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2017LPI....48.2597G | We find the area surrounding Wolf Crater has a composition more similar to highly evolved nonmare volcanic structures than typical lunar crustal rocks. | 2017-03-01T00:00:00Z | ['2017LPI....48.2597G'] | null | Investigating Evolved Compositions Around Wolf Crater | 2,017 | 0 | 0.06 | ['PUB_PDF'] | 0 | null |
2017LPI....48.1240R | NIRVSS spectra and images permit real time water ice monitoring as a function of depth while drilling in cryogenically cooled waterdoped lunar simulant. | 2017-03-01T00:00:00Z | ['2017LPI....48.1240R'] | null | Documenting Surface and SubSurface Volatiles While Drilling in Frozen Lunar Simulant | 2,017 | 0 | 0.1 | ['PUB_PDF'] | 0 | null |
2017LPI....48.1239P | We report the presence of rare Mgrich olivine veinlets and pyroxene veinlets in NWA 1109. They might have formed by shockinduced melting. | 2017-03-01T00:00:00Z | ['2017LPI....48.1239P'] | null | Forsteritic OlivineRich and PyroxeneRich Veinlets in the Brecciated Eucrite Northwest Africa 1109 | 2,017 | 0 | 0 | ['PUB_PDF'] | 0 | null |
2017LPI....48.1806C | We present evidence of reidite and ZrO2 in granular zircon within Muong Nongtype tektites from Thailand providing new insights into their genesis. | 2017-03-01T00:00:00Z | ['2017LPI....48.1806C'] | null | Reidite and ZrO2 in Muong Nongtype Australasian Tektites and the Significance of Granular Zircon in Siliceous Impact Melt | 2,017 | 0 | 0.1 | ['PUB_PDF'] | 0 | null |
2017LPI....48.2696M | A complete textural ad minerochemical description of the ungrouped chondrite NWA 10769 a meteorite related to the supra TFL chondrites is provided. | 2017-03-01T00:00:00Z | ['2017LPI....48.2696M'] | null | Northwest Africa 10769 An Ungrouped Chondrite Related to the SupraTFL Chondrites | 2,017 | 0 | 0.12 | ['PUB_PDF'] | 0 | null |
2017LPI....48.2200M | These spectra provides information about the deep atmosphere and surface of Venus but are difficult to interpret because of straylight from the dayside. | 2017-03-01T00:00:00Z | ['2017LPI....48.2200M'] | null | Derivation of Thermal Emission from VIRTIS on Venus Express 10001400 nm Spectra | 2,017 | 0 | 0 | ['PUB_PDF'] | 0 | null |
2017LPI....48.2680T | We developed a new absorptionphase nanotomography. Pristine carbonaceous chondrites have more complicated textures than expected from 2D observation. | 2017-03-01T00:00:00Z | ['2017LPI....48.2680T'] | null | A New Method of AbsorptionPhase Nanotomography for 3D Observation of MineralOrganicsWater Textures and Its Application to Pristine Carbonaceous Chondrites | 2,017 | 0 | 0 | ['PUB_PDF'] | 0 | null |
2017LPI....48.2479L | We derive the first mineral and FeO maps of the polar regions 5090 in latitude at 1 km per pixel using the LOLA normal albedo and continuumremoved SP data. | 2017-03-01T00:00:00Z | ['2017LPI....48.2479L'] | null | Mineralogy and Iron Content of the Lunar Polar Regions Using the Kaguya Spectral Profiler and the Lunar Orbiter Laser Altimeter | 2,017 | 0 | 0.19 | ['PUB_PDF'] | 1 | null |
2017LPI....48.1707T | We present a 6U CubeSat that will use a visible and thermal cameras to map Phobos and answer questions about surface striations composition and origins. | 2017-03-01T00:00:00Z | ['2017LPI....48.1707T'] | null | An Interplanetary Cubesat Mission to Phobos | 2,017 | 0 | 0.17 | ['PUB_PDF'] | 0 | null |
2017LPI....48.2083B | New thermal corrections of M3 data result in a prominent 2.95 micron absorption interpreted as H2O at all latitudes and local times. | 2017-03-01T00:00:00Z | ['2017LPI....48.2083B'] | null | A Prominent and Ubiquitous OHH2O Feature in Corrected Lunar Spectra | 2,017 | 0 | 0.17 | ['PUB_PDF'] | 0 | null |
