFP for...

  20. Hubble Finds New Dark Spot on Neptune

    NASA Technical Reports Server (NTRS)

    1995-01-01

    NASA's Hubble Space Telescope has discovered a new great dark spot, located in the northern hemisphere of the planet Neptune. Because the planet's northern hemisphere is now tilted away from Earth, the new feature appears near the limb of the planet.

    The spot is a near mirror-image to a similar southern hemisphere dark spot that was discovered in 1989 by the Voyager 2 probe. In 1994, Hubble showed that the southern dark spot had disappeared.

    Like its predecessor, the new spot has high altitude clouds along its edge, caused by gasses that have been pushed to higher altitudes where they cool to form methane ice crystal clouds. The dark spot may be a zone of clear gas that is a window to a cloud deck lower in the atmosphere.

    Planetary scientists don t know how long lived this new feature might be. Hubble's high resolution will allow astronomers to follow the spot's evolution and other unexpected changes in Neptune's dynamic atmosphere.

    The image was taken on November 2, 1994 with Hubble's Wide Field Planetary Camera 2, when Neptune was 2.8 billion miles (4.5 billion kilometers) from Earth. Hubble can resolve features as small as 625 miles (1,000 kilometers) across in Neptune's cloud tops.

    The Wide Field/Planetary Camera 2 was developed by the Jet Propulsion Laboratory and managed by the Goddard Spaced Flight Center for NASA's Office of Space Science.

    This image and other images and data received from the Hubble Space Telescope are posted on the World Wide Web on the Space Telescope Science Institute home page at URL http://oposite.stsci.edu/pubinfo/

  1. 10 CFR 436.32 - Qualified contractors lists.

    Code of Federal Regulations, 2010 CFR

    2010-01-01

    ... 10 Energy 3 2010-01-01 2010-01-01 false Qualified contractors lists. 436.32 Section 436.32 Energy... Procedures for Energy Savings Performance Contracting § 436.32 Qualified contractors lists. (a) DOE shall... energy savings performance contracts. (c) DOE may remove a firm from DOE's list of qualified contractors...

  2. THE GJ1214 SUPER-EARTH SYSTEM: STELLAR VARIABILITY, NEW TRANSITS, AND A SEARCH FOR ADDITIONAL PLANETS

    DOE Office of Scientific and Technical Information (OSTI.GOV)

    Berta, Zachory K.; Charbonneau, David; Bean, Jacob

    2011-07-20

    The super-Earth GJ1214b transits a nearby M dwarf that exhibits a 1% intrinsic variability in the near-infrared. Here, we analyze new observations to refine the physical properties of both the star and planet. We present three years of out-of-transit photometric monitoring of the stellar host GJ1214 from the MEarth Observatory and find the rotation period to be long, most likely an integer multiple of 53 days, suggesting low levels of magnetic activity and an old age for the system. We show that such variability will not pose significant problems to ongoing studies of the planet's atmosphere with transmission spectroscopy. Wemore » analyze two high-precision transit light curves from ESO's Very Large Telescope (VLT) along with seven others from the MEarth and Fred Lawrence Whipple Observatory 1.2 m telescopes, finding physical parameters for the planet that are consistent with previous work. The VLT light curves show tentative evidence for spot occultations during transit. Using two years of MEarth light curves, we place limits on additional transiting planets around GJ1214 with periods out to the habitable zone of the system. We also improve upon the previous photographic V-band estimate for the star, finding V = 14.71 {+-} 0.03.« less

  3. TWO PLANETARY COMPANIONS AROUND THE K7 DWARF GJ 221: A HOT SUPER-EARTH AND A CANDIDATE IN THE SUB-SATURN DESERT RANGE

    DOE Office of Scientific and Technical Information (OSTI.GOV)

    Arriagada, Pamela; Minniti, Dante; Anglada-Escude, Guillem

    2013-07-01

    We report two low-mass companions orbiting the nearby K7 dwarf GJ 221 that have emerged from reanalyzing 4.4 yr of publicly available HARPS spectra complemented with 2 years of high-precision Doppler measurements with Magellan/PFS. The HARPS measurements alone contain the clear signal of a low-mass companion with a period of 125 days and a minimum mass of 53.2 M{sub Circled-Plus} (GJ 221b), falling in a mass range where very few planet candidates have been found (sub-Saturn desert). The addition of 17 PFS observations allows the confident detection of a second low-mass companion (6.5 M{sub Circled-Plus }) in a hot orbitmore » (3.87 day period, GJ 221c). Spectroscopic and photometric calibrations suggest that GJ 221 is slightly depleted ([Fe/H] {approx} -0.1) compared to the Sun, so the presence of two low-mass companions in the system confirms the trend that slightly reduced stellar metallicity does not prevent the formation of planets in the super-Earth to sub-Saturn mass regime.« less

  4. 42 CFR 436.900 - Scope.

    Code of Federal Regulations, 2014 CFR

    2014-10-01

    ... 42 Public Health 4 2014-10-01 2014-10-01 false Scope. 436.900 Section 436.900 Public Health CENTERS FOR MEDICARE & MEDICAID SERVICES, DEPARTMENT OF HEALTH AND HUMAN SERVICES (CONTINUED) MEDICAL ASSISTANCE PROGRAMS ELIGIBILITY IN GUAM, PUERTO RICO, AND THE VIRGIN ISLANDS Eligibility in Guam, Puerto Rico...

  5. 42 CFR 436.900 - Scope.

    Code of Federal Regulations, 2013 CFR

    2013-10-01

    ... 42 Public Health 4 2013-10-01 2013-10-01 false Scope. 436.900 Section 436.900 Public Health CENTERS FOR MEDICARE & MEDICAID SERVICES, DEPARTMENT OF HEALTH AND HUMAN SERVICES (CONTINUED) MEDICAL ASSISTANCE PROGRAMS ELIGIBILITY IN GUAM, PUERTO RICO, AND THE VIRGIN ISLANDS Eligibility in Guam, Puerto Rico...

  6. 42 CFR 436.900 - Scope.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... 42 Public Health 4 2010-10-01 2010-10-01 false Scope. 436.900 Section 436.900 Public Health CENTERS FOR MEDICARE & MEDICAID SERVICES, DEPARTMENT OF HEALTH AND HUMAN SERVICES (CONTINUED) MEDICAL ASSISTANCE PROGRAMS ELIGIBILITY IN GUAM, PUERTO RICO, AND THE VIRGIN ISLANDS Eligibility in Guam, Puerto Rico...

  7. 42 CFR 436.900 - Scope.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... 42 Public Health 4 2011-10-01 2011-10-01 false Scope. 436.900 Section 436.900 Public Health CENTERS FOR MEDICARE & MEDICAID SERVICES, DEPARTMENT OF HEALTH AND HUMAN SERVICES (CONTINUED) MEDICAL ASSISTANCE PROGRAMS ELIGIBILITY IN GUAM, PUERTO RICO, AND THE VIRGIN ISLANDS Eligibility in Guam, Puerto Rico...

  8. 42 CFR 436.900 - Scope.

    Code of Federal Regulations, 2012 CFR

    2012-10-01

    ... 42 Public Health 4 2012-10-01 2012-10-01 false Scope. 436.900 Section 436.900 Public Health CENTERS FOR MEDICARE & MEDICAID SERVICES, DEPARTMENT OF HEALTH AND HUMAN SERVICES (CONTINUED) MEDICAL ASSISTANCE PROGRAMS ELIGIBILITY IN GUAM, PUERTO RICO, AND THE VIRGIN ISLANDS Eligibility in Guam, Puerto Rico...

  9. 10 CFR 436.10 - Purpose.

    Code of Federal Regulations, 2012 CFR

    2012-01-01

    ... effectiveness of energy conservation measures and water conservation measures, and for rank ordering life cycle... 10 Energy 3 2012-01-01 2012-01-01 false Purpose. 436.10 Section 436.10 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS Methodology and Procedures for Life...

  10. 10 CFR 436.10 - Purpose.

    Code of Federal Regulations, 2014 CFR

    2014-01-01

    ... effectiveness of energy conservation measures and water conservation measures, and for rank ordering life cycle... 10 Energy 3 2014-01-01 2014-01-01 false Purpose. 436.10 Section 436.10 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS Methodology and Procedures for Life...

  11. 10 CFR 436.10 - Purpose.

    Code of Federal Regulations, 2013 CFR

    2013-01-01

    ... effectiveness of energy conservation measures and water conservation measures, and for rank ordering life cycle... 10 Energy 3 2013-01-01 2013-01-01 false Purpose. 436.10 Section 436.10 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS Methodology and Procedures for Life...

  12. 10 CFR 436.10 - Purpose.

    Code of Federal Regulations, 2011 CFR

    2011-01-01

    ... effectiveness of energy conservation measures and water conservation measures, and for rank ordering life cycle... 10 Energy 3 2011-01-01 2011-01-01 false Purpose. 436.10 Section 436.10 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS Methodology and Procedures for Life...

  13. Neptune's inner magnetosphere and aurora: Energetic particle constraints

    NASA Technical Reports Server (NTRS)

    Mauk, B. H.; Krimigis, S. M.; Acuna, M. H.

    1994-01-01

    A dramatic and peculiar dropout of greater than 500-keV ions (but not electrons) was observed within Neptune's inner magnetosphere near 2 R(sub N) as the Voyager 2 spacecraft approached the planet. Unlike a number of other energetic particle features this feature could not be accounted for by known material bodies in the context of the most utilized magnetic field models (neither the offset tilted dipole models nor the spehrical harmonic model 'O8'). However, the configuration of Neptune's inner magnetosphere is highly uncertain. By applying a novel technique, utilizing energetic particle measurements, to constrain the magnetic field configuration of the inner regions, we show that appeals to unobserved materials within Neptune's system are unnecessary, and that the ion dropout feature was, in all likelihood, the result of ion interactions with maximum L excursions of the ring 1989N1R. The constraints also favor the se of the M2 magnetic field model (Selesnick, 1992) over the previous models. An electron feature was probably absent because the electron interactions with the ring occurred substantially before the ion interactions (about 2 hours for the electrons versus a few minutes for the ions). Pitch-angle scattering apparently eliminated the electron signature. Minimum scattering rates determined based on this premise yield enough electron precipitation power to explain the brightest component of Neptune's aurora. We propose that this bright component is analogous to the Earth's diffuse aurora.

  14. 10 CFR 436.19 - Life cycle costs.

    Code of Federal Regulations, 2011 CFR

    2011-01-01

    ... 10 Energy 3 2011-01-01 2011-01-01 false Life cycle costs. 436.19 Section 436.19 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS Methodology and Procedures for Life Cycle Cost Analyses § 436.19 Life cycle costs. Life cycle costs are the sum of the...

  15. 10 CFR 436.19 - Life cycle costs.

    Code of Federal Regulations, 2010 CFR

    2010-01-01

    ... 10 Energy 3 2010-01-01 2010-01-01 false Life cycle costs. 436.19 Section 436.19 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS Methodology and Procedures for Life Cycle Cost Analyses § 436.19 Life cycle costs. Life cycle costs are the sum of the...

  16. 46 CFR 154.436 - Design vapor pressure.

    Code of Federal Regulations, 2013 CFR

    2013-10-01

    ... 46 Shipping 5 2013-10-01 2013-10-01 false Design vapor pressure. 154.436 Section 154.436 Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY (CONTINUED) CERTAIN BULK DANGEROUS CARGOES SAFETY STANDARDS FOR SELF-PROPELLED VESSELS CARRYING BULK LIQUEFIED GASES Design, Construction and Equipment Semi-Membrane Tanks § 154.436 Design vapor pressure....

  17. 46 CFR 154.436 - Design vapor pressure.

    Code of Federal Regulations, 2014 CFR

    2014-10-01

    ... 46 Shipping 5 2014-10-01 2014-10-01 false Design vapor pressure. 154.436 Section 154.436 Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY (CONTINUED) CERTAIN BULK DANGEROUS CARGOES SAFETY STANDARDS FOR SELF-PROPELLED VESSELS CARRYING BULK LIQUEFIED GASES Design, Construction and Equipment Semi-Membrane Tanks § 154.436 Design vapor pressure....

  18. 46 CFR 154.436 - Design vapor pressure.

    Code of Federal Regulations, 2012 CFR

    2012-10-01

    ... 46 Shipping 5 2012-10-01 2012-10-01 false Design vapor pressure. 154.436 Section 154.436 Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY (CONTINUED) CERTAIN BULK DANGEROUS CARGOES SAFETY STANDARDS FOR SELF-PROPELLED VESSELS CARRYING BULK LIQUEFIED GASES Design, Construction and Equipment Semi-Membrane Tanks § 154.436 Design vapor pressure....

  19. Latest Developments in the Installation Planning for Stage 1, NEPTUNE Regional Cabled Observatory, Northeast Pacific

    NASA Astrophysics Data System (ADS)

    Barnes, C. R.

    2004-12-01

    for the Wet Plant (cable/nodes) with a contract to be signed in Spring 2005, deployment in 2007 and most sensors deployed in 2008; b) arranging three Ocean Observing Systems workshops in 2004 to establish the community experiments, the desired observing systems, and the preferred node locations, c) initial planning for the Data Management and Archiving System (DMAS), and d) establishing MOUs with partner agencies including NSF/ORION, HIA/NRC, and DND. UVic also acts as the lead for the VENUS Project (www.venus.uvic.ca): a shallow-water, coastal observatory in southern BC whose installation has been funded for 2002-06. Over 60km of cable will be divided into three lines: Saanich Inlet (anoxic fiord), across the Strait of Georgia (from Fraser River delta), and across the Strait of Juan de Fuca (active circulation with Pacific Ocean). VENUS and Stage 1 of NEPTUNE will thus form a linked coastal/regional ocean observatory system. NEPTUNE North and VENUS will be among the first of many such cabled ocean observatories.

  20. 46 CFR 154.436 - Design vapor pressure.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... 46 Shipping 5 2010-10-01 2010-10-01 false Design vapor pressure. 154.436 Section 154.436 Shipping... FOR SELF-PROPELLED VESSELS CARRYING BULK LIQUEFIED GASES Design, Construction and Equipment Semi-Membrane Tanks § 154.436 Design vapor pressure. The Po of a semi-membrane tank must not exceed 24.5 kPa...

  1. 42 CFR 436.522 - Determination of age.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... 42 Public Health 4 2011-10-01 2011-10-01 false Determination of age. 436.522 Section 436.522... Requirements for Medicaid Eligibility Age § 436.522 Determination of age. (a) In determining age, the agency must use the common law method (under which an age is reached the day before the anniversary of birth...

  2. 42 CFR 436.522 - Determination of age.

    Code of Federal Regulations, 2014 CFR

    2014-10-01

    ... 42 Public Health 4 2014-10-01 2014-10-01 false Determination of age. 436.522 Section 436.522... Requirements for Medicaid Eligibility Age § 436.522 Determination of age. (a) In determining age, the agency must use the common law method (under which an age is reached the day before the anniversary of birth...

  3. 42 CFR 436.522 - Determination of age.

    Code of Federal Regulations, 2013 CFR

    2013-10-01

    ... 42 Public Health 4 2013-10-01 2013-10-01 false Determination of age. 436.522 Section 436.522... Requirements for Medicaid Eligibility Age § 436.522 Determination of age. (a) In determining age, the agency must use the common law method (under which an age is reached the day before the anniversary of birth...

  4. 42 CFR 436.522 - Determination of age.

    Code of Federal Regulations, 2012 CFR

    2012-10-01

    ... 42 Public Health 4 2012-10-01 2012-10-01 false Determination of age. 436.522 Section 436.522... Requirements for Medicaid Eligibility Age § 436.522 Determination of age. (a) In determining age, the agency must use the common law method (under which an age is reached the day before the anniversary of birth...

  5. 42 CFR 436.522 - Determination of age.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... 42 Public Health 4 2010-10-01 2010-10-01 false Determination of age. 436.522 Section 436.522... Requirements for Medicaid Eligibility Age § 436.522 Determination of age. (a) In determining age, the agency must use the common law method (under which an age is reached the day before the anniversary of birth...

  6. 10 CFR 436.31 - Definitions.

    Code of Federal Regulations, 2014 CFR

    2014-01-01

    ... locations. Energy unit savings means the determination, in electrical or thermal units (e.g., kilowatt hour (kwh), kilowatt (kw), or British thermal units (Btu)), of the reduction in energy use or demand by... 10 Energy 3 2014-01-01 2014-01-01 false Definitions. 436.31 Section 436.31 Energy DEPARTMENT OF...

  7. 10 CFR 436.31 - Definitions.

    Code of Federal Regulations, 2013 CFR

    2013-01-01

    ... locations. Energy unit savings means the determination, in electrical or thermal units (e.g., kilowatt hour (kwh), kilowatt (kw), or British thermal units (Btu)), of the reduction in energy use or demand by... 10 Energy 3 2013-01-01 2013-01-01 false Definitions. 436.31 Section 436.31 Energy DEPARTMENT OF...

  8. 10 CFR 436.31 - Definitions.

    Code of Federal Regulations, 2012 CFR

    2012-01-01

    ... locations. Energy unit savings means the determination, in electrical or thermal units (e.g., kilowatt hour (kwh), kilowatt (kw), or British thermal units (Btu)), of the reduction in energy use or demand by... 10 Energy 3 2012-01-01 2012-01-01 false Definitions. 436.31 Section 436.31 Energy DEPARTMENT OF...

  9. 10 CFR 436.107 - Review of plan.

    Code of Federal Regulations, 2010 CFR

    2010-01-01

    ... Operations Plans § 436.107 Review of plan. (a) Each plan or revision of a plan shall be submitted to DOE and... general operations plan under the guidelines will be evaluated with respect to: (1) Adequacy of... 10 Energy 3 2010-01-01 2010-01-01 false Review of plan. 436.107 Section 436.107 Energy DEPARTMENT...

  10. Lande gJ factors for even-parity electronic levels in the holmium atom

    NASA Astrophysics Data System (ADS)

    Stefanska, D.; Werbowy, S.; Krzykowski, A.; Furmann, B.

    2018-05-01

    In this work the hyperfine structure of the Zeeman splitting for 18 even-parity levels in the holmium atom was investigated. The experimental method applied was laser induced fluorescence in a hollow cathode discharge lamp. 20 spectral lines were investigated involving odd-parity levels from the ground multiplet, for which Lande gJ factors are known with high precision, as the lower levels; this greatly facilitated the evaluation of gJ factors for the upper levels. The gJ values for the even-parity levels considered are reported for the first time. They proved to compare fairly well with the values obtained recently in a semi-empirical analysis for the even-parity level system of Ho I.

  11. How to Make a Helium Atmosphere

    NASA Image and Video Library

    2015-06-11

    This diagram illustrates how hypothetical helium atmospheres might form. These would be on planets about the mass of Neptune, or smaller, which orbit tightly to their stars, whipping around in just days. They are thought to have cores of water or rock, surrounded by thick atmospheres of gas. Radiation from their nearby stars would boil off hydrogen and helium, but because hydrogen is lighter, more hydrogen would escape. It's also possible that planetary bodies, such as asteroids, could impact the planet, sending hydrogen out into space. Over time, the atmospheres would become enriched in helium. With less hydrogen in the planets' atmospheres, the concentration of methane and water would go down. Both water and methane consist in part of hydrogen. Eventually, billions of years later (a "Gyr" equals one billion years), the abundances of the water and methane would be greatly reduced. Since hydrogen would not be abundant, the carbon would be forced to pair with oxygen, forming carbon monoxide. NASA's Spitzer Space Telescope observed a proposed helium planet, GJ 436b, with these traits: it lacks methane, and appears to contain carbon monoxide. Future observations are needed to detect helium itself in the atmospheres of these planets, and confirm this theory. http://photojournal.jpl.nasa.gov/catalog/PIA19345

  12. JUPITER WILL BECOME A HOT JUPITER: CONSEQUENCES OF POST-MAIN-SEQUENCE STELLAR EVOLUTION ON GAS GIANT PLANETS

    DOE Office of Scientific and Technical Information (OSTI.GOV)

    Spiegel, David S.; Madhusudhan, Nikku, E-mail: dave@ias.edu, E-mail: Nikku.Madhusudhan@yale.edu

    When the Sun ascends the red giant branch (RGB), its luminosity will increase and all the planets will receive much greater irradiation than they do now. Jupiter, in particular, might end up more highly irradiated than the hot Neptune GJ 436b and, hence, could appropriately be termed a 'hot Jupiter'. When their stars go through the RGB or asymptotic giant branch stages, many of the currently known Jupiter-mass planets in several-AU orbits will receive levels of irradiation comparable to the hot Jupiters, which will transiently increase their atmospheric temperatures to {approx}1000 K or more. Furthermore, massive planets around post-main-sequence starsmore » could accrete a non-negligible amount of material from the enhanced stellar winds, thereby significantly altering their atmospheric chemistry as well as causing a significant accretion luminosity during the epochs of most intense stellar mass loss. Future generations of infrared observatories might be able to probe the thermal and chemical structure of such hot Jupiters' atmospheres. Finally, we argue that, unlike their main-sequence analogs (whose zonal winds are thought to be organized in only a few broad, planetary-scale jets), red-giant hot Jupiters should have multiple, narrow jets of zonal winds and efficient day-night redistribution.« less

  13. 10 CFR 436.19 - Life cycle costs.

    Code of Federal Regulations, 2014 CFR

    2014-01-01

    ... 10 Energy 3 2014-01-01 2014-01-01 false Life cycle costs. 436.19 Section 436.19 Energy DEPARTMENT... Procedures for Life Cycle Cost Analyses § 436.19 Life cycle costs. Life cycle costs are the sum of the... (d) Energy and/or water costs. [55 FR 48220, Nov. 20, 1990, as amended at 61 FR 32651, June 25, 1996] ...