2017LPI....48.1790L | Ideas are sought for scientific investigations in the frame of GER mission scenarios. Opportunities exist to shape the implementation of these scenarios. | 2017-03-01T00:00:00Z | ['2017LPI....48.1790L'] | null | Technical Challenges and Scientific Opportunities of Enabling International Access to the Far Side and Polar Regions for Humans and Robots from a Staging Post in the Lunar Vicinity | 2,017 | 0 | 0.06 | ['PUB_PDF'] | 0 | null |
2017LPI....48.2579R | Organic unknowns Is irradiation key Bonding isotopes. | 2017-03-01T00:00:00Z | ['2017LPI....48.2579R'] | null | Preliminary Isotopic Chemical and Microstructural Investigation of Irradiated Organic Dust Analogs | 2,017 | 0 | 0.06 | ['PUB_PDF'] | 0 | null |
2017LPI....48.1430V | Swath profile based morphological analysis of a fluvial valley on Mars TintoB is shown and found to be useful in the identification of old eroded valleys. | 2017-03-01T00:00:00Z | ['2017LPI....48.1430V'] | null | Swath Profile Analysis to Understand Martian Fluvial Valleys Morphology | 2,017 | 0 | 0.06 | ['PUB_PDF'] | 1 | null |
2017LPI....48.1241Z | Subsurface lowpressure boiling of postimpact water solutions causes accumulation of salts at depth and deposition of salty ice grains from plumes. | 2017-03-01T00:00:00Z | ['2017LPI....48.1241Z'] | null | Bright Salts on Ceres Aqueous Accumulation and Airborne Emplacement | 2,017 | 0 | 0.06 | ['PUB_PDF'] | 0 | null |
2017LPI....48.1146B | This investigation combines remote sensing observations across a wide spectral range to characterize shocked and crystalline anorthositic material on the Moon. | 2017-03-01T00:00:00Z | ['2017LPI....48.1146B'] | null | Investigating the Nature of Crystalline and Shocked Anorthosite on the Moon | 2,017 | 0 | 0.1 | ['PUB_PDF'] | 0 | null |
2017LPI....48.2203B | We are currently producing a series of HiRISE DTMs for volcanic features on Mars to facilitate detailed morphologic and topographic analyses. | 2017-03-01T00:00:00Z | ['2017LPI....48.2203B'] | null | HiRISE Digital Terrain Models of Volcanic Features on Mars | 2,017 | 0 | 0 | ['PUB_PDF'] | 0 | null |
2017LPI....48.1047S | An experimental assessment of the survival capabilities of sulfate reducing bacteria in simulated martian conditions. | 2017-03-01T00:00:00Z | ['2017LPI....48.1047S'] | null | An Experimental Assessment on the Effects of Variations in Sulfate Concentrations on Sulfate Reducing Bacteria in Simulated Martian Conditions | 2,017 | 0 | 0 | ['PUB_PDF'] | 0 | null |
2017LPI....48.2308A | This research describes a method for resolving the mass of small bodies during spacecraft flybys using deployed passive testmasses that are optically tracked. | 2017-03-01T00:00:00Z | ['2017LPI....48.2308A'] | null | Optical Gravimetry for Flyby Missions Parametric Study and Validation | 2,017 | 0 | 0 | ['PUB_PDF'] | 0 | null |
2017LPI....48.2209G | Alkali silica reactivity may have been significant in the weathering and erosional process of martian regolith. | 2017-03-01T00:00:00Z | ['2017LPI....48.2209G'] | null | Alkali Silica Reactivity a Problem on Earth a Solution on Mars | 2,017 | 0 | 0.06 | ['PUB_PDF'] | 1 | null |
2017LPI....48.2012D | Kinetic simulations including an observationsbased lunar Bfield model provide strong evidence that solar wind standoff has formed the Reiner Gamma swirls. | 2017-03-01T00:00:00Z | ['2017LPI....48.2012D'] | null | Fully Kinetic Simulations of the Solar Wind Interaction with Lunar Magnetic Anomalies Reiner Gamma and Swirl Formation | 2,017 | 0 | 0.17 | ['PUB_PDF'] | 1 | null |
2017LPI....48.2105A | Proposal to survey community to determine type and format of resources on high precision analyses to aid in public engagement. | 2017-03-01T00:00:00Z | ['2017LPI....48.2105A'] | null | Value of Sample Return and High Precision Analyses Need for a Resource of Compelling Stories Metaphors and Examples for Public Speakers | 2,017 | 0 | 0 | ['PUB_PDF'] | 0 | null |
2017LPI....48.1337H | A meltbearing impact breccia containing clasts of heterogeneous petrologic type thought to have formed within the structural floor of an impact crater. | 2017-03-01T00:00:00Z | ['2017LPI....48.1337H'] | null | LLChondrite Northwest Africa 6813 Sampling an ImpactCratered Asteroid | 2,017 | 0 | 0 | ['PUB_PDF'] | 0 | null |
2017AGUFMSA24A..04B | A highresolution version of the Kuehlungsborn Mechanistic general Circulation Model KMCM with resolved gravity waves GWs is employed to analyze the annual variation of GW activity in both hemispheres at middle and high latitudes. The geographical distributions of GW hotspots in the winter stratosphere are consistent with existing satellite data. Vertical profiles up to the lower thermosphere agree with groundbased measurements for both season. The model confirms the semiannual variation of GW energy in the upper mesosphere that was found previously in radarmeasurements in the northern hemisphere Furthermore the GW potential energy per unit mass during winter shows two maxima one around 5070 km and one around 80100 km. We interpret the upper maximum as a result of secondary GWs that are generated in the stratopause region due to the intermittent body forces of primary GWs. In a recent study we showed that these secondary GWs produce a significant eastward drag in the mesopause region during austral winter. This mechanism is found to be important in the northern winter as well. | 2017-12-01T00:00:00Z | ['2017AGUFMSA24A..04B'] | ['3334 Middle atmosphere dynamics', 'ATMOSPHERIC PROCESSES', '3369 Thermospheric dynamics', 'ATMOSPHERIC PROCESSES', '3384 Acoustic-gravity waves', 'ATMOSPHERIC PROCESSES', '2427 Ionosphere/atmosphere interactions', 'IONOSPHERE'] | Annual variation of gravitywave activity at middle and high latitudes in a highresolution GCM | 2,017 | 0 | 0 | null | 0 | null |
2017LPI....48.1045A | Acidification of a palaeosol sample from SW Egypt yields polymetallic and PSi glass spherules and grains of SiC Ti Snrich alloys and CN of unknown origin. | 2017-03-01T00:00:00Z | ['2017LPI....48.1045A'] | null | Polymetallic and Carbonaceous Debris in Palaeosol from the Libyan Desert Glass Strewn Field SW Egypt Evidence of a Cometary Impact | 2,017 | 0 | 0 | ['PUB_PDF'] | 0 | null |
2017LPI....48.2500A | These rocks from Iceland Vary in composition Help to study Mars. | 2017-03-01T00:00:00Z | ['2017LPI....48.2500A'] | null | The Mineralogic Variability of Icelandic Palagonites An Analog Study for Mars | 2,017 | 0 | 0.06 | ['PUB_PDF'] | 0 | null |
2017LPI....48.1438V | Detailed morphological and mineralogical mapping and study of very fresh craters on Moon. | 2017-03-01T00:00:00Z | ['2017LPI....48.1438V'] | null | Geological Mapping of a Simple Crater Case Study of Lichtenberg B | 2,017 | 0 | 0 | ['PUB_PDF'] | 0 | null |
2017LPI....48.2701R | We exposed calcium silicates and calcium carbonate for 42 days to Venus surface conditions using the Glenn Extreme Environment Rig GEER at NASAGRC. | 2017-03-01T00:00:00Z | ['2017LPI....48.2701R'] | null | The Stability of Calcium Silicates and Calcium Carbonate on the Surface of Venus | 2,017 | 0 | 0.22 | ['PUB_PDF'] | 3 | null |