  14. 10 CFR 436.19 - Life cycle costs.

    Code of Federal Regulations, 2013 CFR

    2013-01-01

    ... 10 Energy 3 2013-01-01 2013-01-01 false Life cycle costs. 436.19 Section 436.19 Energy DEPARTMENT... Procedures for Life Cycle Cost Analyses § 436.19 Life cycle costs. Life cycle costs are the sum of the... (d) Energy and/or water costs. [55 FR 48220, Nov. 20, 1990, as amended at 61 FR 32651, June 25, 1996] ...

  15. 10 CFR 436.19 - Life cycle costs.

    Code of Federal Regulations, 2012 CFR

    2012-01-01

    ... 10 Energy 3 2012-01-01 2012-01-01 false Life cycle costs. 436.19 Section 436.19 Energy DEPARTMENT... Procedures for Life Cycle Cost Analyses § 436.19 Life cycle costs. Life cycle costs are the sum of the... (d) Energy and/or water costs. [55 FR 48220, Nov. 20, 1990, as amended at 61 FR 32651, June 25, 1996] ...

  16. Structure of scintillations in Neptune's occultation shadow

    NASA Technical Reports Server (NTRS)

    Hubbard, W. B.; Lellouch, Emmanuel; Sicardy, Bruno; Brahic, Andre; Vilas, Faith

    1988-01-01

    An exceptionally high-quality data set from a Neptune occultation is used here to derive a number of new results about the statistical properties of the fluctuations of the intensity distribution in various parts of Neptune's occultation shadow. An approximate numerical ray-tracing model which successfully accounts for many of the qualitative aspects of the observed intensity fluctuation distribution is introduced. Strong refractive scintillation is simulated by including the effects of 'turbulence' with projected atmospheric properties allowed to vary in both the direction perpendicular and parallel to the limb, and an explicit two-dimensional picture of a typical intensity distribution throughout an occulting planet's shadow is presented. The results confirm the existence of highly anisotropic turbulence.

  17. Voyager 2 at Neptune - Imaging science results

    NASA Technical Reports Server (NTRS)

    Smith, B. A.; Soderblom, L. A.; Banfield, D.; Barnet, C.; Beebe, R. F.; Bazilevskii, A. T.; Bollinger, K.; Boyce, J. M.; Briggs, G. A.; Brahic, A.

    1989-01-01

    Neptune's atmosphere is revealed by Voyager 2 images to contain clouds of methane ice above a lower deck of hydrogen sulfide or ammonia ices, and to be dominated by an anticyclonic storm system designated the 'Great Dark Spot'; this bears both similarities and differences to the Great Red Spot of Jupiter. Like the rings of Uranus, those of Neptune are composed of very dark, but in addition very dusty, material. Six new regular satellites have been discovered whose radii range from 25 to 200 km. Triton is noted to be a differentiated body showing evidence of early surface-melting episodes. At least two active plumes are found on Triton, which may be driven by solar heating.

  18. Joint Radioisotope Electric Propulsion Studies - Neptune System Explorer

    NASA Technical Reports Server (NTRS)

    Khan, M. Omair; Amini, Rashied; Ervin, Joan; Lang, Jared; Landau, Damon; Oleson, Steven; Spilker, Thomas; Strange, Nathan

    2011-01-01

    The Neptune System Explorer (NSE) mission concept study assessed opportunities to conduct Cassini-like science at Neptune with a radioisotope electric propulsion (REP) based spacecraft. REP is based on powering an electric propulsion (EP) engine with a radioisotope power source (RPS). The NSE study was commissioned under the Joint Radioisotope Electric Propulsion Studies (JREPS) project, which sought to determine the technical feasibility of flagship class REP applications. Within JREPS, special emphasis was given toward identifying tall technology tent poles, as well as recommending any new RPS technology developments that would be required for complicated REP missions. Based on the goals of JREPS, multiple RPS (e.g. thermoelectric and Stirling based RPS) and EP (e.g. Hall and ion engines) technology combinations were traded during the NSE study to determine the most favorable REP design architecture. Among the findings from the study was the need for >400We RPS systems, which was driven by EP operating powers and the requirement for a long-lived mission in the deep solar system. Additionally multiple development and implementation risks were identified for the NSE concept, as well as REP missions in general. Among the strengths of the NSE mission would be the benefits associated with RPS and EP use, such as long-term power (approx. 2-3kW) at Neptune and flexible trajectory options for achieving orbit or tours of the Neptune system. Although there are still multiple issues to mitigate, the NSE concept demonstrated distinct advantages associated with using REP for deep space flagship-class missions.

  19. A Neptune Trojan Survey for the New Horizons Spacecraft

    NASA Astrophysics Data System (ADS)

    Sheppard, Scott

    2010-06-01

    Trojan asteroids share a planet's semi-major axis but lead (L4) or follow (L5) the planet by about 60 degrees near the two triangular Lagrangian points of equilibrium. These minor planets were likely captured in these locations around the planet formation epoch and thus their current dynamical and physical properties will help constrain the formation, evolution and migration of the planets. The Neptune Trojans currently consist of only six known objects, all in the leading L4 cloud. Three of these were discovered in our initial survey of the L4 region allowing us to determine that Neptune was likely on a much more eccentric orbit in the distant past. We propose to continue a survey for Neptune Trojans in the trailing L5 region and to recover promising candidates found in 2009A with Subaru. Only with knowledge of the Trojan numbers and orbits in both the L4 and L5 clouds will we be able to understand their formation and evolution and further constrain planet accretion and migration. In addition, the New Horizons spacecraft will pass through the Neptune L5 region in 2013 on its way to Pluto. It is important that we understand the possible dust production produced by collisions of the Trojans as well as find suitable Trojans that New Horizons will observe as it passes through the area.

  20. Resonant Transneptunian Binaries: Evidence for Slow Migration of Neptune

    NASA Technical Reports Server (NTRS)

    Noll, Keith S.; Grundy, W. M.; Schlichting, H. E.; Murray-Clay, R. A.; Benecchi, S. B.

    2012-01-01

    As Neptune migrated, its mean-motion resonances preceded it into the planetesimal disk. The efficiency of capture into mean motion resonances depends on the smoothness of Neptune's migration and the local population available to be captured. The two strongest resonances, the 3:2 at 39.4 AU and 2:1 at 47.7 AU, straddle the core repository of the physically distinct and binary-rich Cold Classicals, providing a unique opportunity to test the details of Neptune's migration. Smooth migration should result in a measurable difference between the 3:2 and 2:1 resonant object properties, with low inclination 2:1s having a high fraction of red binaries, mirroring that of the Cold Classicals while the 3:2 will would have fewer binaries. Rapid migration would generate a more homogeneous result. Resonant objects observed with HST show a higher rate of binaries in the 2:1 relative to the 3:2, significant at the 2cr level. This suggests slow Neptune migration over a large enough distance that the 2:1 swept through the Cold Classical region. Colors are available for only a fraction of these targets but a prevalence of red objects in outer Resonances has been reported. We report here on ongoing observations with HST in cycle 19 targeting all unobserved Resonants with observations that will measure color and search for binary companions using the WFC3.

  1. A High Mass & Low Envelope Fraction for the Warm Neptune K2-55b

    NASA Astrophysics Data System (ADS)

    Dressing, Courtney; Sinukoff, Evan; Fulton, Benjamin; Lopez, Eric; Beichman, Charles; Howard, Andrew; Knutson, Heather; Werner, Michael; Schlieder, Joshua; Benneke, Björn; Crossfield, Ian; Isaacson, Howard; Krick, Jessica; Gorjian, Varoujan; Livingston, John; Petigura, Erik; Akeson, Rachel; Batygin, Konstantin; Christiansen, Jessie; Ciardi, David; Crepp, Justin; Jasmine Gonzales, Erica; Hardegree-Ullman, Kevin; Hirsch, Lea; Kosiarek, Molly; Weiss, Lauren

    2018-01-01

    The NASA K2 mission is using the Kepler spacecraft to search for transiting planets in multiple fields along the ecliptic plane. One of the planets detected by K2 is K2-55b, a warm Neptune in a short-period orbit (2.8 days) around a late K dwarf. We previously obtained near-infrared spectra from IRTF/SpeX to characterize the system and found that the host star K2-55 has a radius of 0.715 (+0.043/-0.040) solar radii, a mass of 0.668 (+/- 0.069) solar masses, and an effective temperature of 4300K (+100/-107). We then combined our updated stellar properties with new fits to the K2 photometry to estimate a planet radius of 4.38 (+0.29/-0.25) Earth radii, confirmed the transit ephemeris using Spitzer/IRAC (GO 11026, PI Werner), and embarked on radial velocity observations with Keck/HIRES to measure the planet mass. Our RV data suggest that K2-55b is much more massive than expected, indicating that the planet has a high density despite having a relatively high mass. The lack of a significant volatile envelope tests current theories of gas giant formation and indicates that K2-55b may have avoided runaway accretion by migration, delayed formation, or inefficient core accretion. We gratefully acknowledge funding from the NASA Sagan Fellowship Program and the NASA K2 Guest Observer Program. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech.

  2. No evidence of rings around Neptune

    NASA Technical Reports Server (NTRS)

    Elliot, J. L.; Mink, D. J.; Baron, R. L.; Dunham, E.; Pingree, J. E.; French, R. G.; Elias, J. H.; Liller, W.; Nicholson, P. D.; Jones, T. J.

    1981-01-01

    The results of two observations of stellar occultations of Neptune to determine if the planet has a ring system are reported. The sightings were made from Mt. Stromlo, Mauna Kea, and Cerro Tololo, noting that an equatorial ring would subtend only two arcsec of view. An upper accretion limit was defined to set the region around Neptune where rings, rather than satellites, could form. The intensities of the starlight from the two selected stars were recorded by photometers on magnetic tape during the occultation period. One of the stars did not occult, but passed through the entire region where a ring system might be present. No definitive evidence for rings was found, although an optical depth for a Neptunian ring was calculated at 0.07, with a width of more than 5 km and a radius of 31,400 km.

  3. Neptune's small dark spot (D2)

    NASA Technical Reports Server (NTRS)

    1999-01-01

    This bulls-eye view of Neptune's small dark spot (D2) was obtained by Voyager 2's narrow-angle camera. Banding surrounding the feature indicates unseen strong winds, while structures within the bright spot suggest both active upwelling of clouds and rotation about the center. A rotation rate has not yet been measured, but the V-shaped structure near the right edge of the bright area indicates that the spot rotates clockwise. Unlike the Great Red Spot on Jupiter, which rotates counterclockwise, if the D2 spot on Neptune rotates clockwise, the material will be descending in the dark oval region. The fact that infrared data will yield temperature information about the region above the clouds makes this observation especially valuable. The Voyager Mission is conducted by JPL for NASA's Office of Space Science and Applications.

  4. Dynamics of a satellite and normalization around lagrangian points in the Neptune-Triton system

    NASA Astrophysics Data System (ADS)

    Yokoyama, T.; Stuchi, T. J.; Solórzano, C. R. H.; Corria, A. A.; Prado, A. F. B.; Winter, O. C.; Winter, S. M. G.; Sanchez, D. M.

    Since a mission to Pluto-Charon is in progress a similar mission to Neptune-Triton system probably is just a matter of time Besides the interesting items listed in the Hammel s proposal to explore Neptune Hammel et al 2002 there are others very interesting points Triton is a very large satellite with M T M N approx 2 09 times 10 -4 where M T and M N are the masses of Triton and Neptune respectively Its current inclination with respect to Neptune s equator is about 157 345 0 This unusual high and retrograde inclination for a very large inner satellite makes this problem unique in our solar system Hammel et al 2002 also propose that a top priority in this mission should be a Neptune-Triton orbiter not just a flyby tour Therefore assuming a massless spacecraft orbiting Neptune-Triton system basically the system can be stated in terms of the classical restricted three body problem The new ingredient is the Neptune oblateness and the retrograde motion of Triton With some slight displacements the lagrangian equilibria points still exist as well as many of the properties of the classical problem In this work we first give an extensive numerical exploration in the case when the spacecraft orbits Triton considering Sun Neptune and its oblateness as disturbers In the plane bf a times bf I where bf a is the semi major axis and bf I is the inclination of the orbiter we give a plot of the stable regions where the massless can survive for thousand of years Retrograde and direct inclinations were

  5. 40 CFR 436.381 - Specialized definitions.

    Code of Federal Regulations, 2012 CFR

    2012-07-01

    ... 40 Protection of Environment 31 2012-07-01 2012-07-01 false Specialized definitions. 436.381 Section 436.381 Protection of Environment ENVIRONMENTAL PROTECTION AGENCY (CONTINUED) EFFLUENT GUIDELINES AND STANDARDS (CONTINUED) MINERAL MINING AND PROCESSING POINT SOURCE CATEGORY Graphite Subcategory...

  6. 40 CFR 436.181 - Specialized definitions.

    Code of Federal Regulations, 2013 CFR

    2013-07-01

    ... 40 Protection of Environment 31 2013-07-01 2013-07-01 false Specialized definitions. 436.181 Section 436.181 Protection of Environment ENVIRONMENTAL PROTECTION AGENCY (CONTINUED) EFFLUENT GUIDELINES AND STANDARDS (CONTINUED) MINERAL MINING AND PROCESSING POINT SOURCE CATEGORY Phosphate Rock...

  7. 40 CFR 436.181 - Specialized definitions.

    Code of Federal Regulations, 2012 CFR

    2012-07-01

    ... 40 Protection of Environment 31 2012-07-01 2012-07-01 false Specialized definitions. 436.181 Section 436.181 Protection of Environment ENVIRONMENTAL PROTECTION AGENCY (CONTINUED) EFFLUENT GUIDELINES AND STANDARDS (CONTINUED) MINERAL MINING AND PROCESSING POINT SOURCE CATEGORY Phosphate Rock...

  8. 40 CFR 436.181 - Specialized definitions.

    Code of Federal Regulations, 2014 CFR

    2014-07-01

    ... 40 Protection of Environment 30 2014-07-01 2014-07-01 false Specialized definitions. 436.181 Section 436.181 Protection of Environment ENVIRONMENTAL PROTECTION AGENCY (CONTINUED) EFFLUENT GUIDELINES AND STANDARDS (CONTINUED) MINERAL MINING AND PROCESSING POINT SOURCE CATEGORY Phosphate Rock...

  9. 40 CFR 436.241 - Specialized definitions.

    Code of Federal Regulations, 2013 CFR

    2013-07-01

    ... 40 Protection of Environment 31 2013-07-01 2013-07-01 false Specialized definitions. 436.241 Section 436.241 Protection of Environment ENVIRONMENTAL PROTECTION AGENCY (CONTINUED) EFFLUENT GUIDELINES AND STANDARDS (CONTINUED) MINERAL MINING AND PROCESSING POINT SOURCE CATEGORY Diatomite Subcategory...

  10. 40 CFR 436.241 - Specialized definitions.

    Code of Federal Regulations, 2012 CFR

    2012-07-01

    ... 40 Protection of Environment 31 2012-07-01 2012-07-01 false Specialized definitions. 436.241 Section 436.241 Protection of Environment ENVIRONMENTAL PROTECTION AGENCY (CONTINUED) EFFLUENT GUIDELINES AND STANDARDS (CONTINUED) MINERAL MINING AND PROCESSING POINT SOURCE CATEGORY Diatomite Subcategory...

  11. 40 CFR 436.241 - Specialized definitions.

    Code of Federal Regulations, 2014 CFR

    2014-07-01

    ... 40 Protection of Environment 30 2014-07-01 2014-07-01 false Specialized definitions. 436.241 Section 436.241 Protection of Environment ENVIRONMENTAL PROTECTION AGENCY (CONTINUED) EFFLUENT GUIDELINES AND STANDARDS (CONTINUED) MINERAL MINING AND PROCESSING POINT SOURCE CATEGORY Diatomite Subcategory...

  12. Neptune: a bioinformatics tool for rapid discovery of genomic variation in bacterial populations

    PubMed Central

    Marinier, Eric; Zaheer, Rahat; Berry, Chrystal; Weedmark, Kelly A.; Domaratzki, Michael; Mabon, Philip; Knox, Natalie C.; Reimer, Aleisha R.; Graham, Morag R.; Chui, Linda; Patterson-Fortin, Laura; Zhang, Jian; Pagotto, Franco; Farber, Jeff; Mahony, Jim; Seyer, Karine; Bekal, Sadjia; Tremblay, Cécile; Isaac-Renton, Judy; Prystajecky, Natalie; Chen, Jessica; Slade, Peter

    2017-01-01

    Abstract The ready availability of vast amounts of genomic sequence data has created the need to rethink comparative genomics algorithms using ‘big data’ approaches. Neptune is an efficient system for rapidly locating differentially abundant genomic content in bacterial populations using an exact k-mer matching strategy, while accommodating k-mer mismatches. Neptune’s loci discovery process identifies sequences that are sufficiently common to a group of target sequences and sufficiently absent from non-targets using probabilistic models. Neptune uses parallel computing to efficiently identify and extract these loci from draft genome assemblies without requiring multiple sequence alignments or other computationally expensive comparative sequence analyses. Tests on simulated and real datasets showed that Neptune rapidly identifies regions that are both sensitive and specific. We demonstrate that this system can identify trait-specific loci from different bacterial lineages. Neptune is broadly applicable for comparative bacterial analyses, yet will particularly benefit pathogenomic applications, owing to efficient and sensitive discovery of differentially abundant genomic loci. The software is available for download at: http://github.com/phac-nml/neptune. PMID:29048594

  13. Mapping the stability region of the 3:2 Neptune-Pluto resonance

    NASA Technical Reports Server (NTRS)

    Levison, H. F.; Stern, S. A.

    1993-01-01

    Pluto and Charon are most likely the remnants of a large number of objects that existed in the Uranus-Neptune region at early epochs of the solar system. Numerical integrations have shown that, in general, such objects were ejected from the planetary region on timescales of approximately 10(exp 7) years after Neptune and Uranus reached their current masses. It is thought that the Pluto-Charon system survived to current times without being dynamically removed in this way because it is trapped in a set of secular and mean motion resonances with Neptune. The best-known Pluto-Neptune orbit coupling is the 3:2 mean motion resonance discovered almost 30 years ago by C. Cohen and E. Hubbard. These workers showed that the resonance angle, delta is equivalent to 3(lambda(sub P)) - 2(lambda(sub N)) - omega-bar(sub P) where omega-bar(sub P) is the longitude of perihelion of the Pluto-Charon system, and lambda(sub N) and lambda(sub P) are the mean longitude of Neptune and Pluto-Charon respectively, librates about 180 deg with an amplitude, A(sub delta), of 76 deg. A numerical simulation project to map out the stability region of the 3:2 resonance is reported. The results of these simulations are important to understanding whether Pluto's long-term heliocentric stability requires only the 3:2 resonance, or whether it instead requires one or more of the other Pluto-Neptune resonances. Our study also has another important application. By investigating stability timescales as a function of orbital elements, we gain insight into the fraction of orbital phase space which the stable 3:2 resonance occupies. This fraction is directly related to the probability that the Pluto-Charon system (and possibly other small bodies) could have been captured into this resonance.

  14. Plasma and radio waves from Neptune: Source mechamisms and propagation

    NASA Technical Reports Server (NTRS)

    Menietti, J. Douglas

    1994-01-01

    The purpose of this project was to conduct a comprehensive investigation of the radio wave emission observed by the planetary radio astronomy (PRA) instrument on board Voyager 2 as it flew by Neptune. The study has included data analysis, theoretical and numerical calculations, and ray tracing to determine the possible source mechanisms and locations of the radiation, including the narrowband bursty and smooth components of the Neptune radio emission.

  15. 42 CFR 436.840 - Medically needy resource standard: General requirements.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... THE VIRGIN ISLANDS Financial Requirements for the Medically Needy Medically Needy Resource Standard... eligibility under the cash assistance programs that are related to the State's covered medically needy group or groups of individuals under § 436.301. (b) The resource standard established under paragraph (a...

  16. 10 CFR 436.102 - General operations plan format and content.

    Code of Federal Regulations, 2011 CFR

    2011-01-01

    ... tasking resulting from development of the Plan; (B) Guidance for the development of emergency conservation... § 436.106(a); (I) Schedules of plan preparation and publication; (J) Communication, implementation, and... evaluate any innovative energy conserving technologies or methods, not included in this part, which the...

  17. 10 CFR 436.13 - Presuming cost-effectiveness results.

    Code of Federal Regulations, 2014 CFR

    2014-01-01

    ... 10 Energy 3 2014-01-01 2014-01-01 false Presuming cost-effectiveness results. 436.13 Section 436.13 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS Methodology and Procedures for Life Cycle Cost Analyses § 436.13 Presuming cost-effectiveness results. (a) If...

  18. 10 CFR 436.13 - Presuming cost-effectiveness results.

    Code of Federal Regulations, 2012 CFR

    2012-01-01

    ... 10 Energy 3 2012-01-01 2012-01-01 false Presuming cost-effectiveness results. 436.13 Section 436.13 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS Methodology and Procedures for Life Cycle Cost Analyses § 436.13 Presuming cost-effectiveness results. (a) If...

  19. 10 CFR 436.13 - Presuming cost-effectiveness results.

    Code of Federal Regulations, 2011 CFR

    2011-01-01

    ... 10 Energy 3 2011-01-01 2011-01-01 false Presuming cost-effectiveness results. 436.13 Section 436.13 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS Methodology and Procedures for Life Cycle Cost Analyses § 436.13 Presuming cost-effectiveness results. (a) If...

  20. 10 CFR 436.13 - Presuming cost-effectiveness results.

    Code of Federal Regulations, 2013 CFR

    2013-01-01

    ... 10 Energy 3 2013-01-01 2013-01-01 false Presuming cost-effectiveness results. 436.13 Section 436.13 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS Methodology and Procedures for Life Cycle Cost Analyses § 436.13 Presuming cost-effectiveness results. (a) If...