2017LPI....48.3003C | Our experiments demonstrate that jarosite precipitates from halidebearing brine could preferentially incorporate substantial amount of Br rather than Cl. | 2017-03-01T00:00:00Z | ['2017LPI....48.3003C'] | null | Influences of Halogens on Jarosite Crystal Chemistry During Low Temperature FeOxidation Processes on Mars | 2,017 | 0 | 0.06 | ['PUB_PDF'] | 0 | null |
2017LPI....48.1532B | New solar wind observations and theory combined with Genesis solar wind data give improved knowledge of solar nebula composition. | 2017-03-01T00:00:00Z | ['2017LPI....48.1532B'] | null | Solar Nebula Composition Based on Solar Wind Data | 2,017 | 0 | 0.22 | ['PUB_PDF'] | 4 | null |
2017LPICo1967.4009A | The aim of this work is to compare the behavior under irradiation of solid and aqueous DLglyceraldehyde simulating prebiotic conditions. The results show the formation of sugarlike products of prebiotic significance as function of irradiation dose. | 2017-07-01T00:00:00Z | ['2017LPICo1967.4009A'] | null | Evaluation of Glyceraldehyde Under Simulated Prebiotic Conditions | 2,017 | 0 | 0.1 | ['PUB_PDF'] | 0 | null |
2017LPI....48.2602H | We measured the massdependent fractionation of Nd Sm Eu Gd Dy Er and Yb to a precision of around 0.03 amu for different terrestrial geostandards. | 2017-03-01T00:00:00Z | ['2017LPI....48.2602H'] | null | Defining the Baseline of the REE Stable Isotope Variations in Solar System Materials Earth | 2,017 | 0 | 0 | ['PUB_PDF'] | 0 | null |
2017LPI....48.1043P | The Astronomy in Chile Educator Ambassadors Program ACEAP is a program that brings astronomy educators to U.S. astronomy facilities in Chile. | 2017-03-01T00:00:00Z | ['2017LPI....48.1043P'] | null | Observatories at the Extreme My Chilean Telescopes and Southern Sky Experience | 2,017 | 0 | 0 | ['PUB_PDF'] | 0 | null |
2017LPI....48.2009K | We report the petrology of an AOA in Y793261 that preserves evidence of condensation at unusually high temperature combined with lowT interaction with gas. | 2017-03-01T00:00:00Z | ['2017LPI....48.2009K'] | null | UltraRefractory CalciumAluminumRich Inclusion in an AOA in CR Chondrite Yamato793261 | 2,017 | 0 | 0.06 | ['PUB_PDF'] | 1 | null |
2017LPICo1967.4112S | RNA world organisms could have used trimetaphosphate as energy source for thermodynamically unfavorable RNA polymerization. Using in vitro selection we show here that Lanthanides can serve as cofactors for ribozymecatalyzed RNA triphosphorylation. | 2017-07-01T00:00:00Z | ['2017LPICo1967.4112S'] | null | Lanthanide Cofactors for Triphosphorylation Ribozymes | 2,017 | 0 | 0.12 | ['PUB_PDF'] | 0 | null |
2017LPI....48.1333Q | A first model with Moons despinning and cooling histories explains the lunar fossil bulge and suggests a slow recession of the early Moon from the Earth. | 2017-03-01T00:00:00Z | ['2017LPI....48.1333Q'] | null | Formation of the Lunar Fossil Bulge and Its Implication for the Dynamics of the Early Earth and Moon | 2,017 | 0 | 0 | ['PUB_PDF'] | 0 | null |
2017LPI....48.2801M | Enceladus vents Sampling robots will fight through Supersonic winds. | 2017-03-01T00:00:00Z | ['2017LPI....48.2801M'] | null | Dynamic Pressure at Enceladus Vents and Implications for Vent and Conduit InSitu Studies | 2,017 | 0 | 0.17 | ['PUB_PDF'] | 0 | null |
2017LPI....48.2899D | We obtained spectra of 45P that allow measuring its volatile composition. The favorable Doppler shift 35 kms provided sensitive measures of CH4 and CO. | 2017-03-01T00:00:00Z | ['2017LPI....48.2899D'] | null | Compositional Study of Jupiter Family Comet 45PHondaMrkosPajdusakova Near Perihelion Using iSHELL at the NASAInfrared Telescope Facility | 2,017 | 0 | 0.1 | ['PUB_PDF'] | 0 | null |
2017LPI....48.1127H | Earthbased radar have potentials to study the instantaneous rotation rate and related planetary properties to high precision. | 2017-03-01T00:00:00Z | ['2017LPI....48.1127H'] | null | Potentials of Radar Speckle Tracking in Instantaneous Rotation Rate and Related Planetary Properties | 2,017 | 0 | 0 | ['PUB_PDF'] | 0 | null |
2017GCN.21173....1L | MASTERKislovodsk robotic telescope 2x4 square degrees MASTERNet httpobserv.pereplet.ru was pointed to the GRB170531B Evans et al. GCN 21171 12 sec after notice time and 452 sec after trigger time on 20170531 220944 UT. There is marginally seen optical transient at the position 19h 07m 32.03s 16d 25 10.4 with mOT19.00.5 The 5sigma upper limit is about 18.5mag The message may be cited. The observations made on zenit distance 64 degrees galaxy latitude b 11 degree. The moon 44 bright part below the horizon The Moon altitude is 6 degree. The sun altitude is 22.7 degree. The object can be observed till sunrise at 20170601 013050 . The message may be cited. | 2017-05-01T00:00:00Z | ['2017GCN.21173....1L'] | null | GRB 170531B MASTER Net OT detection | 2,017 | 0 | 0.06 | ['PUB_HTML'] | 0 | null |
2017LPI....48.2284H | Geologic mapping results for our study area and the evolution of geologic mapping and interpretations for the western valley system of Libya Montes. | 2017-03-01T00:00:00Z | ['2017LPI....48.2284H'] | null | Geologic Mapping of Western Libya Montes and Northern Tyrrhena Terra | 2,017 | 0 | 0 | ['PUB_PDF'] | 0 | null |
2017LPI....48.1887O | Thermal conductivity of sintered glass beads was measured in vacuum. Planetesimal thermal calculations were conducted with considering the measurement results. | 2017-03-01T00:00:00Z | ['2017LPI....48.1887O'] | null | Thermal Conductivity Measurement of Sintered Glass Beads and Implication for Thermal Evolution of Planetesimal | 2,017 | 0 | 0.1 | ['PUB_PDF'] | 0 | null |
2017LPI....48.1596X | This study shows the difference between lunar anorthite samples with a variety of shock effects using Raman Spectroscopy. | 2017-03-01T00:00:00Z | ['2017LPI....48.1596X'] | null | Raman Study of Shock Effects in Lunar Anorthite from the Apollo Missions | 2,017 | 0 | 0 | ['PUB_PDF'] | 0 | null |
2017LPI....48.1784N | We performed statistical investigation of the bulk chemical composition of Apollo 16 impact melt rocks only using major element. | 2017-03-01T00:00:00Z | ['2017LPI....48.1784N'] | null | Statistical Classification of Apollo 16 Impact Melt Using Major Element Compositions | 2,017 | 0 | 0 | ['PUB_PDF'] | 0 | null |
2017JDSO...13..585L | Reports are presented of lunar occultations of close double stars observed using video techniques. Included are cases where a determination of the position angle and separation of the pair can be made as well as instances where no duplicity has been observed of known or reported double stars. A number of double stars discovered as a result of an occultation are also included together with the light curves for the discovery event. | 2017-10-01T00:00:00Z | ['2017JDSO...13..585L'] | null | Lunar Occultation Observations of Double Stars x80x93 Report 6 | 2,017 | 0 | 0 | null | 0 | null |