  1. 44 CFR 206.436 - Application procedures.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... 44 Emergency Management and Assistance 1 2010-10-01 2010-10-01 false Application procedures. 206.436 Section 206.436 Emergency Management and Assistance FEDERAL EMERGENCY MANAGEMENT AGENCY... application will identify one or more mitigation measures for which funding is requested. The application must...

  2. 42 CFR 436.1005 - Institutionalized individuals.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... 42 Public Health 4 2011-10-01 2011-10-01 false Institutionalized individuals. 436.1005 Section 436.1005 Public Health CENTERS FOR MEDICARE & MEDICAID SERVICES, DEPARTMENT OF HEALTH AND HUMAN SERVICES (CONTINUED) MEDICAL ASSISTANCE PROGRAMS ELIGIBILITY IN GUAM, PUERTO RICO, AND THE VIRGIN ISLANDS Federal...

  3. 42 CFR 436.1005 - Institutionalized individuals.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... 42 Public Health 4 2010-10-01 2010-10-01 false Institutionalized individuals. 436.1005 Section 436.1005 Public Health CENTERS FOR MEDICARE & MEDICAID SERVICES, DEPARTMENT OF HEALTH AND HUMAN SERVICES (CONTINUED) MEDICAL ASSISTANCE PROGRAMS ELIGIBILITY IN GUAM, PUERTO RICO, AND THE VIRGIN ISLANDS Federal...

  4. Neptune's blue-green atmosphere

    NASA Technical Reports Server (NTRS)

    1989-01-01

    Neptune's blue-green atmosphere is shown in greater detail than ever before by the Voyager 2 spacecraft as it rapidly approaches its encounter with the giant planet. This color image, produced from a distance of about 16 million kilometers, shows several complex and puzzling atmospheric features. The Great Dark Spot (GDS) seen at the center is about 13,000 km by 6,600 km in size -- as large along its longer dimension as the Earth. The bright, wispy 'cirrus-type' clouds seen hovering in the vicinity of the GDS are higher in altitude than the dark material of unknown origin which defines its boundaries. A thin veil often fills part of the GDS interior, as seen on the image. The bright cloud at the southern (lower) edge of the GDS measures about 1,000 km in its north-south extent. The small, bright cloud below the GDS, dubbed the 'scooter,' rotates faster than the GDS, gaining about 30 degrees eastward (toward the right) in longitude every rotation. Bright streaks of cloud at the latitude of the GDS, the small clouds overlying it, and a dimly visible dark protrusion at its western end are examples of dynamic weather patterns on Neptune, which can change significantly on time scales of one rotation (about 18 hours).

  5. 10 CFR 436.12 - Life cycle cost methodology.

    Code of Federal Regulations, 2012 CFR

    2012-01-01

    ... 10 Energy 3 2012-01-01 2012-01-01 false Life cycle cost methodology. 436.12 Section 436.12 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS Methodology and Procedures for Life Cycle Cost Analyses § 436.12 Life cycle cost methodology. The life cycle cost methodology...

  6. 10 CFR 436.12 - Life cycle cost methodology.

    Code of Federal Regulations, 2014 CFR

    2014-01-01

    ... 10 Energy 3 2014-01-01 2014-01-01 false Life cycle cost methodology. 436.12 Section 436.12 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS Methodology and Procedures for Life Cycle Cost Analyses § 436.12 Life cycle cost methodology. The life cycle cost methodology...

  7. 10 CFR 436.12 - Life cycle cost methodology.

    Code of Federal Regulations, 2013 CFR

    2013-01-01

    ... 10 Energy 3 2013-01-01 2013-01-01 false Life cycle cost methodology. 436.12 Section 436.12 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS Methodology and Procedures for Life Cycle Cost Analyses § 436.12 Life cycle cost methodology. The life cycle cost methodology...

  8. 10 CFR 436.12 - Life cycle cost methodology.

    Code of Federal Regulations, 2010 CFR

    2010-01-01

    ... 10 Energy 3 2010-01-01 2010-01-01 false Life cycle cost methodology. 436.12 Section 436.12 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS Methodology and Procedures for Life Cycle Cost Analyses § 436.12 Life cycle cost methodology. The life cycle cost methodology...

  9. 10 CFR 436.12 - Life cycle cost methodology.

    Code of Federal Regulations, 2011 CFR

    2011-01-01

    ... 10 Energy 3 2011-01-01 2011-01-01 false Life cycle cost methodology. 436.12 Section 436.12 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS Methodology and Procedures for Life Cycle Cost Analyses § 436.12 Life cycle cost methodology. The life cycle cost methodology...

  10. 42 CFR 436.403 - State residence.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... 42 Public Health 4 2011-10-01 2011-10-01 false State residence. 436.403 Section 436.403 Public Health CENTERS FOR MEDICARE & MEDICAID SERVICES, DEPARTMENT OF HEALTH AND HUMAN SERVICES (CONTINUED) MEDICAL ASSISTANCE PROGRAMS ELIGIBILITY IN GUAM, PUERTO RICO, AND THE VIRGIN ISLANDS General Eligibility...

  11. 42 CFR 436.811 - Medically needy income standard: General requirements.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... THE VIRGIN ISLANDS Financial Requirements for the Medically Needy Medically Needy Income Standard... groups that meets the requirements of this section. (b) The income standard must take into account the... the State's covered medically needy group or groups of individuals under § 436.301. (d) The income...

  12. Precise Masses & Radii of the Planets Orbiting K2-3 and GJ3470

    NASA Astrophysics Data System (ADS)

    Kosiarek, Molly; Crossfield, Ian; Hardegree-Ullman, Kevin; Livingston, John; Howard, Andrew; Fulton, Benjamin; Hirsch, Lea; Isaacson, Howard; Petigura, Erik; Sinukoff, Evan; Weiss, Lauren; Knutson, Heather; Bonfils, Xavier; Benneke, Björn; Beichman, Charles; Dressing, Courtney

    2018-01-01

    We report improved masses, radii, and densities for two planetary systems, K2-3 and GJ3470, derived from a combination of new radial velocity and transit observations. Both stars are nearby, early M dwarfs. K2-3 hosts three super-Earth planets between 1.5 and 2 Earth-radii at orbital periods between 10 and 45 days, while GJ 3470 hosts one 4 Earth-radii planet with a period of 3.3 days. Furthermore, we confirmed GJ3470's rotation period through multi-year ground-based photometry; RV analysis must account for this rotation signature. Due to the planets' low densities (all < 4.2 g/cm3) and bright host stars, they are among the best candidates for transmission spectroscopy with JWST and HST in order to characterize their atmospheric compositions.

  13. Investigation of atmospheric waves on Neptune

    NASA Technical Reports Server (NTRS)

    Eshleman, Von R.; Hinson, David P.

    1994-01-01

    This document constitutes the final report for grant NAGW-2442 of the Neptune Data Analysis Program, which supported research concerning atmospheric dynamics on Neptune. Professor Von R. Eshleman was the principal investigator. David P. Hinson was a Co-Investigator. The grant covered the period 1 March 1991 through 31 August 1994, including a six month no-cost extension. Funding from this grant resulted in publication of one journal article and one book chapter as well as presentation of results at two conferences and in numerous seminars. A complete bibliography is given below. A copy of the journal article is attached along with abstracts from the book chapter and the conference presentations. With support from this grant we extended our analysis and interpretation of the Voyager Project. This research contributed to an improvement in our basic understanding of atmospheric dynamics on Neptune. The highlight was the discovery and characterization of inertio-gravity waves in the troposphere and stratosphere. Results include measures of basic wave properties, such as amplitudes and vertical wavelengths, as well as estimates of the effect of the waves on the photochemistry and momentum balance of the stratosphere. This investigation also yielded a better understanding of the potential of radio occultation experiments for studies of atmospheric waves. At the same time we developed new methods of data analysis for exploiting these capabilities. These are currently being applied to radio occultation data obtained with the Magellan spacecraft to study waves in the atmosphere of Venus. Future planetary missions, such as Mars Global Surveyor and Cassini, will benefit from these accomplishments.

  14. Neptune - Unexpected and predicted: Prognosis of theory and Voyager-2 observations

    NASA Astrophysics Data System (ADS)

    Chechel'Nitskii, A. M.

    1992-08-01

    The impact of the Voyager-2 discoveries at Neptune on theory are reviewed. The theories of the shell structure of astronomical systems, shell hierarchy, the multicomponent cosmic medium, weak and power elite orbits, quantization of dynamic parameters, and transspheres are summarized and their relevance to the Neptune system, particularly the rings, is considered in the context of the findings of Voyager-2.

  15. The Moons of Uranus, Neptune and Pluto.

    ERIC Educational Resources Information Center

    Brown, Robert Hamilton; Cruikshank, Dale P.

    1985-01-01

    In preparation for the Voyager flybys in 1989, the pace of ground-based investigations of the moons of Uranus, Neptune, and Pluto has quickened considerably. Information derived from these investigations is presented. (JN)

  16. 10 CFR 436.21 - Savings-to-investment ratio.

    Code of Federal Regulations, 2010 CFR

    2010-01-01

    ... 10 Energy 3 2010-01-01 2010-01-01 false Savings-to-investment ratio. 436.21 Section 436.21 Energy... Procedures for Life Cycle Cost Analyses § 436.21 Savings-to-investment ratio. The savings-to-investment ratio... conservation measure. The denominator of the ratio is the present value of the net increase in investment and...

  17. 10 CFR 436.21 - Savings-to-investment ratio.

    Code of Federal Regulations, 2011 CFR

    2011-01-01

    ... 10 Energy 3 2011-01-01 2011-01-01 false Savings-to-investment ratio. 436.21 Section 436.21 Energy... Procedures for Life Cycle Cost Analyses § 436.21 Savings-to-investment ratio. The savings-to-investment ratio... conservation measure. The denominator of the ratio is the present value of the net increase in investment and...

  18. 10 CFR 436.106 - Reporting requirements.

    Code of Federal Regulations, 2010 CFR

    2010-01-01

    ... 10 Energy 3 2010-01-01 2010-01-01 false Reporting requirements. 436.106 Section 436.106 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS Guidelines for... shall submit an “Annual Report on Energy Management” based on fiscal year data to the Secretary of DOE...

  19. 10 CFR 436.106 - Reporting requirements.

    Code of Federal Regulations, 2011 CFR

    2011-01-01

    ... 10 Energy 3 2011-01-01 2011-01-01 false Reporting requirements. 436.106 Section 436.106 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS Guidelines for... shall submit an “Annual Report on Energy Management” based on fiscal year data to the Secretary of DOE...

  20. 10 CFR 436.106 - Reporting requirements.

    Code of Federal Regulations, 2012 CFR

    2012-01-01

    ... 10 Energy 3 2012-01-01 2012-01-01 false Reporting requirements. 436.106 Section 436.106 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS Guidelines for... shall submit an “Annual Report on Energy Management” based on fiscal year data to the Secretary of DOE...

  1. 10 CFR 436.106 - Reporting requirements.

    Code of Federal Regulations, 2013 CFR

    2013-01-01

    ... 10 Energy 3 2013-01-01 2013-01-01 false Reporting requirements. 436.106 Section 436.106 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS Guidelines for... shall submit an “Annual Report on Energy Management” based on fiscal year data to the Secretary of DOE...

  2. 10 CFR 436.106 - Reporting requirements.

    Code of Federal Regulations, 2014 CFR

    2014-01-01

    ... 10 Energy 3 2014-01-01 2014-01-01 false Reporting requirements. 436.106 Section 436.106 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS Guidelines for... shall submit an “Annual Report on Energy Management” based on fiscal year data to the Secretary of DOE...

  3. 10 CFR 436.15 - Formatting cost data.

    Code of Federal Regulations, 2013 CFR

    2013-01-01

    ... Procedures for Life Cycle Cost Analyses § 436.15 Formatting cost data. In establishing cost data under §§ 436... software referenced in the Life Cycle Cost Manual for the Federal Energy Management Program. ...

  4. 10 CFR 436.15 - Formatting cost data.

    Code of Federal Regulations, 2014 CFR

    2014-01-01

    ... Procedures for Life Cycle Cost Analyses § 436.15 Formatting cost data. In establishing cost data under §§ 436... software referenced in the Life Cycle Cost Manual for the Federal Energy Management Program. ...

  5. 10 CFR 436.15 - Formatting cost data.

    Code of Federal Regulations, 2012 CFR

    2012-01-01

    ... Procedures for Life Cycle Cost Analyses § 436.15 Formatting cost data. In establishing cost data under §§ 436... software referenced in the Life Cycle Cost Manual for the Federal Energy Management Program. ...

  6. 10 CFR 436.15 - Formatting cost data.

    Code of Federal Regulations, 2010 CFR

    2010-01-01

    ... Procedures for Life Cycle Cost Analyses § 436.15 Formatting cost data. In establishing cost data under §§ 436... software referenced in the Life Cycle Cost Manual for the Federal Energy Management Program. ...

  7. Magnetospheric Science at Uranus and Neptune

    NASA Astrophysics Data System (ADS)

    Hospodarsky, G. B.; Masters, A.; Soderlund, K. M.; Mandt, K. E.

    2017-12-01

    The magnetospheres of the Ice Giant planets Uranus and Neptune have only been sampled in-situ by the Voyager 2 spacecraft, which revealed a very complicated and dynamic system. In combination with the much weaker solar wind at these distances, the large diurnal and seasonal variability of the magnetospheres' orientation with respect to the solar wind, results in characteristics that are very different from the magnetospheres of Earth and the Gas Giants, Jupiter and Saturn. Studying these magnetospheres is important for furthering our understanding of fundamental physical and chemical processes in the Solar System, and may help in understanding the magnetic fields of exoplanets as well. A number of studies, proposals, and reports, including the recently completed "Ice Giants Pre-Decadal Survey Mission Study Report" have demonstrated the interest in a new mission to the Ice Giants. We will review the magnetospheric results from Voyager 2, summarize outstanding science questions, and discuss possible goals of a future mission to Uranus and/or Neptune.

  8. 42 CFR 436.301 - General rules.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ...) MEDICAL ASSISTANCE PROGRAMS ELIGIBILITY IN GUAM, PUERTO RICO, AND THE VIRGIN ISLANDS Optional Coverage of... provide Medicaid to any or all of the following groups of individuals: (i) Individuals under age 21 (§ 436...) Disabled (§ 436.322). (3) If the agency provides Medicaid to any individual in a group specified in...

  9. Plasma and radio waves from Neptune: Source mechanisms and propagation

    NASA Astrophysics Data System (ADS)

    Wong, H. K.

    1994-03-01

    This report summarizes results obtained through the support of NASA Grant NAGW-2412. The objective of this project is to conduct a comprehensive investigation of the radio wave emission observed by the planetary radio astronomy (PRA) instrument on board Voyager 2 as if flew by Neptune. This study has included data analysis, theoretical and numerical calculations, ray tracing, and modeling to determine the possible source mechanism(s) and locations of the Neptune radio emissions. We have completed four papers, which are included in the appendix. The paper 'Modeling of Whistler Ray Paths in the Magnetosphere of Neptune' investigated the propagation and dispersion of lighting-generated whistler in the magnetosphere of Neptune by using three dimensional ray tracing. The two papers 'Numerical Simulations of Bursty Radio Emissions from Planetary Magnetospheres' and 'Numerical Simulations of Bursty Planetary Radio Emissions' employed numerical simulations to investigate an alternate source mechanism of bursty radio emissions in addition to the cyclotron maser instability. We have also studied the possible generation of Z and whistler mode waves by the temperature anisotropic beam instability and the result was published in 'Electron Cyclotron Wave Generation by Relativistic Electrons.' Besides the aforementioned studies, we have also collaborated with members of the PRA team to investigate various aspects of the radio wave data. Two papers have been submitted for publication and the abstracts of these papers are also listed in the appendix.

  10. Plasma and radio waves from Neptune: Source mechanisms and propagation

    NASA Technical Reports Server (NTRS)

    Wong, H. K.

    1994-01-01

    This report summarizes results obtained through the support of NASA Grant NAGW-2412. The objective of this project is to conduct a comprehensive investigation of the radio wave emission observed by the planetary radio astronomy (PRA) instrument on board Voyager 2 as if flew by Neptune. This study has included data analysis, theoretical and numerical calculations, ray tracing, and modeling to determine the possible source mechanism(s) and locations of the Neptune radio emissions. We have completed four papers, which are included in the appendix. The paper 'Modeling of Whistler Ray Paths in the Magnetosphere of Neptune' investigated the propagation and dispersion of lighting-generated whistler in the magnetosphere of Neptune by using three dimensional ray tracing. The two papers 'Numerical Simulations of Bursty Radio Emissions from Planetary Magnetospheres' and 'Numerical Simulations of Bursty Planetary Radio Emissions' employed numerical simulations to investigate an alternate source mechanism of bursty radio emissions in addition to the cyclotron maser instability. We have also studied the possible generation of Z and whistler mode waves by the temperature anisotropic beam instability and the result was published in 'Electron Cyclotron Wave Generation by Relativistic Electrons.' Besides the aforementioned studies, we have also collaborated with members of the PRA team to investigate various aspects of the radio wave data. Two papers have been submitted for publication and the abstracts of these papers are also listed in the appendix.

  11. 16 CFR 436.6 - Instructions for preparing disclosure documents.

    Code of Federal Regulations, 2010 CFR

    2010-01-01

    ... 16 Commercial Practices 1 2010-01-01 2010-01-01 false Instructions for preparing disclosure documents. 436.6 Section 436.6 Commercial Practices FEDERAL TRADE COMMISSION TRADE REGULATION RULES DISCLOSURE REQUIREMENTS AND PROHIBITIONS CONCERNING FRANCHISING Instructions § 436.6 Instructions for...

  12. Loddigesiinols G-J: α-glucosidase inhibitors from Dendrobium loddigesii.

    PubMed

    Lu, Yu; Kuang, Ming; Hu, Gu-Ping; Wu, Rui-Bo; Wang, Jun; Liu, Lan; Lin, Yong-Cheng

    2014-06-23

    Four new polyphenols, loddigesiinols G-J (compounds 1-4) and a known compound, crepidatuol B (5), were isolated from the stems of Dendrobium loddigesii that have long been used in Traditional Chinese Medicine and have recently been used to treat type 2 diabetes. Compounds 1-5 structures were elucidated based on spectroscopic analysis. The absolute configurations of compounds 1-4 were determined using theoretical calculations of electronic circular dichroism (ECD), and the absolute configuration of compound 5 was determined by a comparison of the experimental ECD spectra and the literature data. Compounds 1-5 are strong inhibitors of α-glucosidase, with IC50 values of 16.7, 10.9, 2.7, 3.2, and 18.9 μM, respectively. Their activities were significantly stronger than trans-resveratrol as a positive control (IC50 values of 27.9 μM).

  13. 10 CFR 436.24 - Uncertainty analyses.

    Code of Federal Regulations, 2010 CFR

    2010-01-01

    ... Procedures for Life Cycle Cost Analyses § 436.24 Uncertainty analyses. If particular items of cost data or timing of cash flows are uncertain and are not fixed under § 436.14, Federal agencies may examine the impact of uncertainty on the calculation of life cycle cost effectiveness or the assignment of rank order...

  14. Some aspects of the cosmogonic outward migration of Neptune. Co-planar migration

    NASA Astrophysics Data System (ADS)

    Neslušan, L.; Jakubík, M.

    2013-10-01

    Considering a simple model of the cosmogonic outward migration of Neptune, we investigate if the assumption of an extremely low orbital inclination of small bodies in a once-existing proto-planetary disk could influence the structure of reservoirs of the objects in the trans-Neptunian region. We found no significant influence. Our models predict only the existence of the mean-motion resonances (MMRs) with Neptune 2:3, 3:5, 1:2, and an anemic scattered disk (MMRs 3:4, 5:7, and 9:11 are also indicated). To explain the classical Edgeworth-Kuiper belt, relatively abundant 4:7 and 2:5 MMRs, and the more numerous scattered disk, we need to assume that, e.g., the outer boundary of the original proto-planetary disk considerably exceeded the distance of the current Neptune's orbit (Neptune probably ended its migration at the distance, where the disk's density started to be sub-critical), or that some Pluto-sized objects resided inside the MMRs and in the distant parts of the original proto-planetary disk.

  15. Neptune - Changes in Great Dark Spot

    NASA Technical Reports Server (NTRS)

    1989-01-01

    These images show changes in the clouds around Neptune's Great Dark Spot (GDS) over a four and one-half-day period. From top to bottom the images show successive rotations of the planet an interval of about 18 hours. The GDS is at a mean latitude of 20 degrees south, and covers about 30 degrees of longitude. The violet filter of the Voyager narrow angle camera was used to produce these images at distances ranging from 17 million kilometers (10.5 million miles) at the top, to 10 million kilometers (6.2 million miles) at bottom. The images have been mapped on to a rectangular latitude longitude grid to remove the effects of changing viewing geometry and the changing distance to Neptune. The sequence shows a large change in the western end (left side) of the GDS, where a dark extension apparent in the earlier images converges into an extended string of small dark spots over the next five rotations. This 'string of beads' extends from the GDS at a surprisingly large angle relative to horizontal lines of constant latitude. The large bright cloud at the southern (bottom) border of the GDS is a more or less permanent companion of the GDS. The apparent motion of smaller clouds at the periphery of the GDS suggests a counterclockwise rotation of the GDS reminiscent of flow around the Great Red Spot in Jupiter's atmosphere. This activity of the GDS is surprising because the total energy flux from the sun and from Neptune's interior is only 5 percent as large as the total energy flux on Jupiter.