2017nuco.confa0306T | Type Ia Supernovae SNe Ia are key objects for the present cosmology as the most mature standard candles. It is important to verify theoretical models of SN Ia explosions observationally. Since emissions from SN Ia are mainly drived by the radioactive sources generated in the explosion gammaray observations are the key for the study. We performed a soft gammaray observation of the nearby SN Ia SN2014J with the hard Xray detector HXD onboard Suzaku satellite at 77 2 days after the explosion. After careful treatments of Xray contaminations from ultraluminous Xray source in the M82 galaxy non Xray background events Cosmic Xray background emission and the Earths albedo we found gammaray signals are measured from SN2014J at 2 sigma confidence with the flux at 1.2 0.7 10SUP4SUP ph sSUP1SUP cmSUP2SUP in the 170250 keV band. The flux ratio between the continuum and the line from SUP56SUPCo is sensitive to the ejecta mass and might distinguish progenitor models between single and double degenerate scenarios. Our Suzaku data of continuum emission and line emission reported by INTEGRAL satellite has been examined with this relation but could not distinguish these models. However thanks to the high sensitivities of the HXD around 200 keV in the shorter exposure than INTEGRAL the Suzaku observations clearly exclude explosion models with heavier SUP56SUPNi mass than 1 solar mass. | 2017-01-01T00:00:00Z | ['2017nuco.confa0306T', '10.7566/JPSCP.14.010306'] | null | Soft Gammaray Observation of SN2014J with Suzaku | 2,017 | 0 | 0.19 | ['PUB_HTML'] | 0 | null |
2013APS..APRJ15006V | Current computational methods for the Dirac equation are prone to negative behavior such as fermion doubling instability and poor performance for lowmass particles. These issues are usually addressed by artificial stabilizers and careful aftersimulation tuning but this may cast doubt on the physical accuracy of computational results. We show that our spacetime finite element method for the timebased Dirac equation converges to analytic solutions without artificial stabilization or aftersimulation tuning even in the lowmass regime. This method may be an important tool for simulating partially understood particles such as neutrinos where lowmass performance is essential and aftersimulation tuning is inappropriate. | 2013-04-01T00:00:00Z | ['2013APS..APRJ15006V'] | null | New Computational method for solving the timebased Dirac Equation | 2,013 | 0 | 0 | ['PUB_HTML'] | 0 | null |
2021cosp...43E1625T | The gravitationalwave GW objects kilonova or the neutron star mergers NSMs are currently recognized as the rprocess nucleosynthesis sites under the neutron rich environment i.e. small electron fraction Y e and are expected to emit nuclear gammarays from unstable nuclei generated via the rprocess. Therefore the NSMs have a potential to emit MeV gammarays but the flux from NSM transients is expected to be very dim below the sensitivity of current gammaray missions Hotokezaka et al 2016. Instead of aiming to catch gammarays of transient events one of the more feasible ways is to survey gammarays from Galactic NSM remnants accumulated within a long decay time of nuclei for a few hundredtothousand years by deeper observations with longer exposures Wu et al 2019. In our study we first performed a numerical estimation of the gammaray flux from Galactic NSM Remnants using the nucleosynthesis calculations in the range of Y e of 0.1 0.45 by Freiburghauet et al 1999 and the distribution of Y e in NSMs by Wanajo 2014 adopting the nucleardecay database of JENDL DDF2015patch and the Doppler broadening effect by LiXin et al 2019. As a result we picked up several feasible nuclei for detection such as 227Th 223Ra 125Sb 137Ba 125Sb and so on from remnants younger than about 300 years and 243Am 126Sn 239Np 214Pb 214Bi and so on from older ones. We then performed a systematic survey of Galactic NSM Remnants with the INTEGRAL SPI in these lineenergy bands and no significant object was found along the galactic plane although several insignificant lineemitters may exist. Finally by combining the above theoretical and observational studies we extracted the upper limit on the event rate of NSMs at about 6000 Myr 1 par galaxy. Our gammaray studies must be very important as the independent diagnostics of the GW event rate. | 2021-01-01T00:00:00Z | ['2021cosp...43E1625T'] | null | Theoretical Estimations and Observational Systematic Survey of Rprocess Gammarays from Galactic Kilonova Remnants | 2,021 | 0 | 0.17 | null | 0 | null |