  16. A Search for Small Distant Moons of Neptune

    NASA Astrophysics Data System (ADS)

    Holman, Matthew; Kavelaars, Jj; Gladman, Brett; Petit, Jean-Marc; Grav, Tommy; Nicholson, Philip

    2002-08-01

    With many new jovian, saturnian, and uranian irregular satellites having been discovered in the last few years, our attention naturally falls upon Neptune. In 1999, we conducted a search for neptunian satellites covering about 8 square degrees (almost the entire stable region around the planet). This survey yielded no new satellites down to R magnitude 24. We interpreted this as supporting a violent destruction of the Neptunian outer satellite system as Triton was captured. However, there were good reasons to believe that the largest un-discovered Neptune satellites lay just beyond the previous survey's magnitude limit. In August 2001, we used the mosaic camera on the Blanco 4-m to push down to m_R~eq25.5, to test this hypothesis. We discovered two neptunian satellites candidates. Using the time available after Neptune had set, we also discovered four faint uranian satellite candidates. However, poor weather at Palomar and Magellan in September 2001 and instrumental problems on the VLT in November 2001 prevented the tracking these candidates to conclusively prove that they are moons. We request time to repeat last summer's search and "re- discover" these moons, armed with the knowledge that they are there as well as having assured access to large-aperture southern hemisphere tracking time (on VLT and Magellan).

  17. Neptune Blue-green Atmosphere

    NASA Image and Video Library

    2000-02-16

    Neptune's blue-green atmosphere is shown in greater detail than ever before by the Voyager 2 spacecraft as it rapidly approaches its encounter with the giant planet. This color image, produced from a distance of about 16 million kilometers, shows several complex and puzzling atmospheric features. The Great Dark Spot (GDS) seen at the center is about 13,000 km by 6,600 km in size -- as large along its longer dimension as the Earth. The bright, wispy "cirrus-type" clouds seen hovering in the vicinity of the GDS are higher in altitude than the dark material of unknown origin which defines its boundaries. A thin veil often fills part of the GDS interior, as seen on the image. The bright cloud at the southern (lower) edge of the GDS measures about 1,000 km in its north-south extent. The small, bright cloud below the GDS, dubbed the "scooter," rotates faster than the GDS, gaining about 30 degrees eastward (toward the right) in longitude every rotation. Bright streaks of cloud at the latitude of the GDS, the small clouds overlying it, and a dimly visible dark protrusion at its western end are examples of dynamic weather patterns on Neptune, which can change significantly on time scales of one rotation (about 18 hours). https://photojournal.jpl.nasa.gov/catalog/PIA02245

  18. 10 CFR 436.104 - Energy conservation measures and standards.

    Code of Federal Regulations, 2012 CFR

    2012-01-01

    ... 10 Energy 3 2012-01-01 2012-01-01 false Energy conservation measures and standards. 436.104 Section 436.104 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS Guidelines for General Operations Plans § 436.104 Energy conservation measures and standards. (a...

  19. 10 CFR 436.104 - Energy conservation measures and standards.

    Code of Federal Regulations, 2011 CFR

    2011-01-01

    ... 10 Energy 3 2011-01-01 2011-01-01 false Energy conservation measures and standards. 436.104 Section 436.104 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS Guidelines for General Operations Plans § 436.104 Energy conservation measures and standards. (a...

  20. 10 CFR 436.104 - Energy conservation measures and standards.

    Code of Federal Regulations, 2010 CFR

    2010-01-01

    ... 10 Energy 3 2010-01-01 2010-01-01 false Energy conservation measures and standards. 436.104 Section 436.104 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS Guidelines for General Operations Plans § 436.104 Energy conservation measures and standards. (a...

  1. 10 CFR 436.104 - Energy conservation measures and standards.

    Code of Federal Regulations, 2013 CFR

    2013-01-01

    ... 10 Energy 3 2013-01-01 2013-01-01 false Energy conservation measures and standards. 436.104 Section 436.104 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS Guidelines for General Operations Plans § 436.104 Energy conservation measures and standards. (a...

  2. 10 CFR 436.104 - Energy conservation measures and standards.

    Code of Federal Regulations, 2014 CFR

    2014-01-01

    ... 10 Energy 3 2014-01-01 2014-01-01 false Energy conservation measures and standards. 436.104 Section 436.104 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS Guidelines for General Operations Plans § 436.104 Energy conservation measures and standards. (a...

  3. 40 CFR 98.436 - Data reporting requirements.

    Code of Federal Regulations, 2012 CFR

    2012-07-01

    ... 40 Protection of Environment 22 2012-07-01 2012-07-01 false Data reporting requirements. 98.436 Section 98.436 Protection of Environment ENVIRONMENTAL PROTECTION AGENCY (CONTINUED) AIR PROGRAMS (CONTINUED) MANDATORY GREENHOUSE GAS REPORTING Importers and Exporters of Fluorinated Greenhouse Gases...

  4. First generation atmospheric probes (10-BARS) for Uranus and Neptune

    NASA Technical Reports Server (NTRS)

    Sullivan, R. J.; Waters, J. I.; Dunkin, J. H.

    1972-01-01

    The feasibility of atmospheric entry probe missions to Uranus and Neptune is studied, and preliminary estimates of missions parameters are presented. Most of the study results are applicable, with only minor modifications, to Uranus-Neptune entry probes included on any type of outer planet mission. Trajectory dynamics is discussed first because it imposes some important constraints upon the total time available for data transmission, which in turn determines the descent rate. This last quantity provides important information for the design of the scientific payload.

  5. 48 CFR 436.609-1 - Design within funding limitations.

    Code of Federal Regulations, 2012 CFR

    2012-10-01

    ... 48 Federal Acquisition Regulations System 4 2012-10-01 2012-10-01 false Design within funding limitations. 436.609-1 Section 436.609-1 Federal Acquisition Regulations System DEPARTMENT OF AGRICULTURE SPECIAL CATEGORIES OF CONTRACTING CONSTRUCTION AND ARCHITECT-ENGINEER CONTRACTS Architect-Engineer Service 436.609-1 Design within funding...

  6. 48 CFR 436.609-1 - Design within funding limitations.

    Code of Federal Regulations, 2013 CFR

    2013-10-01

    ... 48 Federal Acquisition Regulations System 4 2013-10-01 2013-10-01 false Design within funding limitations. 436.609-1 Section 436.609-1 Federal Acquisition Regulations System DEPARTMENT OF AGRICULTURE SPECIAL CATEGORIES OF CONTRACTING CONSTRUCTION AND ARCHITECT-ENGINEER CONTRACTS Architect-Engineer Service 436.609-1 Design within funding...

  7. 48 CFR 436.609-1 - Design within funding limitations.

    Code of Federal Regulations, 2014 CFR

    2014-10-01

    ... 48 Federal Acquisition Regulations System 4 2014-10-01 2014-10-01 false Design within funding limitations. 436.609-1 Section 436.609-1 Federal Acquisition Regulations System DEPARTMENT OF AGRICULTURE SPECIAL CATEGORIES OF CONTRACTING CONSTRUCTION AND ARCHITECT-ENGINEER CONTRACTS Architect-Engineer Service 436.609-1 Design within funding...

  8. 48 CFR 436.609-1 - Design within funding limitations.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... 48 Federal Acquisition Regulations System 4 2011-10-01 2011-10-01 false Design within funding limitations. 436.609-1 Section 436.609-1 Federal Acquisition Regulations System DEPARTMENT OF AGRICULTURE... 436.609-1 Design within funding limitations. (a) Should the head of the contracting activity appoint a...

  9. Hubble Finds New Dark Spot on Neptune

    NASA Image and Video Library

    1998-08-02

    In 1995, NASA Hubble Space Telescope discovered a new great dark spot, located in the northern hemisphere of the planet Neptune. Because the planet northern hemisphere was tilted away from Earth, the new feature appeared near the limb of the planet.

  10. The "Theft" of the Neptune Papers

    NASA Astrophysics Data System (ADS)

    Rawlins, Dennis

    1994-10-01

    Correspondence 1966-1993 attempting to flush out the long-secreted Royal Greenwich Observatory file on Neptune's discovery, hinting that it was in the possession of a former Chief Ass't to the Astronomer Royal. The file was ultimately found among his effects, four years after this article, when he unexpectedly died in Chile.

  11. GJ 1214: Rotation period, starspots, and uncertainty on the optical slope of the transmission spectrum

    NASA Astrophysics Data System (ADS)

    Mallonn, M.; Herrero, E.; Juvan, I. G.; Essen, C. von; Rosich, A.; Ribas, I.; Granzer, T.; Alexoudi, X.; Strassmeier, K. G.

    2018-06-01

    Aims: Brightness inhomogeneities in the stellar photosphere (dark spots or bright regions) affect the measurements of the planetary transmission spectrum. To investigate the star spots of the M dwarf GJ 1214, we conducted a multicolor photometric monitoring from 2012 to 2016. Methods: The time-series photometry was analyzed with the light curve inversion tool StarSim. Using the derived stellar surface properties from the light curve inversion, we modeled the impact of the star spots when unocculted by the transiting planet. We compared the photometric variability of GJ 1214 to published results of mid- to late M dwarfs from the MEarth sample. Results: The measured variability shows a periodicity of 125 ± 5 days, which we interpret as the signature of the stellar rotation period. This value overrules previous suggestions of a significantly shorter stellar rotation period. A light curve inversion of the monitoring data yields an estimation of the flux dimming of a permanent spot filling factor not contributing to the photometric variability, a temperature contrast of the spots of 370 K and persistent active longitudes. The derived surface maps over all five seasons were used to estimate the influence of the star spots on the transmission spectrum of the planet from 400 to 2000 nm. The monitoring data presented here do not support a recent interpretation of a measured transmission spectrum of GJ 1214b as to be caused by bright regions in the stellar photosphere. Instead, we list arguments as to why the effect of dark spots likely dominated over bright regions in the period of our monitoring. Furthermore, our photometry proves an increase in variability over at least four years, indicative for a cyclic activity behavior. The age of GJ 1214 is likely between 6 and 10 Gyr. Conclusions: The long-term photometry allows for a correction of unocculted spots. For an active star such as GJ 1214, there remains a degeneracy between occulted spots and the transit parameters used

  12. 42 CFR 436.520 - Age requirements for the aged.

    Code of Federal Regulations, 2013 CFR

    2013-10-01

    ... 42 Public Health 4 2013-10-01 2013-10-01 false Age requirements for the aged. 436.520 Section 436... Requirements for Medicaid Eligibility Age § 436.520 Age requirements for the aged. The agency must not impose an age requirement of more than 65 years. [58 FR 4936, Jan. 19, 1993] ...

  13. 42 CFR 436.520 - Age requirements for the aged.

    Code of Federal Regulations, 2012 CFR

    2012-10-01

    ... 42 Public Health 4 2012-10-01 2012-10-01 false Age requirements for the aged. 436.520 Section 436... Requirements for Medicaid Eligibility Age § 436.520 Age requirements for the aged. The agency must not impose an age requirement of more than 65 years. [58 FR 4936, Jan. 19, 1993] ...

  14. 42 CFR 436.520 - Age requirements for the aged.

    Code of Federal Regulations, 2014 CFR

    2014-10-01

    ... 42 Public Health 4 2014-10-01 2014-10-01 false Age requirements for the aged. 436.520 Section 436... Requirements for Medicaid Eligibility Age § 436.520 Age requirements for the aged. The agency must not impose an age requirement of more than 65 years. [58 FR 4936, Jan. 19, 1993] ...

  15. 42 CFR 436.520 - Age requirements for the aged.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... 42 Public Health 4 2011-10-01 2011-10-01 false Age requirements for the aged. 436.520 Section 436... Requirements for Medicaid Eligibility Age § 436.520 Age requirements for the aged. The agency must not impose an age requirement of more than 65 years. [58 FR 4936, Jan. 19, 1993] ...

  16. 42 CFR 436.520 - Age requirements for the aged.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... 42 Public Health 4 2010-10-01 2010-10-01 false Age requirements for the aged. 436.520 Section 436... Requirements for Medicaid Eligibility Age § 436.520 Age requirements for the aged. The agency must not impose an age requirement of more than 65 years. [58 FR 4936, Jan. 19, 1993] ...

  17. NEPTUNE: an under-sea plate scale observatory

    NASA Technical Reports Server (NTRS)

    Beauchamp, P. M.; Heath, G. R.; Maffei, A.; Chave, A.; Howe, B.; Wilcock, W.; Delaney, J.; Kirkham, H.

    2002-01-01

    The NEPTUNE project will establish a linked array of undersea observatories on the Juan de Fuca tectonic plate. This observatory will provide a new kind of research platform for real-time, long-term, plate-scale studies in the ocean and Earth sciences.

  18. 48 CFR 436.603 - Collecting data on and appraising firms' qualifications.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... 48 Federal Acquisition Regulations System 4 2010-10-01 2010-10-01 false Collecting data on and... Architect-Engineer Service 436.603 Collecting data on and appraising firms' qualifications. (a) HCA's which....603. (b) The procedures shall include a list of names, addresses, and phone numbers of offices or...

  19. 48 CFR 436.603 - Collecting data on and appraising firms' qualifications.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... 48 Federal Acquisition Regulations System 4 2011-10-01 2011-10-01 false Collecting data on and... Architect-Engineer Service 436.603 Collecting data on and appraising firms' qualifications. (a) HCA's which....603. (b) The procedures shall include a list of names, addresses, and phone numbers of offices or...

  20. Voyager planetary radio astronomy at neptune.

    PubMed

    Warwick, J W; Evans, D R; Peltzer, G R; Peltzer, R G; Romig, J H; Sawyer, C B; Riddle, A C; Schweitzer, A E; Desch, M D; Kaiser, M L; Farrell, W M; Carr, T D; de Pater, I; Staelin, D H; Gulkis, S; Poynter, R L; Boischot, A; Genova, F; Leblanc, Y; Lecacheux, A; Pedersen, B M; Zarka, P

    1989-12-15

    Detection of very intense short radio bursts from Neptune was possible as early as 30 days before closest approach and at least 22 days after closest approach. The bursts lay at frequencies in the range 100 to 1300 kilohertz, were narrowband and strongly polarized, and presumably originated in southern polar regions ofthe planet. Episodes of smooth emissions in the frequency range from 20 to 865 kilohertz were detected during an interval of at least 10 days around closest approach. The bursts and the smooth emissions can be described in terms of rotation in a period of 16.11 +/- 0.05 hours. The bursts came at regular intervals throughout the encounter, including episodes both before and after closest approach. The smooth emissions showed a half-cycle phase shift between the five episodes before and after closest approach. This experiment detected the foreshock of Neptune's magnetosphere and the impacts of dust at the times of ring-plane crossings and also near the time of closest approach. Finally, there is no evidence for Neptunian electrostatic discharges.

  1. 42 CFR 436.121 - Qualified family members.

    Code of Federal Regulations, 2014 CFR

    2014-10-01

    ... 42 Public Health 4 2014-10-01 2014-10-01 false Qualified family members. 436.121 Section 436.121 Public Health CENTERS FOR MEDICARE & MEDICAID SERVICES, DEPARTMENT OF HEALTH AND HUMAN SERVICES (CONTINUED) MEDICAL ASSISTANCE PROGRAMS ELIGIBILITY IN GUAM, PUERTO RICO, AND THE VIRGIN ISLANDS Mandatory...

  2. 42 CFR 436.10 - State plan requirements.

    Code of Federal Regulations, 2014 CFR

    2014-10-01

    ... 42 Public Health 4 2014-10-01 2014-10-01 false State plan requirements. 436.10 Section 436.10 Public Health CENTERS FOR MEDICARE & MEDICAID SERVICES, DEPARTMENT OF HEALTH AND HUMAN SERVICES (CONTINUED) MEDICAL ASSISTANCE PROGRAMS ELIGIBILITY IN GUAM, PUERTO RICO, AND THE VIRGIN ISLANDS General...

  3. 48 CFR 436.602-1 - Selection criteria.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... 48 Federal Acquisition Regulations System 4 2010-10-01 2010-10-01 false Selection criteria. 436.602-1 Section 436.602-1 Federal Acquisition Regulations System DEPARTMENT OF AGRICULTURE SPECIAL... Selection criteria. The HCA is authorized to approve the use of design competition under the conditions in...

  4. 40 CFR 436.240 - Applicability; description of the diatomite subcategory.

    Code of Federal Regulations, 2014 CFR

    2014-07-01

    ... diatomite subcategory. 436.240 Section 436.240 Protection of Environment ENVIRONMENTAL PROTECTION AGENCY... Diatomite Subcategory § 436.240 Applicability; description of the diatomite subcategory. The provisions of this subpart are applicable to the processing of diatomite. ...

  5. 40 CFR 436.240 - Applicability; description of the diatomite subcategory.

    Code of Federal Regulations, 2013 CFR

    2013-07-01

    ... diatomite subcategory. 436.240 Section 436.240 Protection of Environment ENVIRONMENTAL PROTECTION AGENCY... Diatomite Subcategory § 436.240 Applicability; description of the diatomite subcategory. The provisions of this subpart are applicable to the processing of diatomite. ...

  6. 40 CFR 436.240 - Applicability; description of the diatomite subcategory.

    Code of Federal Regulations, 2012 CFR

    2012-07-01

    ... diatomite subcategory. 436.240 Section 436.240 Protection of Environment ENVIRONMENTAL PROTECTION AGENCY... Diatomite Subcategory § 436.240 Applicability; description of the diatomite subcategory. The provisions of this subpart are applicable to the processing of diatomite. ...

  7. 42 CFR 436.128 - Coverage for certain qualified aliens.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... 42 Public Health 4 2010-10-01 2010-10-01 false Coverage for certain qualified aliens. 436.128... Mandatory Coverage of the Categorically Needy § 436.128 Coverage for certain qualified aliens. The agency... § 440.255(c) of this chapter to those aliens described in § 436.406(c) of this subpart. [55 FR 36820...

  8. 42 CFR 436.128 - Coverage for certain qualified aliens.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... 42 Public Health 4 2011-10-01 2011-10-01 false Coverage for certain qualified aliens. 436.128... Mandatory Coverage of the Categorically Needy § 436.128 Coverage for certain qualified aliens. The agency... § 440.255(c) of this chapter to those aliens described in § 436.406(c) of this subpart. [55 FR 36820...

  9. 42 CFR 436.128 - Coverage for certain qualified aliens.

    Code of Federal Regulations, 2012 CFR

    2012-10-01

    ... 42 Public Health 4 2012-10-01 2012-10-01 false Coverage for certain qualified aliens. 436.128... Mandatory Coverage of the Categorically Needy § 436.128 Coverage for certain qualified aliens. The agency... § 440.255(c) of this chapter to those aliens described in § 436.406(c) of this subpart. [55 FR 36820...

  10. 42 CFR 436.128 - Coverage for certain qualified aliens.

    Code of Federal Regulations, 2014 CFR

    2014-10-01

    ... 42 Public Health 4 2014-10-01 2014-10-01 false Coverage for certain qualified aliens. 436.128... Mandatory Coverage of the Categorically Needy § 436.128 Coverage for certain qualified aliens. The agency... § 440.255(c) of this chapter to those aliens described in § 436.406(c) of this subpart. [55 FR 36820...

  11. 42 CFR 436.128 - Coverage for certain qualified aliens.

    Code of Federal Regulations, 2013 CFR

    2013-10-01

    ... 42 Public Health 4 2013-10-01 2013-10-01 false Coverage for certain qualified aliens. 436.128... Mandatory Coverage of the Categorically Needy § 436.128 Coverage for certain qualified aliens. The agency... § 440.255(c) of this chapter to those aliens described in § 436.406(c) of this subpart. [55 FR 36820...

  12. An Analysis of Neptune's Stratospheric Haze Using High-Phase-Angle Voyager Images

    NASA Technical Reports Server (NTRS)

    Moses, Julianne I.; Rages, Kathy; Pollack, James B.

    1995-01-01

    We have inverted high-phase-angle Voyager images of Neptune to determine the atmospheric extinction coefficient as a function of altitude and the scattering phase function at a reference altitude. Comparisons between theoretical model and observations help separate the contributions from molecular Rayleigh and aerosol scattering and help determine the variation of the aerosol size, concentration, and scattering properties with altitude. Further comparisons between models and data allow us to place constraints on the location and composition of the hazes, the concentration and downward flux of certain condensible hydrocarbon gases, the eddy diffusion coefficient in the lower stratosphere, and the thermal profile in parts of Neptune's stratosphere. We find that a distinct stratospheric haze layer exists near 12(sub -1, sup +1) mbar in Neptune's lower stratosphere, most probably due to condensed ethane. The derived stratospheric haze production rate of 1.0(sub -0.3, sup +0.2) x 10(exp -15) g cm(exp -2) sec(exp -1) is substantially lower than photochemical model predictions. Evidence for hazes at higher altitudes also exists. Unlike the situation on Uranus, large particles (0.08-0.11 microns) may be present at high altitudes on Neptune (e.g., near 0.5 mbar), well above the region in which we expect the major hydrocarbon species to condense. Near 28 mbar, the mean particle size is about 0.13(sub -0.02, sup +0.02) microns with a concentration of 5(sub -3, sup +3) particles cm(exp -3). The cumulative haze extinction optical depth above 15 mbar in the clear filter is approx. 3 x 10(exp -3), and much of this extinction is due to scattering rather than absorption; thus, if our limb-scan sites are typical, the hazes cannot account for the stratospheric temperature inversion on Neptune and may not contribute significantly to atmospheric heating. We compare the imaging results with the results from other observations, including those of the Voyager Photopolarimeter Subsystem

  13. 48 CFR 436.209 - Construction contracts with architect-engineer firms.

    Code of Federal Regulations, 2013 CFR

    2013-10-01

    ... with architect-engineer firms. 436.209 Section 436.209 Federal Acquisition Regulations System DEPARTMENT OF AGRICULTURE SPECIAL CATEGORIES OF CONTRACTING CONSTRUCTION AND ARCHITECT-ENGINEER CONTRACTS Special Aspects of Contracting for Construction 436.209 Construction contracts with architect-engineer...

  14. 48 CFR 436.209 - Construction contracts with architect-engineer firms.

    Code of Federal Regulations, 2014 CFR

    2014-10-01

    ... with architect-engineer firms. 436.209 Section 436.209 Federal Acquisition Regulations System DEPARTMENT OF AGRICULTURE SPECIAL CATEGORIES OF CONTRACTING CONSTRUCTION AND ARCHITECT-ENGINEER CONTRACTS Special Aspects of Contracting for Construction 436.209 Construction contracts with architect-engineer...

  15. 48 CFR 436.209 - Construction contracts with architect-engineer firms.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... with architect-engineer firms. 436.209 Section 436.209 Federal Acquisition Regulations System DEPARTMENT OF AGRICULTURE SPECIAL CATEGORIES OF CONTRACTING CONSTRUCTION AND ARCHITECT-ENGINEER CONTRACTS Special Aspects of Contracting for Construction 436.209 Construction contracts with architect-engineer...

  16. 48 CFR 436.209 - Construction contracts with architect-engineer firms.

    Code of Federal Regulations, 2012 CFR

    2012-10-01

    ... with architect-engineer firms. 436.209 Section 436.209 Federal Acquisition Regulations System DEPARTMENT OF AGRICULTURE SPECIAL CATEGORIES OF CONTRACTING CONSTRUCTION AND ARCHITECT-ENGINEER CONTRACTS Special Aspects of Contracting for Construction 436.209 Construction contracts with architect-engineer...

  17. 48 CFR 436.209 - Construction contracts with architect-engineer firms.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... with architect-engineer firms. 436.209 Section 436.209 Federal Acquisition Regulations System DEPARTMENT OF AGRICULTURE SPECIAL CATEGORIES OF CONTRACTING CONSTRUCTION AND ARCHITECT-ENGINEER CONTRACTS Special Aspects of Contracting for Construction 436.209 Construction contracts with architect-engineer...

  18. 10 CFR 436.18 - Measuring cost-effectiveness.

    Code of Federal Regulations, 2012 CFR

    2012-01-01

    ... water system, considered in determining such matters as the optimal size of a solar energy system, the... 10 Energy 3 2012-01-01 2012-01-01 false Measuring cost-effectiveness. 436.18 Section 436.18 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS Methodology and...

  19. 10 CFR 436.18 - Measuring cost-effectiveness.

    Code of Federal Regulations, 2014 CFR

    2014-01-01

    ... water system, considered in determining such matters as the optimal size of a solar energy system, the... 10 Energy 3 2014-01-01 2014-01-01 false Measuring cost-effectiveness. 436.18 Section 436.18 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS Methodology and...

  20. 10 CFR 436.18 - Measuring cost-effectiveness.

    Code of Federal Regulations, 2013 CFR

    2013-01-01

    ... water system, considered in determining such matters as the optimal size of a solar energy system, the... 10 Energy 3 2013-01-01 2013-01-01 false Measuring cost-effectiveness. 436.18 Section 436.18 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS Methodology and...

  1. Mid-Infrared Ethane Emission on Neptune: 2005-2009

    NASA Astrophysics Data System (ADS)

    Hammel, Heidi B.; Sitko, M. L.; Russell, R. W.; Lynch, D. K.; Bernstein, L. S.; Perry, R. B.

    2009-09-01

    Hammel et al. (2006, ApJ 644, 1326) reported 8- to 13-micron spectral observations of Neptune spanning more than a decade. Those data indicated a steady increase in Neptune's 12-micron atmospheric ethane emission from 1985 to 2003, followed by a slight decrease in 2004. The simplest explanation for the intensity variation was an increase in stratospheric effective temperature from 155 K in 1985 to 176 K in 2003 (an average rate of 1.2 K/year), and subsequent decrease to 165 K in 2004 (uncertainties +/- 3 K). Later disk-resolved 12-micron images (Hammel et al. 2007, AJ 134, 637; Orton et al. 2007, AA 473, L5) showed Neptune's ethane emission arose mainly from two regions: emission distributed nearly uniformly around the planet's limb and emission near the south pole. Because much of the non-limb emission was confined to the near-polar region, seasonal variation may play some role in the long-term mid-infrared brightness variations: i.e., more of that region was revealed as Neptune neared solstice in 2005. We will report the results of an additional half decade of mid-infrared spectroscopic observations, from 2005 through 2009, using the Broadband Array Spectrograph System on the NASA Infrared Telescope Facility (IRTF). These post-solstice data should elucidate whether the variations are intrinsic, or due to changes in viewing angle. HBH acknowledges support from NASA grants NNX06AD12G and NNA07CN65A. This work was supported at The Aerospace Corporation by the Independent Research and Development Program. LSB acknowledges the support of Spectral Sciences, Inc. IR and D funding. We also gratefully acknowledge D. Kim (The Aerospace Corporation) for BASS technical support, as well as the support of IRTF staff and telescope operators. We recognize the significant cultural role of Mauna Kea within the indigenous Hawaiian community, and we appreciate the opportunity to conduct observations from this revered site.

  2. 75 FR 34929 - Safety Zones: Neptune Deep Water Port, Atlantic Ocean, Boston, MA

    Federal Register 2010, 2011, 2012, 2013, 2014

    2010-06-21

    ...-AA00 Safety Zones: Neptune Deep Water Port, Atlantic Ocean, Boston, MA AGENCY: Coast Guard, DHS. ACTION..., Boston, MA; Final Rule (USCG-2009-0589), to protect vessels from the hazard posed by the presence of the... read as follows: Sec. 165.T01-0542 Safety Zones: Neptune Deepwater Port, Atlantic Ocean, Boston, MA. (a...

  3. Oblateness, radius, and mean stratospheric temperature of Neptune from the 1985 August 20 occultation

    NASA Technical Reports Server (NTRS)

    Hubbard, W. B.; Nicholson, Philip D.; Lellouch, Emmanuel; Sicardy, Bruno; Brahic, Andre; Vilas, Faith

    1987-01-01

    The oblateness and equatorial radius of Neptune at the 1-microbar pressure level, together with the position angle of the projected spin axis, are the goals of a general oblate atmosphere model for Neptune employing a data ensemble obtained from the occultation of a bright IR star that provided accurate measurements of the limb position at these and several other stations. The observed reduction in central flash intensity is explained by a 150-135 K temperature decrease as pressure rises from 1 to 400 microbar. Attention is given to the implications of these oblateness results for models of the Neptune interior.

  4. 40 CFR 436.380 - Applicability; description of the graphite subcategory.

    Code of Federal Regulations, 2011 CFR

    2011-07-01

    ... graphite subcategory. 436.380 Section 436.380 Protection of Environment ENVIRONMENTAL PROTECTION AGENCY (CONTINUED) EFFLUENT GUIDELINES AND STANDARDS MINERAL MINING AND PROCESSING POINT SOURCE CATEGORY Graphite Subcategory § 436.380 Applicability; description of the graphite subcategory. The provisions of this subpart...

  5. 40 CFR 436.380 - Applicability; description of the graphite subcategory.

    Code of Federal Regulations, 2012 CFR

    2012-07-01

    ... graphite subcategory. 436.380 Section 436.380 Protection of Environment ENVIRONMENTAL PROTECTION AGENCY... Graphite Subcategory § 436.380 Applicability; description of the graphite subcategory. The provisions of this subpart are applicable to the mining and processing of naturally occurring graphite. ...

  6. 40 CFR 436.240 - Applicability; description of the diatomite subcategory.

    Code of Federal Regulations, 2011 CFR

    2011-07-01

    ... diatomite subcategory. 436.240 Section 436.240 Protection of Environment ENVIRONMENTAL PROTECTION AGENCY (CONTINUED) EFFLUENT GUIDELINES AND STANDARDS MINERAL MINING AND PROCESSING POINT SOURCE CATEGORY Diatomite Subcategory § 436.240 Applicability; description of the diatomite subcategory. The provisions of this subpart...

  7. 40 CFR 436.240 - Applicability; description of the diatomite subcategory.

    Code of Federal Regulations, 2010 CFR

    2010-07-01

    ... diatomite subcategory. 436.240 Section 436.240 Protection of Environment ENVIRONMENTAL PROTECTION AGENCY (CONTINUED) EFFLUENT GUIDELINES AND STANDARDS MINERAL MINING AND PROCESSING POINT SOURCE CATEGORY Diatomite Subcategory § 436.240 Applicability; description of the diatomite subcategory. The provisions of this subpart...

  8. 40 CFR 436.380 - Applicability; description of the graphite subcategory.

    Code of Federal Regulations, 2010 CFR

    2010-07-01

    ... graphite subcategory. 436.380 Section 436.380 Protection of Environment ENVIRONMENTAL PROTECTION AGENCY (CONTINUED) EFFLUENT GUIDELINES AND STANDARDS MINERAL MINING AND PROCESSING POINT SOURCE CATEGORY Graphite Subcategory § 436.380 Applicability; description of the graphite subcategory. The provisions of this subpart...

  9. Neptune's New Dark Vortex: Aerosol Properties from Optical Data

    NASA Astrophysics Data System (ADS)

    Tollefson, J.; Luszcz-Cook, S.; Wong, M. H.; De Pater, I.

    2016-12-01

    Over the past year, amateur and professional astronomers alike have monitored the appearance of a new dark vortex on Neptune, dubbed SDS-2015 for "southern dark spot discovered in 2015" (Wong et al. 2016; CBET 4278). The discovery of SDS-2015 is fortuitous, being one of only five dark spots observed on Neptune since Voyager 2 imaged the Great Dark Spot (Smith et al. 1989, Science 246, 1422). A companion abstract (Wong et al., this meeting) will present Hubble Space Telescope images of SDS-2015, showcasing the discovery of the vortex in September 2015 and subsequent observations in May 2016. These observations span the optical regime. Longer wavelengths track bright companion clouds thought to form as air is diverted around SDS-2015. Shorter wavelengths reveal the dark spot itself. Combined, these data probe the vertical extent of the dark spot and Neptune's surrounding upper atmosphere. We present preliminary radiative transfer analyses of SDS-2015 using our multispectral data. Our model is the same as that in Luszcz-Cook et al. (2016, Icarus 276, 52) but extended to optical wavelengths. Prior to this work, little was known about the composition and vertical extent of Neptune's dark spots. Only data at optical wavelengths reveal these vortices, suggesting they consist of clearings in the background of fine, evenly-distributed haze particle. Alternatively, the spots may consist of low-albedo aerosols, causing their apparent darkness. Radiative transfer modeling is also one way to determine the vortex top altitude. Simulations of the Great Dark Spot by Stratman et al. (2001, Icarus 151, 275) found that the vortex top altitude is coupled to the brightness of companion clouds, where cloud opacity weakened as the top of the vortex reached higher into the tropopause region. The modeling presented here will compare these hypotheses and provide the first glimpses into the vertical structure of SDS-2015.

  10. Neptune's Discovery: Le Verrier, Adams, and the Assignment of Credit

    NASA Astrophysics Data System (ADS)

    Sheehan, William

    2011-01-01

    As one of the most significant achievements of 19th century astronomy, the discovery of Neptune has been the subject of a vast literature. A large part of this literature--beginning with the period immediately after the optical discovery in Berlin--has been the obsession with assigning credit to the two men who attempted to calculate the planet's position (and initially this played out against the international rivalry between France and England). Le Verrier and Adams occupied much different positions in the Scientific Establishments of their respective countries; had markedly different personalities; and approached the investigation using different methods. A psychiatrist and historian of astronomy tries to provide some new contexts to the familiar story of the discovery of Neptune, and argues that the personalities of these two men played crucial roles in their approaches to the problem they set themselves and the way others reacted to their stimuli. Adams had features of high-functioning autism, while Le Verrier's domineering, obsessive, orderly personality--though it allowed him to be immensely productive--eventually led to serious difficulties with his peers (and an outright revolt). Though it took extraordinary smarts to calculate the position of Neptune, the discovery required social skills that these men lacked--and thus the process to discovery was more bumbling and adventitious than it might have been. The discovery of Neptune occurred at a moment when astronomy was changing from that of heroic individuals to team collaborations involving multiple experts, and remains an object lesson in the sociological aspects of scientific endeavor.

  11. 40 CFR 436.130 - Applicability; description of the borax subcategory.

    Code of Federal Regulations, 2011 CFR

    2011-07-01

    ... borax subcategory. 436.130 Section 436.130 Protection of Environment ENVIRONMENTAL PROTECTION AGENCY (CONTINUED) EFFLUENT GUIDELINES AND STANDARDS MINERAL MINING AND PROCESSING POINT SOURCE CATEGORY Borax Subcategory § 436.130 Applicability; description of the borax subcategory. The provisions of this subpart are...

  12. 40 CFR 436.130 - Applicability; description of the borax subcategory.

    Code of Federal Regulations, 2010 CFR

    2010-07-01

    ... borax subcategory. 436.130 Section 436.130 Protection of Environment ENVIRONMENTAL PROTECTION AGENCY (CONTINUED) EFFLUENT GUIDELINES AND STANDARDS MINERAL MINING AND PROCESSING POINT SOURCE CATEGORY Borax Subcategory § 436.130 Applicability; description of the borax subcategory. The provisions of this subpart are...

  13. TOWARD THE FORMATION OF CARBONACEOUS REFRACTORY MATTER IN HIGH TEMPERATURE HYDROCARBON-RICH ATMOSPHERES OF EXOPLANETS UPON MICROMETEOROID IMPACT

    DOE Office of Scientific and Technical Information (OSTI.GOV)

    Dangi, Beni B.; Kim, Yong S.; Krasnokutski, Serge A.

    2015-05-20

    We report on laboratory simulation experiments mimicking the chemical processing of model atmospheres of exoplanets containing C3 and C4 hydrocarbons at moderate temperatures of 400 K upon interaction of catalytic surfaces of micrometeoroids. By utilizing an ultrasonic levitator device and heating singly levitated particles under simulated microgravity conditions, Raman spectroscopy is utilized as a non-invasive tool to probe on line and in situ the conversion of C3 and C4 hydrocarbons to refractory carbonaceous matter on the surfaces of levitated particles. Secondary Ion Mass Spectrometry and electron microscopic imaging were also conducted to gain further insight into the elementary composition andmore » structures of the refractories formed. Our results provide compelling evidence that in the presence of a catalytic surface, which can be supplied in the form of micrometeoroids and atmospheric dust particles, hydrocarbon gases present in the atmospheres of exoplanets can be converted to refractory, carbon-rich carbonaceous matter of mainly graphitic structure with a carbon content of at least 90% at elevated temperatures. This finding might explain the low methane to carbon monoxide (CH{sub 4}–CO) ratio in the hot Neptune GJ 436b, where the abundant methane photochemically converts to higher order hydrocarbons and ultimately to refractory graphite-like carbon in the presence of a silicon surface.« less

  14. 40 CFR 436.130 - Applicability; description of the borax subcategory.

    Code of Federal Regulations, 2013 CFR

    2013-07-01

    ... borax subcategory. 436.130 Section 436.130 Protection of Environment ENVIRONMENTAL PROTECTION AGENCY... Borax Subcategory § 436.130 Applicability; description of the borax subcategory. The provisions of this subpart are applicable to the processing of borate minerals. Borax obtained from brine lakes is regulated...

  15. 40 CFR 436.130 - Applicability; description of the borax subcategory.

    Code of Federal Regulations, 2012 CFR

    2012-07-01

    ... borax subcategory. 436.130 Section 436.130 Protection of Environment ENVIRONMENTAL PROTECTION AGENCY... Borax Subcategory § 436.130 Applicability; description of the borax subcategory. The provisions of this subpart are applicable to the processing of borate minerals. Borax obtained from brine lakes is regulated...

  16. 40 CFR 436.130 - Applicability; description of the borax subcategory.

    Code of Federal Regulations, 2014 CFR

    2014-07-01

    ... borax subcategory. 436.130 Section 436.130 Protection of Environment ENVIRONMENTAL PROTECTION AGENCY... Borax Subcategory § 436.130 Applicability; description of the borax subcategory. The provisions of this subpart are applicable to the processing of borate minerals. Borax obtained from brine lakes is regulated...

  17. Dynamic compression of water to 700 GPa: single- and double shock experiments on Sandia's Z machine, first principles simulations, and structure of water planets

    NASA Astrophysics Data System (ADS)

    Mattsson, Thomas R.

    2011-11-01

    Significant progress has over the last few years been made in high energy density physics (HEDP) by executing high-precision multi-Mbar experiments and performing first-principles simulations for elements ranging from carbon [1] to xenon [2]. The properties of water under HEDP conditions are of particular importance in planetary science due to the existence of ice-giants like Neptune and Uranus. Modeling the two planets, as well as water-rich exoplanets, requires knowing the equation of state (EOS), the pressure as a function of density and temperature, of water with high accuracy. Although extensive density functional theory (DFT) simulations have been performed for water under planetary conditions [3] experimental validation has been lacking. Accessing thermodynamic states along planetary isentropes in dynamic compression experiments is challenging because the principal Hugoniot follows a significantly different path in the phase diagram. In this talk, we present experimental data for dynamic compression of water up to 700 GPa, including in a regime of the phase-diagram intersected by the Neptune isentrope and water-rich models for the exoplanet GJ436b. The data was obtained on the Z-accelerator at Sandia National Laboratories by performing magnetically accelerated flyer plate impact experiments measuring both the shock and re-shock in the sample. The high accuracy makes it possible for the data to be used for detailed model validation: the results validate first principles based thermodynamics as a reliable foundation for planetary modeling and confirm the fine effect of including nuclear quantum effects on the shock pressure. Sandia National Laboratories is a multiprogram laboratory managed and operated by Sandia Corporation, a wholly owned subsidiary of Lockheed Martin Corporation, for the U.S. Department of Energy's National Nuclear Security Administration under Contract No. DE-AC04-94AL85000. [4pt] [1] M.D. Knudson, D.H. Dolan, and M.P. Desjarlais, SCIENCE

  18. 40 CFR 436.380 - Applicability; description of the graphite subcategory.

    Code of Federal Regulations, 2013 CFR

    2013-07-01

    ... 40 Protection of Environment 31 2013-07-01 2013-07-01 false Applicability; description of the graphite subcategory. 436.380 Section 436.380 Protection of Environment ENVIRONMENTAL PROTECTION AGENCY (CONTINUED) EFFLUENT GUIDELINES AND STANDARDS (CONTINUED) MINERAL MINING AND PROCESSING POINT SOURCE CATEGORY Graphite Subcategory § 436.380...

  19. 40 CFR 436.380 - Applicability; description of the graphite subcategory.

    Code of Federal Regulations, 2014 CFR

    2014-07-01

    ... 40 Protection of Environment 30 2014-07-01 2014-07-01 false Applicability; description of the graphite subcategory. 436.380 Section 436.380 Protection of Environment ENVIRONMENTAL PROTECTION AGENCY (CONTINUED) EFFLUENT GUIDELINES AND STANDARDS (CONTINUED) MINERAL MINING AND PROCESSING POINT SOURCE CATEGORY Graphite Subcategory § 436.380...

  20. 48 CFR 436.574 - Control of erosion, sedimentation, and pollution.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ..., sedimentation, and pollution. 436.574 Section 436.574 Federal Acquisition Regulations System DEPARTMENT OF... 436.574 Control of erosion, sedimentation, and pollution. The contracting officer shall insert the clause at 452.236-74, Control of Erosion, Sedimentation and Pollution, if there is a need for applying...

  1. 48 CFR 436.574 - Control of erosion, sedimentation, and pollution.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ..., sedimentation, and pollution. 436.574 Section 436.574 Federal Acquisition Regulations System DEPARTMENT OF... 436.574 Control of erosion, sedimentation, and pollution. The contracting officer shall insert the clause at 452.236-74, Control of Erosion, Sedimentation and Pollution, if there is a need for applying...

  2. 48 CFR 436.574 - Control of erosion, sedimentation, and pollution.

    Code of Federal Regulations, 2013 CFR

    2013-10-01

    ..., sedimentation, and pollution. 436.574 Section 436.574 Federal Acquisition Regulations System DEPARTMENT OF... 436.574 Control of erosion, sedimentation, and pollution. The contracting officer shall insert the clause at 452.236-74, Control of Erosion, Sedimentation and Pollution, if there is a need for applying...

  3. 48 CFR 436.574 - Control of erosion, sedimentation, and pollution.

    Code of Federal Regulations, 2014 CFR

    2014-10-01

    ..., sedimentation, and pollution. 436.574 Section 436.574 Federal Acquisition Regulations System DEPARTMENT OF... 436.574 Control of erosion, sedimentation, and pollution. The contracting officer shall insert the clause at 452.236-74, Control of Erosion, Sedimentation and Pollution, if there is a need for applying...

  4. 48 CFR 436.574 - Control of erosion, sedimentation, and pollution.

    Code of Federal Regulations, 2012 CFR

    2012-10-01

    ..., sedimentation, and pollution. 436.574 Section 436.574 Federal Acquisition Regulations System DEPARTMENT OF... 436.574 Control of erosion, sedimentation, and pollution. The contracting officer shall insert the clause at 452.236-74, Control of Erosion, Sedimentation and Pollution, if there is a need for applying...

  5. Absolute spectrophotometry of Titan, Uranus, and Neptune 3500-10,500 A

    NASA Technical Reports Server (NTRS)

    Neff, J. S.; Humm, D. C.; Bergstralh, J. T.; Cochran, A. L.; Cochran, W. D.; Barker, E. S.; Tull, R. G.

    1984-01-01

    The present absolute measurements of Titan, Uranus and Neptune geometric albedo spectra in the 3500-10,500 A range have a resolution of about 7 A, together with high SNR, in virtue of the exceptional effeciency of the spectrograph and Reticon detector employed. The high precision and spectral resolution of the data, which are in excellent agreement with the Uranus albedo measurements of Lockwood et al. (1983), make possible quantitative measurements of the effects of Raman scattering by H2 in the Uranus and Neptune atmospheres.

  6. 10 CFR 436.17 - Establishing energy or water cost data.

    Code of Federal Regulations, 2010 CFR

    2010-01-01

    ... 10 Energy 3 2010-01-01 2010-01-01 false Establishing energy or water cost data. 436.17 Section 436.17 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS Methodology and Procedures for Life Cycle Cost Analyses § 436.17 Establishing energy or water cost data. (a...

  7. 10 CFR 436.17 - Establishing energy or water cost data.

    Code of Federal Regulations, 2014 CFR

    2014-01-01

    ... 10 Energy 3 2014-01-01 2014-01-01 false Establishing energy or water cost data. 436.17 Section 436.17 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS Methodology and Procedures for Life Cycle Cost Analyses § 436.17 Establishing energy or water cost data. (a...

  8. 10 CFR 436.17 - Establishing energy or water cost data.

    Code of Federal Regulations, 2012 CFR

    2012-01-01

    ... 10 Energy 3 2012-01-01 2012-01-01 false Establishing energy or water cost data. 436.17 Section 436.17 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS Methodology and Procedures for Life Cycle Cost Analyses § 436.17 Establishing energy or water cost data. (a...

  9. Starspots and Activity of the Flare Star GJ 1243

    NASA Astrophysics Data System (ADS)

    Savanov, I. S.; Dmitrienko, E. S.

    2018-04-01

    The photometric variability of the uniqueMdwarf flare star GJ 1243 (KIC 9726699) is investigated using the most complete set of observationalmaterial obtained with the Kepler Space Telescope. The analysis is based on 49 487 individual brightness measurements obtained during an interval of 1460 days (nearly four years). The periodicity of the brightness variations with the period P phot = 0.59261 ± 0.00060d is confirmed. The temperature inhomogeneities on the stellar surface reconstructed from the light curve are used to drive maps of these surface-temperature inhomogeneities (of the filling factor f). The resulting maps are used to determine the positions of active regions. Analysis of the surface-temperature maps for GJ 1243 led to the conclusion that the positions of spots on the stellar surface displayed appreciable evolution during the analyzed time interval. The maximum value for the lower limit on the differentialrotation parameter ΔΩ is 0.0022 rad/day. This more accurate estimate of ΔΩ is lower than the values presented earlier by Davenport et al. [1] (0.0058 and 0.0036 rad/day), due to the more accurate account of variations in the positions of the most active longitude in the current study. However, the differentialrotation estimate obtained in [1] using a method based on fitting the evolution of spots using twodimensional Gaussian functions essentially coincides with the new estimate presented here. The fractional area of the total spotted surface S of the star during the observing interval considered varied from 7 to 2%. The amplitude of the brightness variability of the star slowly decreased, varying in the range 1.6-0.5%. Overall, the position of GJ 1243 in spottedness-age, spottedness-rotation period, and spottedness-Rossby number diagrams agrees very well with the general character of the dependences displayed in earlier studies of M dwarfs.

  10. Progress on the NEPTUNE Canada Seismograph Network

    NASA Astrophysics Data System (ADS)

    Rogers, G. C.; Meldrum, R. D.; Heesemann, M.; Mulder, T. L.; Brillon, C. D.; Cassidy, J. F.

    2012-12-01

    NEPTUNE Canada is the world's first deep-sea regional multi-disciplinary scientific cabled ocean observatory. In the fall of 2007 an 800 kilometer ring of powered fiber optic cable was laid on the seafloor over the northern part of the Juan de Fuca plate and connected to a shore facility near Port Alberni on Vancouver Island. In September 2009, three broadband OBS packages were deployed in the form of a large triangle with apexes at mid plate near ODP 1027 (water depth of 2654m) and two sites on the continental slope, near ODP 889 (1256m) and Barkley Canyon (396m). The broadband systems comprise a broadband seismometer and strong motion accelerometer in a spherical titanium case surficially buried in a caisson backfilled with glass beads. Noise levels observed are as expected with the spectra being similar to, or quieter than, coastal seismograph stations in approximately the 10 to 20 second period range. The OBS's have higher noise levels at longer periods where ocean swells and the resultant infragravity waves dominate the noise spectra, and in the 1-10 Hz bandwidth typically used for locating local earthquakes. The shallowest site at Barkley Canyon has the highest noise levels. A small array, about 6 km in maximum dimension, is under construction on the Endeavour segment of the Juan de Fuca Ridge to record earthquake activity in the vicinity of the many NEPTUNE Canada multi-disciplinary ridge experiments. Two short period instruments were installed there in 2010. A broadband instrument and two additional short period instruments are planned to complete the initial ridge array. Even though the NEPTUNE Canada seismograph network is not yet complete, measured by the use of its data, it is a success already. The data are routinely used along with data from land seismographs of the Canadian National Seismograph Network for locating earthquakes in the region. However, the smallest seismic arrivals picked on the land stations cannot be routinely picked on the OBS

  11. Neptune False Color Image of Haze

    NASA Technical Reports Server (NTRS)

    1989-01-01

    This false color photograph of Neptune was made from Voyager 2 images taken through three filters: blue, green, and a filter that passes light at a wavelength that is absorbed by methane gas. Thus, regions that appear white or bright red are those that reflect sunlight before it passes through a large quantity of methane. The image reveals the presence of a ubiquitous haze that covers Neptune in a semitransparent layer. Near the center of the disk, sunlight passes through the haze and deeper into the atmosphere, where some wavelengths are absorbed by methane gas, causing the center of the image to appear less red. Near the edge of the planet, the haze scatters sunlight at higher altitude, above most of the methane, causing the bright red edge around the planet. By measuring haze brightness at several wavelengths, scientists are able to estimate the thickness of the haze and its ability to scatter sunlight. The image is among the last full disk photos that Voyager 2 took before beginning its endless journey into interstellar space. The Voyager Mission is conducted by JPL for NASA's Office of Space Science and Applications.

  12. Binaries in Transneptunian Resonances: Evidence for Slow Migration of Neptune?

    NASA Technical Reports Server (NTRS)

    Noll, Keith

    2012-01-01

    A distinguishing feature of trans neptunian objects (TNO) is the high fraction that arc binary. This is particularly true for the Cold Classicals (CC), objects in lowe and low i orbits concentrated between the 3:2 and 2: 1 mean-motion resonances. CCs have other physical markers: red colors, high albedos, and equal-mass binaries. The CCs appear to be a coherent and physically distinct population of planetesimals that has survived to the present with their physical properties relatively unaltered. Their spatial concentration between 39.4 and 47.7 AU has made identification of the CCs as a physical group possible. However, objects that started out as CCs arc almost certainly 1101 limited to this one dynamical niche. We can, therefore, use the measurable physical properties of CCs as tracers of Neptune-driven dynamical mixing in the Kuiper Belt. As Neptune migrated, its mean-motion resonances preceded it into the planetesimal disk. The efficiency of capture into mean motion resonances depends on the smoothness of Neptune's migration and the local population available to be captured. The two strongest resonances, the 3:2 at 39.4 AU and 2: 1 at 47.7 AU, straddle the core repository of the physically distinct CCs, providing a unique opportunity to test the details of Neptune's migration. Smooth migration should result in a measurable difference between the 3:2 and 2:1 with low inclination 2:1s having a red, binary population mirroring that of the CC itself while the 3:2 will be less contaminated. Alternative models with rapid migration would generate a more homogeneous result.

  13. 42 CFR 436.308 - Medically needy coverage of individuals under age 21.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... THE VIRGIN ISLANDS Optional Coverage of the Medically Needy § 436.308 Medically needy coverage of... (b) of this section: (1) Who would not be covered under the mandatory medically needy group of... nursing facility services are provided under the plan to individuals within the age group selected under...

  14. 10 CFR 436.42 - Evaluation of Life-Cycle Cost Effectiveness.

    Code of Federal Regulations, 2011 CFR

    2011-01-01

    ... the life-cycle cost analysis method in part 436, subpart A, of title 10 of the Code of Federal... 10 Energy 3 2011-01-01 2011-01-01 false Evaluation of Life-Cycle Cost Effectiveness. 436.42... PROGRAMS Agency Procurement of Energy Efficient Products § 436.42 Evaluation of Life-Cycle Cost...

  15. Dynamical evolution of a fictitious population of binary Neptune Trojans

    NASA Astrophysics Data System (ADS)

    Brunini, Adrián

    2018-03-01

    We present numerical simulations of the evolution of a synthetic population of Binary Neptune Trojans, under the influence of the solar perturbations and tidal friction (the so-called Kozai cycles and tidal friction evolution). Our model includes the dynamical influence of the four giant planets on the heliocentric orbit of the binary centre of mass. In this paper, we explore the evolution of initially tight binaries around the Neptune L4 Lagrange point. We found that the variation of the heliocentric orbital elements due to the libration around the Lagrange point introduces significant changes in the orbital evolution of the binaries. Collisional processes would not play a significant role in the dynamical evolution of Neptune Trojans. After 4.5 × 109 yr of evolution, ˜50 per cent of the synthetic systems end up separated as single objects, most of them with slow diurnal rotation rate. The final orbital distribution of the surviving binary systems is statistically similar to the one found for Kuiper Belt Binaries when collisional evolution is not included in the model. Systems composed by a primary and a small satellite are more fragile than the ones composed by components of similar sizes.

  16. 48 CFR 436.602 - Selection of firms for architect-engineer contracts.

    Code of Federal Regulations, 2013 CFR

    2013-10-01

    ... architect-engineer contracts. 436.602 Section 436.602 Federal Acquisition Regulations System DEPARTMENT OF AGRICULTURE SPECIAL CATEGORIES OF CONTRACTING CONSTRUCTION AND ARCHITECT-ENGINEER CONTRACTS Architect-Engineer Service 436.602 Selection of firms for architect-engineer contracts. ...

  17. 48 CFR 436.602 - Selection of firms for architect-engineer contracts.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... architect-engineer contracts. 436.602 Section 436.602 Federal Acquisition Regulations System DEPARTMENT OF AGRICULTURE SPECIAL CATEGORIES OF CONTRACTING CONSTRUCTION AND ARCHITECT-ENGINEER CONTRACTS Architect-Engineer Service 436.602 Selection of firms for architect-engineer contracts. ...

  18. 48 CFR 436.602 - Selection of firms for architect-engineer contracts.

    Code of Federal Regulations, 2012 CFR

    2012-10-01

    ... architect-engineer contracts. 436.602 Section 436.602 Federal Acquisition Regulations System DEPARTMENT OF AGRICULTURE SPECIAL CATEGORIES OF CONTRACTING CONSTRUCTION AND ARCHITECT-ENGINEER CONTRACTS Architect-Engineer Service 436.602 Selection of firms for architect-engineer contracts. ...

  19. 48 CFR 436.602 - Selection of firms for architect-engineer contracts.

    Code of Federal Regulations, 2014 CFR

    2014-10-01

    ... architect-engineer contracts. 436.602 Section 436.602 Federal Acquisition Regulations System DEPARTMENT OF AGRICULTURE SPECIAL CATEGORIES OF CONTRACTING CONSTRUCTION AND ARCHITECT-ENGINEER CONTRACTS Architect-Engineer Service 436.602 Selection of firms for architect-engineer contracts. ...

  20. 48 CFR 436.602 - Selection of firms for architect-engineer contracts.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... architect-engineer contracts. 436.602 Section 436.602 Federal Acquisition Regulations System DEPARTMENT OF AGRICULTURE SPECIAL CATEGORIES OF CONTRACTING CONSTRUCTION AND ARCHITECT-ENGINEER CONTRACTS Architect-Engineer Service 436.602 Selection of firms for architect-engineer contracts. ...

  1. 10 CFR 436.17 - Establishing energy or water cost data.

    Code of Federal Regulations, 2013 CFR

    2013-01-01

    ... period is the product of water costs in the base year as established under § 436.17(a), or as calculated... 10 Energy 3 2013-01-01 2013-01-01 false Establishing energy or water cost data. 436.17 Section 436.17 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS...

  2. Cuckoo in the Nest: The Fate of the Original Moons of Neptune

    NASA Astrophysics Data System (ADS)

    Cuk, Matija; Hamilton, Douglas P.

    2016-10-01

    Neptune's moon Triton is the largest captured satellite in the solar system, as indicated by its inclined retrograde orbit. The most likely mechanism for its capture is binary disruption, which ejected its former binary companion and placed Triton on a large, eccentric orbit around Neptune (Agnor and Hamilton 2006). While the tides would in principle circularize Triton's orbit (Goldreich et al. 1989), Triton's early orbit would have evolved much faster through interactions with preexisting moons of Neptune (Cuk and Gladman 2005). Assuming that the pre-existing moons of Neptune were similar to those of Uranus, analytical estimates are unclear on which outcome is most likely during moon-moon scattering. Cuk and Gladman (2005) suggested that collisions among the regular moons happen first, while Nogueira et al. (2011) find that collisions between Triton and an old moon, or an ejection should happen first. Here we use the general purpose (T+U) symplectic integrator to explore this short-lived epoch of orbit crossing in the Neptunian system. Our preliminary results indicate that Triton might have collided with one of the preexisting moons of Neptune before the regular satellites could have been destroyed in mutual collisions. Goldreich et al. (1989) claimed that a collision with a moon larger than Miranda would destroy Triton and therefore could be ruled out. However, using modern collisional disruption estimated from Stewart and Leinhardt (2012), we find that Triton could have accreted a 1000-km moon at relevant velocities without being disrupted. The product of this merger would have a much tighter orbit as the accreted moon would not have been retrograde like Triton. At the meeting we will present a more detailed exploration of possible post-capture configurations, and report quantitative probabilities for different outcomes of this exciting and violent episode of Triton's history.

  3. NEPTUNE'S DYNAMIC ATMOSPHERE FROM KEPLER K2 OBSERVATIONS: IMPLICATIONS FOR BROWN DWARF LIGHT CURVE ANALYSES.

    PubMed

    Simon, Amy A; Rowe, Jason F; Gaulme, Patrick; Hammel, Heidi B; Casewell, Sarah L; Fortney, Jonathan J; Gizis, John E; Lissauer, Jack J; Morales-Juberias, Raul; Orton, Glenn S; Wong, Michael H; Marley, Mark S

    2016-02-01

    Observations of Neptune with the Kepler Space Telescope yield a 49 day light curve with 98% coverage at a 1 minute cadence. A significant signature in the light curve comes from discrete cloud features. We compare results extracted from the light curve data with contemporaneous disk-resolved imaging of Neptune from the Keck 10-m telescope at 1.65 microns and Hubble Space Telescope visible imaging acquired nine months later. This direct comparison validates the feature latitudes assigned to the K2 light curve periods based on Neptune's zonal wind profile, and confirms observed cloud feature variability. Although Neptune's clouds vary in location and intensity on short and long timescales, a single large discrete storm seen in Keck imaging dominates the K2 and Hubble light curves; smaller or fainter clouds likely contribute to short-term brightness variability. The K2 Neptune light curve, in conjunction with our imaging data, provides context for the interpretation of current and future brown dwarf and extrasolar planet variability measurements. In particular we suggest that the balance between large, relatively stable, atmospheric features and smaller, more transient, clouds controls the character of substellar atmospheric variability. Atmospheres dominated by a few large spots may show inherently greater light curve stability than those which exhibit a greater number of smaller features.

  4. 40 CFR 436.60 - Applicability; description of the asphaltic mineral subcategory.

    Code of Federal Regulations, 2012 CFR

    2012-07-01

    ... asphaltic mineral subcategory. 436.60 Section 436.60 Protection of Environment ENVIRONMENTAL PROTECTION AGENCY (CONTINUED) EFFLUENT GUIDELINES AND STANDARDS (CONTINUED) MINERAL MINING AND PROCESSING POINT SOURCE CATEGORY Asphaltic Mineral Subcategory § 436.60 Applicability; description of the asphaltic...

  5. 40 CFR 436.60 - Applicability; description of the asphaltic mineral subcategory.

    Code of Federal Regulations, 2013 CFR

    2013-07-01

    ... asphaltic mineral subcategory. 436.60 Section 436.60 Protection of Environment ENVIRONMENTAL PROTECTION AGENCY (CONTINUED) EFFLUENT GUIDELINES AND STANDARDS (CONTINUED) MINERAL MINING AND PROCESSING POINT SOURCE CATEGORY Asphaltic Mineral Subcategory § 436.60 Applicability; description of the asphaltic...

  6. 40 CFR 436.60 - Applicability; description of the asphaltic mineral subcategory.

    Code of Federal Regulations, 2014 CFR

    2014-07-01

    ... asphaltic mineral subcategory. 436.60 Section 436.60 Protection of Environment ENVIRONMENTAL PROTECTION AGENCY (CONTINUED) EFFLUENT GUIDELINES AND STANDARDS (CONTINUED) MINERAL MINING AND PROCESSING POINT SOURCE CATEGORY Asphaltic Mineral Subcategory § 436.60 Applicability; description of the asphaltic...

  7. 10 CFR 436.17 - Establishing energy or water cost data.

    Code of Federal Regulations, 2011 CFR

    2011-01-01

    ... escalation rate assumptions under § 436.14. When energy costs begin to accrue at a later time, subtract the... assumptions under § 436.14. When water costs begin to accrue at a later time, subtract the present value of... Methodology and Procedures for Life Cycle Cost Analyses § 436.17 Establishing energy or water cost data. (a...

  8. 48 CFR 436.605 - Government cost estimate for architect-engineer work.

    Code of Federal Regulations, 2012 CFR

    2012-10-01

    ... for architect-engineer work. 436.605 Section 436.605 Federal Acquisition Regulations System DEPARTMENT OF AGRICULTURE SPECIAL CATEGORIES OF CONTRACTING CONSTRUCTION AND ARCHITECT-ENGINEER CONTRACTS Architect-Engineer Service 436.605 Government cost estimate for architect-engineer work. The contracting...

  9. 48 CFR 436.605 - Government cost estimate for architect-engineer work.

    Code of Federal Regulations, 2013 CFR

    2013-10-01

    ... for architect-engineer work. 436.605 Section 436.605 Federal Acquisition Regulations System DEPARTMENT OF AGRICULTURE SPECIAL CATEGORIES OF CONTRACTING CONSTRUCTION AND ARCHITECT-ENGINEER CONTRACTS Architect-Engineer Service 436.605 Government cost estimate for architect-engineer work. The contracting...

  10. 48 CFR 436.605 - Government cost estimate for architect-engineer work.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... for architect-engineer work. 436.605 Section 436.605 Federal Acquisition Regulations System DEPARTMENT OF AGRICULTURE SPECIAL CATEGORIES OF CONTRACTING CONSTRUCTION AND ARCHITECT-ENGINEER CONTRACTS Architect-Engineer Service 436.605 Government cost estimate for architect-engineer work. The contracting...

  11. 48 CFR 436.605 - Government cost estimate for architect-engineer work.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... for architect-engineer work. 436.605 Section 436.605 Federal Acquisition Regulations System DEPARTMENT OF AGRICULTURE SPECIAL CATEGORIES OF CONTRACTING CONSTRUCTION AND ARCHITECT-ENGINEER CONTRACTS Architect-Engineer Service 436.605 Government cost estimate for architect-engineer work. The contracting...

  12. 48 CFR 436.605 - Government cost estimate for architect-engineer work.

    Code of Federal Regulations, 2014 CFR

    2014-10-01

    ... for architect-engineer work. 436.605 Section 436.605 Federal Acquisition Regulations System DEPARTMENT OF AGRICULTURE SPECIAL CATEGORIES OF CONTRACTING CONSTRUCTION AND ARCHITECT-ENGINEER CONTRACTS Architect-Engineer Service 436.605 Government cost estimate for architect-engineer work. The contracting...

  13. 42 CFR 436.110 - Individuals receiving cash assistance.

    Code of Federal Regulations, 2014 CFR

    2014-10-01

    ... 42 Public Health 4 2014-10-01 2014-10-01 false Individuals receiving cash assistance. 436.110 Section 436.110 Public Health CENTERS FOR MEDICARE & MEDICAID SERVICES, DEPARTMENT OF HEALTH AND HUMAN SERVICES (CONTINUED) MEDICAL ASSISTANCE PROGRAMS ELIGIBILITY IN GUAM, PUERTO RICO, AND THE VIRGIN ISLANDS...

  14. 10 CFR Appendix A to Part 436... - [Reserved

    Code of Federal Regulations, 2013 CFR

    2013-01-01

    ... 10 Energy 3 2013-01-01 2013-01-01 false [Reserved] A Appendix A to Part 436-Energy Conservation Standards for General Operations Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS Appendix A to Part 436—Energy Conservation Standards for General Operations...

  15. 10 CFR Appendix A to Part 436... - [Reserved

    Code of Federal Regulations, 2014 CFR

    2014-01-01

    ... 10 Energy 3 2014-01-01 2014-01-01 false [Reserved] A Appendix A to Part 436-Energy Conservation Standards for General Operations Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS Appendix A to Part 436—Energy Conservation Standards for General Operations...

  16. 10 CFR Appendix A to Part 436... - [Reserved

    Code of Federal Regulations, 2011 CFR

    2011-01-01

    ... 10 Energy 3 2011-01-01 2011-01-01 false [Reserved] A Appendix A to Part 436-Energy Conservation Standards for General Operations Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS Appendix A to Part 436—Energy Conservation Standards for General Operations...

  17. 10 CFR Appendix A to Part 436... - [Reserved

    Code of Federal Regulations, 2012 CFR

    2012-01-01

    ... 10 Energy 3 2012-01-01 2012-01-01 false [Reserved] A Appendix A to Part 436-Energy Conservation Standards for General Operations Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS Appendix A to Part 436—Energy Conservation Standards for General Operations...

  18. 10 CFR Appendix A to Part 436... - [Reserved

    Code of Federal Regulations, 2010 CFR

    2010-01-01

    ... 10 Energy 3 2010-01-01 2010-01-01 false [Reserved] A Appendix A to Part 436-Energy Conservation Standards for General Operations Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS Appendix A to Part 436—Energy Conservation Standards for General Operations...

  19. Building a Geologic Map of Neptune's Moon Triton

    NASA Astrophysics Data System (ADS)

    Martin, E. S.; Patthoff, D. A.; Bland, M. T.; Watters, T. R.; Collins, G. C.; Becker, T.

    2018-06-01

    Triton serves as a bridge between KBOs and icy satellites, and characterization of its terrains is important for advancing comparative planetological studies. We aim to create a geologic map of the Neptune-facing side of Triton at a scale of 1:5M.

  20. The Phase Space Structure Near Neptune Resonances in the Kuiper Belt

    NASA Technical Reports Server (NTRS)

    Malhotra, Renu

    1996-01-01

    The Solar system beyond Neptune is believed to house a population of small primordial bodies left over from the planet formation process. The region up to heliocentric distance -50 AU (a.k.a. the Kuiper Belt) may be the source of the observed short-period comets. In this region, the phase space structure near orbital resonances with Neptune is of special interest for the long-term stability of orbits. There is reason to believe that a significant fraction (perhaps most) of the Kuiper Belt objects reside preferentially in these resonance locations. This paper describes the dynamics of small objects near the major orbital resonances with Neptune. Estimates of the widths of stable resonance zones as well as the properties of resonant orbits are obtained from the circular, planar restricted three-body model. Although this model does not contain the full complexity of the long-term orbital dynamics of Kuiper Belt objects subject to the full N-body perturbations of all the planets, it does provide a baseline for the phase space structure and properties of resonant orbits in the trans-Neptunian Solar system.

  1. 40 CFR 436.60 - Applicability; description of the asphaltic mineral subcategory.

    Code of Federal Regulations, 2011 CFR

    2011-07-01

    ... asphaltic mineral subcategory. 436.60 Section 436.60 Protection of Environment ENVIRONMENTAL PROTECTION AGENCY (CONTINUED) EFFLUENT GUIDELINES AND STANDARDS MINERAL MINING AND PROCESSING POINT SOURCE CATEGORY Asphaltic Mineral Subcategory § 436.60 Applicability; description of the asphaltic mineral subcategory. The...

  2. 40 CFR 436.60 - Applicability; description of the asphaltic mineral subcategory.

    Code of Federal Regulations, 2010 CFR

    2010-07-01

    ... asphaltic mineral subcategory. 436.60 Section 436.60 Protection of Environment ENVIRONMENTAL PROTECTION AGENCY (CONTINUED) EFFLUENT GUIDELINES AND STANDARDS MINERAL MINING AND PROCESSING POINT SOURCE CATEGORY Asphaltic Mineral Subcategory § 436.60 Applicability; description of the asphaltic mineral subcategory. The...

  3. Monitoring Active Atmospheres on Uranus and Neptune

    NASA Astrophysics Data System (ADS)

    Rages, Kathy

    2009-07-01

    We propose Snapshot observations of Uranus and Neptune to monitor changes in their atmospheres on time scales of weeks and months, as we have been doing for the past seven years. Previous Hubble Space Telescope observations {including previous Snapshot programs 8634, 10170, 10534, and 11156}, together with near-IR images obtained using adaptive optics on the Keck Telescope, reveal both planets to be dynamic worlds which change on time scales ranging from hours to {terrestrial} years. Uranus equinox occurred in December 2007, and the northern hemisphere is becoming fully visible for the first time since the early 1960s. HST observations during the past several years {Hammel et al. 2005, Icarus 175, 284 and references therein} have revealed strongly wavelength-dependent latitudinal structure, the presence of numerous visible-wavelength cloud features in the northern hemisphere, at least one very long-lived discrete cloud in the southern hemisphere, and in 2006 the first clearly defined dark spot seen on Uranus. Long-term ground-based observations {Lockwood and Jerzekiewicz, 2006, Icarus 180, 442; Hammel and Lockwood 2007, Icarus 186, 291} reveal seasonal brightness changes that seem to demand the appearance of a bright northern polar cap within the next few years. Recent HST and Keck observations of Neptune {Sromovsky et al. 2003, Icarus 163, 256 and references therein} show a general increase in activity at south temperate latitudes until 2004, when Neptune returned to a rather Voyager-like appearance with discrete bright spots rather than active latitude bands. Further Snapshot observations of these two dynamic planets will elucidate the nature of long-term changes in their zonal atmospheric bands and clarify the processes of formation, evolution, and dissipation of discrete albedo features.

  4. 40 CFR 436.150 - Applicability; description of the sodium sulfate subcategory.

    Code of Federal Regulations, 2012 CFR

    2012-07-01

    ... sodium sulfate subcategory. 436.150 Section 436.150 Protection of Environment ENVIRONMENTAL PROTECTION... SOURCE CATEGORY Sodium Sulfate Subcategory § 436.150 Applicability; description of the sodium sulfate subcategory. The provisions of this subpart are applicable to the processing of sodium sulfate. Sodium sulfate...

  5. 40 CFR 436.150 - Applicability; description of the sodium sulfate subcategory.

    Code of Federal Regulations, 2011 CFR

    2011-07-01

    ... sodium sulfate subcategory. 436.150 Section 436.150 Protection of Environment ENVIRONMENTAL PROTECTION... Sodium Sulfate Subcategory § 436.150 Applicability; description of the sodium sulfate subcategory. The provisions of this subpart are applicable to the processing of sodium sulfate. Sodium sulfate obtained from...

  6. 40 CFR 436.150 - Applicability; description of the sodium sulfate subcategory.

    Code of Federal Regulations, 2013 CFR

    2013-07-01

    ... sodium sulfate subcategory. 436.150 Section 436.150 Protection of Environment ENVIRONMENTAL PROTECTION... SOURCE CATEGORY Sodium Sulfate Subcategory § 436.150 Applicability; description of the sodium sulfate subcategory. The provisions of this subpart are applicable to the processing of sodium sulfate. Sodium sulfate...

  7. 40 CFR 436.150 - Applicability; description of the sodium sulfate subcategory.

    Code of Federal Regulations, 2014 CFR

    2014-07-01

    ... sodium sulfate subcategory. 436.150 Section 436.150 Protection of Environment ENVIRONMENTAL PROTECTION... SOURCE CATEGORY Sodium Sulfate Subcategory § 436.150 Applicability; description of the sodium sulfate subcategory. The provisions of this subpart are applicable to the processing of sodium sulfate. Sodium sulfate...

  8. 40 CFR 436.150 - Applicability; description of the sodium sulfate subcategory.

    Code of Federal Regulations, 2010 CFR

    2010-07-01

    ... sodium sulfate subcategory. 436.150 Section 436.150 Protection of Environment ENVIRONMENTAL PROTECTION... Sodium Sulfate Subcategory § 436.150 Applicability; description of the sodium sulfate subcategory. The provisions of this subpart are applicable to the processing of sodium sulfate. Sodium sulfate obtained from...

  9. 40 CFR 436.180 - Applicability; description of the phosphate rock subcategory.

    Code of Federal Regulations, 2013 CFR

    2013-07-01

    ... phosphate rock subcategory. 436.180 Section 436.180 Protection of Environment ENVIRONMENTAL PROTECTION... SOURCE CATEGORY Phosphate Rock Subcategory § 436.180 Applicability; description of the phosphate rock... bearing rock, ore or earth for the phosphate content. [43 FR 9809, Mar. 10, 1978] ...

  10. 40 CFR 436.180 - Applicability; description of the phosphate rock subcategory.

    Code of Federal Regulations, 2012 CFR

    2012-07-01

    ... phosphate rock subcategory. 436.180 Section 436.180 Protection of Environment ENVIRONMENTAL PROTECTION... SOURCE CATEGORY Phosphate Rock Subcategory § 436.180 Applicability; description of the phosphate rock... bearing rock, ore or earth for the phosphate content. [43 FR 9809, Mar. 10, 1978] ...

  11. 40 CFR 436.180 - Applicability; description of the phosphate rock subcategory.

    Code of Federal Regulations, 2014 CFR

    2014-07-01

    ... phosphate rock subcategory. 436.180 Section 436.180 Protection of Environment ENVIRONMENTAL PROTECTION... SOURCE CATEGORY Phosphate Rock Subcategory § 436.180 Applicability; description of the phosphate rock... bearing rock, ore or earth for the phosphate content. [43 FR 9809, Mar. 10, 1978] ...

  12. An overabundance of low-density Neptune-like planets

    NASA Astrophysics Data System (ADS)

    Cubillos, Patricio; Erkaev, Nikolai V.; Juvan, Ines; Fossati, Luca; Johnstone, Colin P.; Lammer, Helmut; Lendl, Monika; Odert, Petra; Kislyakova, Kristina G.

    2017-04-01

    We present a uniform analysis of the atmospheric escape rate of Neptune-like planets with estimated radius and mass (restricted to Mp < 30 M⊕). For each planet, we compute the restricted Jeans escape parameter, Λ, for a hydrogen atom evaluated at the planetary mass, radius, and equilibrium temperature. Values of Λ ≲ 20 suggest extremely high mass-loss rates. We identify 27 planets (out of 167) that are simultaneously consistent with hydrogen-dominated atmospheres and are expected to exhibit extreme mass-loss rates. We further estimate the mass-loss rates (Lhy) of these planets with tailored atmospheric hydrodynamic models. We compare Lhy to the energy-limited (maximum-possible high-energy driven) mass-loss rates. We confirm that 25 planets (15 per cent of the sample) exhibit extremely high mass-loss rates (Lhy > 0.1 M⌖ Gyr-1), well in excess of the energy-limited mass-loss rates. This constitutes a contradiction, since the hydrogen envelopes cannot be retained given the high mass-loss rates. We hypothesize that these planets are not truly under such high mass-loss rates. Instead, either hydrodynamic models overestimate the mass-loss rates, transit-timing-variation measurements underestimate the planetary masses, optical transit observations overestimate the planetary radii (due to high-altitude clouds), or Neptunes have consistently higher albedos than Jupiter planets. We conclude that at least one of these established estimations/techniques is consistently producing biased values for Neptune planets. Such an important fraction of exoplanets with misinterpreted parameters can significantly bias our view of populations studies, like the observed mass-radius distribution of exoplanets for example.

  13. 42 CFR 436.608 - Applications for other benefits.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... 42 Public Health 4 2010-10-01 2010-10-01 false Applications for other benefits. 436.608 Section... General Financial Eligibility Requirements and Options § 436.608 Applications for other benefits. (a) As a... obtain any annuities, pensions, and retirement and disability benefits to which they are entitled, unless...

  14. 42 CFR 436.608 - Applications for other benefits.

    Code of Federal Regulations, 2014 CFR

    2014-10-01

    ... 42 Public Health 4 2014-10-01 2014-10-01 false Applications for other benefits. 436.608 Section... General Financial Eligibility Requirements and Options § 436.608 Applications for other benefits. (a) As a... to obtain any annuities, pensions, and retirement and disability benefits to which they are entitled...

  15. 40 CFR 436.180 - Applicability; description of the phosphate rock subcategory.

    Code of Federal Regulations, 2011 CFR

    2011-07-01

    ... phosphate rock subcategory. 436.180 Section 436.180 Protection of Environment ENVIRONMENTAL PROTECTION... Phosphate Rock Subcategory § 436.180 Applicability; description of the phosphate rock subcategory. The provisions of this subpart are applicable to the mining and the processing of phosphate bearing rock, ore or...

  16. 40 CFR 436.180 - Applicability; description of the phosphate rock subcategory.

    Code of Federal Regulations, 2010 CFR

    2010-07-01

    ... phosphate rock subcategory. 436.180 Section 436.180 Protection of Environment ENVIRONMENTAL PROTECTION... Phosphate Rock Subcategory § 436.180 Applicability; description of the phosphate rock subcategory. The provisions of this subpart are applicable to the mining and the processing of phosphate bearing rock, ore or...

  17. 40 CFR 436.190 - Applicability; description of the Frasch sulfur subcategory.

    Code of Federal Regulations, 2012 CFR

    2012-07-01

    ... Frasch sulfur subcategory. 436.190 Section 436.190 Protection of Environment ENVIRONMENTAL PROTECTION... SOURCE CATEGORY Frasch Sulfur Subcategory § 436.190 Applicability; description of the Frasch sulfur subcategory. The provisions of this subpart are applicable to the processing of sulfur on shore and in marshes...

  18. 40 CFR 436.190 - Applicability; description of the Frasch sulfur subcategory.

    Code of Federal Regulations, 2010 CFR

    2010-07-01

    ... Frasch sulfur subcategory. 436.190 Section 436.190 Protection of Environment ENVIRONMENTAL PROTECTION... Frasch Sulfur Subcategory § 436.190 Applicability; description of the Frasch sulfur subcategory. The provisions of this subpart are applicable to the processing of sulfur on shore and in marshes and estuaries...

  19. 40 CFR 436.190 - Applicability; description of the Frasch sulfur subcategory.

    Code of Federal Regulations, 2014 CFR

    2014-07-01

    ... Frasch sulfur subcategory. 436.190 Section 436.190 Protection of Environment ENVIRONMENTAL PROTECTION... SOURCE CATEGORY Frasch Sulfur Subcategory § 436.190 Applicability; description of the Frasch sulfur subcategory. The provisions of this subpart are applicable to the processing of sulfur on shore and in marshes...

  20. 40 CFR 436.190 - Applicability; description of the Frasch sulfur subcategory.

    Code of Federal Regulations, 2011 CFR

    2011-07-01

    ... Frasch sulfur subcategory. 436.190 Section 436.190 Protection of Environment ENVIRONMENTAL PROTECTION... Frasch Sulfur Subcategory § 436.190 Applicability; description of the Frasch sulfur subcategory. The provisions of this subpart are applicable to the processing of sulfur on shore and in marshes and estuaries...

  1. 40 CFR 436.190 - Applicability; description of the Frasch sulfur subcategory.

    Code of Federal Regulations, 2013 CFR

    2013-07-01

    ... Frasch sulfur subcategory. 436.190 Section 436.190 Protection of Environment ENVIRONMENTAL PROTECTION... SOURCE CATEGORY Frasch Sulfur Subcategory § 436.190 Applicability; description of the Frasch sulfur subcategory. The provisions of this subpart are applicable to the processing of sulfur on shore and in marshes...

  2. Significance of large Neptune-crossing objects for terrestrial catastrophism

    NASA Astrophysics Data System (ADS)

    Steel, D.

    2014-07-01

    Over the past few decades a substantial number of objects have been discovered on orbits beyond Neptune (i.e. transneptunian objects, in various sub-classes), crossing Neptune's orbit (here: the Neptune-crossers of interest), and also others crossing the orbits of any or all of the jovian planets (i.e. Centaurs). These range in size from tens of kilometres across to hundreds of kilometres and more. Although formally classified as minor planets/asteroids, plus a few dwarf planets, the physical reality of these objects is that they are giant comets. That is, they seem to be composed largely of ices and if they were to enter the inner solar system then they would demonstrate the commonly-observed behaviour of comets such as outgassing, and the formation of ion and dust tails. Commonly-observed cometary behaviour, however, also includes fragmentation events and sometimes complete disintegration for no apparent cause (such as tidal disruption or thermal stresses). One might therefore wonder what the implications would be for life on Earth and terrestrial catastrophism if and when one of these objects, say 100 to 500 kilometres in size, dropped into a short-period orbit with perihelion distance (q) less than 1 au; or even q ˜ 5 au, given what Jupiter's gravity might do to it. How often might such events occur? One way to address that question would be to conduct numerical integrations of suitable test orbits and identify how often small-q orbits result, but this comes up against the problem of identifying very-infrequent events (with annual probabilities per object perhaps of order 10^{-12}-10^{-10}. For example, Emel'yanenko et al. [1] recently followed test orbits for approximately 5 × 10^{14} particle-years (8,925 objects with 200 clones of each, for 300 Myr) but because these were selected on the basis of initial values of q only below 36 (rather than ˜30) au many were not immediately Neptune-crossers; however, many test particles did eventually migrate into small

  3. 16 CFR 436.10 - Other laws and rules.

    Code of Federal Regulations, 2011 CFR

    2011-01-01

    ... franchisees outside of the disclosure document under Section 5 of the Federal Trade Commission Act. The... franchise practices laws of any state or local government, except to the extent of any inconsistency with part 436. A law is not inconsistent with part 436 if it affords prospective franchisees equal or...

  4. 16 CFR 436.10 - Other laws and rules.

    Code of Federal Regulations, 2014 CFR

    2014-01-01

    ... franchisees outside of the disclosure document under Section 5 of the Federal Trade Commission Act. The... franchise practices laws of any state or local government, except to the extent of any inconsistency with part 436. A law is not inconsistent with part 436 if it affords prospective franchisees equal or...

  5. 16 CFR 436.10 - Other laws and rules.

    Code of Federal Regulations, 2010 CFR

    2010-01-01

    ... franchisees outside of the disclosure document under Section 5 of the Federal Trade Commission Act. The... franchise practices laws of any state or local government, except to the extent of any inconsistency with part 436. A law is not inconsistent with part 436 if it affords prospective franchisees equal or...

  6. 16 CFR 436.10 - Other laws and rules.

    Code of Federal Regulations, 2013 CFR

    2013-01-01

    ... franchisees outside of the disclosure document under Section 5 of the Federal Trade Commission Act. The... franchise practices laws of any state or local government, except to the extent of any inconsistency with part 436. A law is not inconsistent with part 436 if it affords prospective franchisees equal or...

  7. 16 CFR 436.10 - Other laws and rules.

    Code of Federal Regulations, 2012 CFR

    2012-01-01

    ... franchisees outside of the disclosure document under Section 5 of the Federal Trade Commission Act. The... franchise practices laws of any state or local government, except to the extent of any inconsistency with part 436. A law is not inconsistent with part 436 if it affords prospective franchisees equal or...

  8. The planets Uranus, Neptune, and Pluto (1971)

    NASA Technical Reports Server (NTRS)

    Palluconi, F. D.

    1972-01-01

    Design criteria relating to spacecraft intended to investigate the planets of Uranus, Neptune, and Pluto are presented. Assessments were made of the potential effects of environmental properties on vehicle performance. Pertinent data on the mass, radius, shape, mean density, rotational pole location, and mean orbital elements for the three planets are given in graphs and tables.

  9. VizieR Online Data Catalog: Broadband photometry of Neptune from K2 (Rowe+, 2017)

    NASA Astrophysics Data System (ADS)

    Rowe, J. F.; Gaulme, P.; Lissauer, J. J.; Marley, M. S.; Simon, A. A.; Hammel, H. B.; Silva Aguirre, V.; Barclay, T.; Benomar, O.; Boumier, P.; Caldwell, D. A.; Casewell, S. L.; Chaplin, W. J.; Colon, K. D.; Corsaro, E.; Davies, G. R.; Fortney, J. J.; Garcia, R. A.; Gizis, J. E.; Haas, M. R.; Mosser, B.; Schmider, F.-X.

    2017-08-01

    The K2 C3 field provided the first opportunity to observe the planet Neptune for up to 80 days with short-cadence (1 minute) sampling (the C3 campaign had an actual duration of 69.2 days, limited by on-board data storage). We were awarded sufficient pixel allocation from Guest Observer Programs GO3060 (PI: Rowe) and GO3057 (PI: Gaulme) to continuously monitor Neptune for 49 days. Short-cadence target pixel files were obtained from Mikulski Archive for Space Telescopes (MAST). The Neptune short-cadence subraster was spread across 161 FITS files. Each file contained 1 column of time-series pixel data. Each target pixel file contains observations starting on 2014 November 15 and finishing on 2015 January 18. (1 data file).

  10. Uranus' and Neptune's Clouds as Revealed by UKIRT/UIST Observations

    NASA Astrophysics Data System (ADS)

    Irwin, Patrick G. J.; Teanby, N. A.; Davis, G. R.

    2009-09-01

    In 2006, 2007 and 2008 observations of the near-infrared spectrum of Uranus were made with the UIST instrument of the UK Infrared Telescope, covering the period of Uranus’ Northern Spring Equinox. A significant change in the visible appearance of Uranus occurred during this time with the southern polar zone at 45°S fading, while a corresponding zone at 45°N began to form. In addition the visibility of the equatorial zone increased. The observed spectra were fitted using the NEMESIS optimal estimation retrieval model to determine the variation in the latitudinal and vertical cloud structure during this time. Retrievals were conducted using both the methane absorption coefficients used in our previous analyses and also a newly available revised set of methane coefficients and significant differences were seen, which will be reported. During the Uranus observations in 2007, corresponding observations were also made of Neptune's near-infrared spectrum, albeit with substantially less spatial resolution. The spectra were nevertheless sufficient to retrieve the gross variation in Neptune's latitudinal-vertical cloud structure using both sets of methane absorption coefficients. The retrieved vertical-latitudinal cloud structure on Uranus and Neptune, observed with identical instrument setups, are directly compared and the similarities and differences will be presented and discussed.

  11. New Ca-Tims and La-Icp Analyses of GJ-1, Plesovice, and FC1 Reference Materials

    NASA Astrophysics Data System (ADS)

    Feldman, J. D.; Möller, A.; Walker, J. D.

    2014-12-01

    Laser ablation inductively coupled plasma mass spectrometry (LA-ICP-MS) U-Pb zircon geochronology relies on external reference standards to monitor and correct for different mass fractionation effects and instrument drift. Common zircon reference materials used within the community, including the KU Isotope Geochemistry Laboratory, are GJ-1 (207Pb/206Pb age: 608.53 +/- 0.37Ma; Jackson et al., 2004), Plesovice (337.13 +/- 0.37 Ma; Slama et al., 2008), and FC-1 (1099.0 +/-0.6 Ma; Paces and Miller, 1993). The age distribution of zircon reference material varies slightly from sample fraction to sample fraction, and the published results for GJ-1 are slightly discordant. As a result, using the published data for the distributed standard splits can lead to small systematic variations when comparing datasets from different labs, and more high precision data are needed to evaluate potential inhomogeneity of sample splits used in different laboratories. Here we characterize these reference materials with cathodoluminescence, LA-ICP-MS traverses across grains, and high precision CA-TIMS to better constrain the ages and assess zoning of these standards, and present the data for comparison with other laboratories. Reducing systematic error by dating our own reference material lends confidence to our analyses and allows for inter-laboratory age reproducibility of unknowns. Additionally, the reduction in propagated uncertainties (especially in GJ-1, for which both the red and yellow variety will be analyzed) will be used to improve long-term reproducibility, comparisons between samples of similar age, detrital populations and composite pluton zircons. Jackson, S.E., et al., 2004, Chemical Geology, v. 211, p. 47-69. Paces, J.B. & Miller, J.D., 1993, Journal of Geophysical Research, v. 80, p. 13997-14013. Slama, J., et al., 2008, Chemical Geology, v. 249. p. 1-35.

  12. 33 CFR 165.T01-0542 - Safety Zones: Neptune Deepwater Port, Atlantic Ocean, Boston, MA.

    Code of Federal Regulations, 2010 CFR

    2010-07-01

    ... 33 Navigation and Navigable Waters 2 2010-07-01 2010-07-01 false Safety Zones: Neptune Deepwater Port, Atlantic Ocean, Boston, MA. 165.T01-0542 Section 165.T01-0542 Navigation and Navigable Waters... Guard District § 165.T01-0542 Safety Zones: Neptune Deepwater Port, Atlantic Ocean, Boston, MA. (a...

  13. Neptune's Southern Hemisphere

    NASA Technical Reports Server (NTRS)

    1989-01-01

    This photograph of Neptune's southern hemisphere was taken by the narrow-angle camera on NASA's Voyager 2 when the spacecraft was 4.2 million km (2.6 million miles) from the planet. The smallest features that can be seen are 38 km (24 miles) across. The almond-shaped structure at the left is a large cloud system that has been seen for several weeks. Internal details in the feature have become increasingly apparent as Voyager 2 has approached. Systems with similar shapes in Jupiter's atmosphere rotate about their centers, rolling in the local winds that increase toward the south. However, the wispy nature of the white central clouds in this Neptunian feature make confirmation of the system's rotation difficult. The Voyager Mission is conducted by JPL for NASA's Office of Space Science and Applications.

  14. Tidal interaction: A possible explanation for geysers and other fluid phenomena in the Neptune-Triton system

    NASA Technical Reports Server (NTRS)

    Kelly, W. D.; Wood, C. L.

    1993-01-01

    Discovery of geyser-like plumes on the surface of Triton was a highlight of Voyager 2's passage through the Neptune planetary system. Remarkable as these observations were, they were not entirely without precedent. Considering the confirmed predictions for the 1979 Voyager Jovian passage, it was logical to consider other solar system bodies beside Io where tidal effects could be a significant factor in surface processes. It was our intuition that the Neptune-Triton gravitational bond acting at high inclination to the Neptune equator and the fact that Neptune was a fluid body was significant oblateness would produce tidal and mechanical forces that could be transformed into thermal energy vented on Triton's surface. Prior to the Voyager flyby, others have noted that capture and evolution of Triton's orbit from extreme eccentricity to near circular state today would have resulted in significant tidal heating, but these analysts disregard current day forces. Our calculations indicate that the time varying forces between Neptune-Triton fall midway between those exerted in the Earth-Moon and Jupiter-Io systems, and considering the low level of other energy inputs, this source of internal energy should not be ignored when seeking an explanation for surface activity. In each planet-satellite case, residual or steady-state eccentricity causes time-varying stresses on internal satellite strata. In the case of Jupiter the residual eccentricity is due largely to Galilean satellite interactions, particularly Io-Europa, but in the case of Neptune-Triton, it is the effect of Triton's inclined orbit about an oblate primary.

  15. 10 CFR Appendix D to Part 436 - Energy Program Conservation Elements

    Code of Federal Regulations, 2013 CFR

    2013-01-01

    ... 10 Energy 3 2013-01-01 2013-01-01 false Energy Program Conservation Elements D Appendix D to Part 436 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS Pt. 436, App. D Appendix D to Part 436—Energy Program Conservation Elements (a) In all successful energy...

  16. 10 CFR Appendix D to Part 436 - Energy Program Conservation Elements

    Code of Federal Regulations, 2014 CFR

    2014-01-01

    ... 10 Energy 3 2014-01-01 2014-01-01 false Energy Program Conservation Elements D Appendix D to Part 436 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS Pt. 436, App. D Appendix D to Part 436—Energy Program Conservation Elements (a) In all successful energy...

  17. 10 CFR Appendix D to Part 436 - Energy Program Conservation Elements

    Code of Federal Regulations, 2011 CFR

    2011-01-01

    ... 10 Energy 3 2011-01-01 2011-01-01 false Energy Program Conservation Elements D Appendix D to Part 436 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS Pt. 436, App. D Appendix D to Part 436—Energy Program Conservation Elements (a) In all successful energy...

  18. 10 CFR Appendix D to Part 436 - Energy Program Conservation Elements

    Code of Federal Regulations, 2012 CFR

    2012-01-01

    ... 10 Energy 3 2012-01-01 2012-01-01 false Energy Program Conservation Elements D Appendix D to Part 436 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS Pt. 436, App. D Appendix D to Part 436—Energy Program Conservation Elements (a) In all successful energy...

  19. 10 CFR Appendix D to Part 436 - Energy Program Conservation Elements

    Code of Federal Regulations, 2010 CFR

    2010-01-01

    ... 10 Energy 3 2010-01-01 2010-01-01 false Energy Program Conservation Elements D Appendix D to Part 436 Energy DEPARTMENT OF ENERGY ENERGY CONSERVATION FEDERAL ENERGY MANAGEMENT AND PLANNING PROGRAMS Pt. 436, App. D Appendix D to Part 436—Energy Program Conservation Elements (a) In all successful energy...

  20. Discrete cloud structure on Neptune

    NASA Technical Reports Server (NTRS)

    Hammel, H. B.

    1989-01-01

    Recent CCD imaging data for the discrete cloud structure of Neptune shows that while cloud features at CH4-band wavelengths are manifest in the southern hemisphere, they have not been encountered in the northern hemisphere since 1986. A literature search has shown the reflected CH4-band light from the planet to have come from a single discrete feature at least twice in the last 10 years. Disk-integrated photometry derived from the imaging has demonstrated that a bright cloud feature was responsible for the observed 8900 A diurnal variation in 1986 and 1987.

  1. The near real time image navigation of pictures returned by Voyager 2 at Neptune

    NASA Technical Reports Server (NTRS)

    Underwood, Ian M.; Bachman, Nathaniel J.; Taber, William L.; Wang, Tseng-Chan; Acton, Charles H.

    1990-01-01

    The development of a process for performing image navigation in near real time is described. The process was used to accurately determine the camera pointing for pictures returned by the Voyager 2 spacecraft at Neptune Encounter. Image navigation improves knowledge of the pointing of an imaging instrument at a particular epoch by correlating the spacecraft-relative locations of target bodies in inertial space with the locations of their images in a picture taken at that epoch. More than 8,500 pictures returned by Voyager 2 at Neptune were processed in near real time. The results were used in several applications, including improving pointing knowledge for nonimaging instruments ('C-smithing'), making 'Neptune, the Movie', and providing immediate access to geometrical quantities similar to those traditionally supplied in the Supplementary Experiment Data Record.

  2. Chaotic Excitation and Tidal Damping in the GJ 876 System

    NASA Astrophysics Data System (ADS)

    Puranam, Abhijit; Batygin, Konstantin

    2018-04-01

    The M-dwarf GJ 876 is the closest known star to harbor a multi-planetary system. With three outer planets locked in a chaotic Laplace-type resonance and an appreciably eccentric short-period super-Earth, this system represents a unique exposition of extrasolar planetary dynamics. A key question that concerns the long-term evolution of this system, and the fate of close-in planets in general, is how the significant eccentricity of the inner-most planet is maintained against tidal circularization on timescales comparable to the age of the universe. Here, we employ stochastic secular perturbation theory and N-body simulations to show that the orbit of the inner-most planet is shaped by a delicate balance between extrinsic chaotic forcing and tidal dissipation. As such, the planet’s orbital eccentricity represents an indirect measure of its tidal quality factor. Based on the system’s present-day architecture, we estimate that the extrasolar super-Earth GJ 876 d has a tidal Q ∼ 104–105, a value characteristic of solar system gas giants.

  3. An Empirically-derived non-LTE XUV-Visible Spectral Synthesis Model of the M1 V Exoplanet Host Star GJ832

    NASA Astrophysics Data System (ADS)

    Linsky, Jeffrey; Fontenla, Juan; Witbrod, Jesse; France, Kevin

    2016-01-01

    GJ832 (HD 204961) is a nearby M1 V host star with two exoplanets: a Jovian mass planet and a super-Earth. We have obtained near-UV and far-UV spectra of GJ832 with the STIS and COS instruments on HST as part of the Cycle 19 MUSCLES pilot program (France et al. 2013). Our objective is to obtain the first accurate physical model for a representative M-dwarf host star in order to understand the stellar radiative emission at all wavelengths and to infer the radiation environment of their exoplanets that drives their atmospheric photochemistry.We have calculated a full non-LTE model for GJ 832 including the photosphere, chromosphere, transition region, and corona to fit the observed emission lines formed over a wide range of temperatures and the X-ray flux. Our one-dimensional semi-empirical model uses the Solar-Stellar Physical Modelling tools that are an offspring of the tools used by Fontenla and collaborators for computing solar models. For this model of GJ832, we calculate the populations of 52 atoms and ions and 20 molecules with 2 million spectral lines. We find excellent agreement with the observed H-alpha, CaII, MgII, CII, SiIV, CIV, and NV lines. Our model for GJ832 has a temperature minimum in the lower chromosphere much cooler than the Sun and then a steep temperature rise different from the Sun. The different thermal structure of GJ832 compared to the Sun results in the formation regions of the emission lines being different for the two stars. We also compute theradiative cooling rates as a function of height and temperature in the atmosphere of GJ832.This work is supported by grants from STScI to the University of Colorado.

  4. 42 CFR 436.601 - Application of financial eligibility methodologies.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... VIRGIN ISLANDS General Financial Eligibility Requirements and Options § 436.601 Application of financial... methodologies in determining financial eligibility of the following groups: (i) Qualified pregnant women and children under the mandatory categorically needy group under § 436.120; (ii) Low-income pregnant women...

  5. Ethane abundance on Neptune

    NASA Technical Reports Server (NTRS)

    Kostiuk, Theodor; Espenak, Fred; Romani, Paul; Zipoy, David; Goldstein, Jeff

    1990-01-01

    IR spectroscopic measurements of the C2H6 RR (4,5) emission line at 840.9764/cm have been used to infer Neptune's ethane mole fractions; while the resulting value is lower than that obtained by Orton et al. (1987), it lies within their 2-sigma error bounds. The present results are also found to require 2.0-5.8 times more ethane in the 0.02-2 mbar pressure region than predicted by the Romani and Atreya (1989) photochemical model. Better agreement is obtainable through a reduction of eddy mixing in the lower stratosphere and/or an increase of stratospheric temperature by more than 10 K above the 6-mbar level.

  6. 40 CFR 436.70 - Applicability; description of the asbestos and wollastonite subcategory.

    Code of Federal Regulations, 2014 CFR

    2014-07-01

    ... asbestos and wollastonite subcategory. 436.70 Section 436.70 Protection of Environment ENVIRONMENTAL... POINT SOURCE CATEGORY Asbestos and Wollastonite Subcategory § 436.70 Applicability; description of the asbestos and wollastonite subcategory. The provisions of this subpart are applicable to the processing of...

  7. 40 CFR 436.70 - Applicability; description of the asbestos and wollastonite subcategory.

    Code of Federal Regulations, 2013 CFR

    2013-07-01

    ... asbestos and wollastonite subcategory. 436.70 Section 436.70 Protection of Environment ENVIRONMENTAL... POINT SOURCE CATEGORY Asbestos and Wollastonite Subcategory § 436.70 Applicability; description of the asbestos and wollastonite subcategory. The provisions of this subpart are applicable to the processing of...

  8. 40 CFR 436.70 - Applicability; description of the asbestos and wollastonite subcategory.

    Code of Federal Regulations, 2011 CFR

    2011-07-01

    ... asbestos and wollastonite subcategory. 436.70 Section 436.70 Protection of Environment ENVIRONMENTAL... CATEGORY Asbestos and Wollastonite Subcategory § 436.70 Applicability; description of the asbestos and wollastonite subcategory. The provisions of this subpart are applicable to the processing of asbestos and...

  9. 40 CFR 436.70 - Applicability; description of the asbestos and wollastonite subcategory.

    Code of Federal Regulations, 2012 CFR

    2012-07-01

    ... asbestos and wollastonite subcategory. 436.70 Section 436.70 Protection of Environment ENVIRONMENTAL... POINT SOURCE CATEGORY Asbestos and Wollastonite Subcategory § 436.70 Applicability; description of the asbestos and wollastonite subcategory. The provisions of this subpart are applicable to the processing of...

  10. 40 CFR 436.70 - Applicability; description of the asbestos and wollastonite subcategory.

    Code of Federal Regulations, 2010 CFR

    2010-07-01

    ... asbestos and wollastonite subcategory. 436.70 Section 436.70 Protection of Environment ENVIRONMENTAL... CATEGORY Asbestos and Wollastonite Subcategory § 436.70 Applicability; description of the asbestos and wollastonite subcategory. The provisions of this subpart are applicable to the processing of asbestos and...

  11. Dynamics of the Trans-Neptune Region: Apsidal Waves in the Kuiper Belt

    NASA Technical Reports Server (NTRS)

    Ward, William R.; Hahn, Joseph M.

    1998-01-01

    The role of apsidal density waves propagating in a primordial trans-Neptune disk (i.e., Kuiper belt) is investigated. It is shown that Neptune launches apsidal waves at its secular resonance near 40 AU that propagate radially outward, deeper into the particle disk. The wavelength of apsidal waves is considerably longer than waves that might be launched at Lindblad resonances, because the pattern speed, g(sub s), resulting from the apsis precession of Neptune is much slower than its mean motion, Omega(sub s). If the early Kuiper belt had a sufficient surface density, sigma, the disk's wave response to Neptune's secular perturbation would have spread the disturbing torque radially over a collective scale lambda(sub *) approx. = r(2(mu)(sub d)Omega/ absolute value of r dg/dr)(sup 1/2), where mu(sub d)equivalent pi(sigma)r(exp 2)/(1 solar mass) and Omega(r) and g(r) are respectively the mean motion and precession frequency of the disk particles. This results in considerably smaller eccentricities at resonance than had the disk particles been treated as noninteracting test particles. Consequently, particles are less apt to be excited into planet-crossing orbits, implying that the erosion timescales reported by earlier test-particle simulations of the Kuiper belt may be underestimated. It is also shown that the torque the disk exerts upon the planet (due to its gravitational attraction for the disk's spiral wave pattern) damps the planet's eccentricity and further inhibits the planet's ability to erode the disk. Key words: celestial mechanics, stellar dynamics - comets: general minor planets, asteroids

  12. Neptune Clouds Showing Vertical Relief

    NASA Image and Video Library

    1996-01-29

    NASA's Voyager 2 high resolution color image, taken 2 hours before closest approach, provides obvious evidence of vertical relief in Neptune's bright cloud streaks. These clouds were observed at a latitude of 29 degrees north near Neptune's east terminator. The linear cloud forms are stretched approximately along lines of constant latitude and the sun is toward the lower left. The bright sides of the clouds which face the sun are brighter than the surrounding cloud deck because they are more directly exposed to the sun. Shadows can be seen on the side opposite the sun. These shadows are less distinct at short wavelengths (violet filter) and more distinct at long wavelengths (orange filter). This can be understood if the underlying cloud deck on which the shadow is cast is at a relatively great depth, in which case scattering by molecules in the overlying atmosphere will diffuse light into the shadow. Because molecules scatter blue light much more efficiently than red light, the shadows will be darkest at the longest (reddest) wavelengths, and will appear blue under white light illumination. The resolution of this image is 11 kilometers (6.8 miles per pixel) and the range is only 157,000 kilometers (98,000 miles). The width of the cloud streaks range from 50 to 200 kilometers (31 to 124 miles), and their shadow widths range from 30 to 50 kilometers (18 to 31 miles). Cloud heights appear to be of the order of 50 kilometers (31 miles). This corresponds to 2 scale heights. http://photojournal.jpl.nasa.gov/catalog/PIA00058

  13. 42 CFR 436.3 - Definitions and use of terms.

    Code of Federal Regulations, 2014 CFR

    2014-10-01

    ... 42 Public Health 4 2014-10-01 2014-10-01 false Definitions and use of terms. 436.3 Section 436.3 Public Health CENTERS FOR MEDICARE & MEDICAID SERVICES, DEPARTMENT OF HEALTH AND HUMAN SERVICES (CONTINUED) MEDICAL ASSISTANCE PROGRAMS ELIGIBILITY IN GUAM, PUERTO RICO, AND THE VIRGIN ISLANDS General...

  14. 42 CFR 436.201 - Individuals included in optional groups.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... 42 Public Health 4 2010-10-01 2010-10-01 false Individuals included in optional groups. 436.201... SERVICES (CONTINUED) MEDICAL ASSISTANCE PROGRAMS ELIGIBILITY IN GUAM, PUERTO RICO, AND THE VIRGIN ISLANDS Options for Coverage as Categorically Needy § 436.201 Individuals included in optional groups. (a) The...

  15. 42 CFR 436.229 - Optional targeted low-income children.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... 42 Public Health 4 2011-10-01 2011-10-01 false Optional targeted low-income children. 436.229... Options for Coverage as Categorically Needy Options for Coverage of Families and Children and Aged, Blind, and Disabled Individuals, Including Pregnant Women § 436.229 Optional targeted low-income children...

  16. 42 CFR 436.229 - Optional targeted low-income children.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... 42 Public Health 4 2010-10-01 2010-10-01 false Optional targeted low-income children. 436.229... Options for Coverage as Categorically Needy Options for Coverage of Families and Children and Aged, Blind, and Disabled Individuals, Including Pregnant Women § 436.229 Optional targeted low-income children...

  17. 42 CFR 436.229 - Optional targeted low-income children.

    Code of Federal Regulations, 2013 CFR

    2013-10-01

    ... 42 Public Health 4 2013-10-01 2013-10-01 false Optional targeted low-income children. 436.229... Options for Coverage as Categorically Needy Options for Coverage of Families and Children and Aged, Blind, and Disabled Individuals, Including Pregnant Women § 436.229 Optional targeted low-income children...

  18. 42 CFR 436.229 - Optional targeted low-income children.

    Code of Federal Regulations, 2012 CFR

    2012-10-01

    ... 42 Public Health 4 2012-10-01 2012-10-01 false Optional targeted low-income children. 436.229... Options for Coverage as Categorically Needy Options for Coverage of Families and Children and Aged, Blind, and Disabled Individuals, Including Pregnant Women § 436.229 Optional targeted low-income children...

  19. 42 CFR 436.229 - Optional targeted low-income children.

    Code of Federal Regulations, 2014 CFR

    2014-10-01

    ... 42 Public Health 4 2014-10-01 2014-10-01 false Optional targeted low-income children. 436.229... Options for Coverage as Categorically Needy Options for Coverage of Families and Children and Aged, Blind, and Disabled Individuals, Including Pregnant Women § 436.229 Optional targeted low-income children...

  20. SPITZER SPACE TELESCOPE MID-IR LIGHT CURVES OF NEPTUNE

    DOE Office of Scientific and Technical Information (OSTI.GOV)

    Stauffer, John; Rebull, Luisa; Carey, Sean J.

    2016-11-01

    We have used the Spitzer Space Telescope in 2016 February to obtain high cadence, high signal-to-noise, 17 hr duration light curves of Neptune at 3.6 and 4.5 μ m. The light curve duration was chosen to correspond to the rotation period of Neptune. Both light curves are slowly varying with time, with full amplitudes of 1.1 mag at 3.6 μ m and 0.6 mag at 4.5 μ m. We have also extracted sparsely sampled 18 hr light curves of Neptune at W1 (3.4 μ m) and W2 (4.6 μ m) from the Wide-feld Infrared Survey Explorer ( WISE )/ NEOWISEmore » archive at six epochs in 2010–2015. These light curves all show similar shapes and amplitudes compared to the Spitzer light curves but with considerable variation from epoch to epoch. These amplitudes are much larger than those observed with Kepler / K 2 in the visible (amplitude ∼0.02 mag) or at 845 nm with the Hubble Space Telescope ( HST ) in 2015 and at 763 nm in 2016 (amplitude ∼0.2 mag). We interpret the Spitzer and WISE light curves as arising entirely from reflected solar photons, from higher levels in Neptune’s atmosphere than for K 2. Methane gas is the dominant opacity source in Neptune’s atmosphere, and methane absorption bands are present in the HST 763 and 845 nm, WISE W1, and Spitzer 3.6 μ m filters.« less