2017GReGr..49...91K | In this work we attempt to investigate the effect of minimal length on the thermodynamic properties of a polarized ideal gas. The modified electric field in three spatial dimensions based on the Kempf algebra is obtained. The modifications of the thermodynamic parameters of the polarized ideal gas such as the mean energy and entropy are found. Also we obtain the polarization and dielectric constant in the presence of a minimal length. By considering the values of experimental characteristics the upper bound on the deformation parameter is estimated. | 2017-07-01T00:00:00Z | ['2017GReGr..49...91K', '10.1007/s10714-017-2252-5'] | ['Generalized uncertainty principle', 'Minimal length', 'Thermodynamic properties', 'Polarized ideal gas', 'Polarization'] | Thermodynamic properties of the polarized ideal gas in the presence of a minimal length | 2,017 | 0 | 0.1 | ['PUB_HTML'] | 1 | null |
2015Ge&Ae..55.1076I | In our earlier works Ivanov and Miletsky 2012 2014 we demonstrated that 1 the evolution of average sunspot latitudes can be described by a universal latitude curve the shape of which does not depend on the cycle amplitude and 2 at the cycle decline phase these latitudes correlate well with the current level of solar activity. In this work we demonstrate that these features of the latitude evolution of the cycle as well as the empirical Waldmeier rule can be described by a simple model of a convective dynamo in a thin spherical layer with the addition of some nonlinearities. | 2015-12-01T00:00:00Z | ['2015Ge&Ae..55.1076I', '10.1134/S0016793215080113'] | ['Solar Activity', 'Solar Cycle', 'Secular Variation', 'Dynamo Model', 'Toroidal Field'] | Features of the spatial distribution of spots in the solar cycle and a model of dynamo in a thin layer | 2,015 | 0 | 0 | ['PUB_HTML'] | 0 | null |
2015AGUFMSH31A2392D | We present a composite analysis H and O of energetic ion spectra and kappa distribution fits using combined ion measurements from Charge Energy Mass Spectrometer CHEMS 3 to 236 keVe Low Energy Magnetospheric Measurements System LEMMS 0.024 lt E lt 18 MeV and the Ion Neutral Camera INCA 5.2 to gt220 keV for H. The modeled expressions of these energetic ion distributions are then used to obtain the four integral particle moments from zeroth to 3rd moment n In P IE i.e. Density Integral number intensity Pressure Integral energy intensity as well as the characteristic energy ECIEIn of these ions as a function of Local Time and LShell. We find that a protons dominate the energetic ion gt30 keV integral number and energy intensity at all radial distances Lgt5 Rs and local times while the H and O partial pressures and densities are comparable b the 12ltLlt20 Rs region corresponds to a local equatorial acceleration region where quasiadiabatic transport of H and nonadiabatic acceleration of O dominate the ion energetics compared to the contribution of charge exchange with the Saturnian neutral cloud c energetic ion bundles in the 12ltLlt17 Rs that possibly result from rotating energetic particle blobs shown in previous studies produce durable signatures enhancements in the H and O pressure density and temperature d energetic ions are depleted inside the orbit of Rhea 8 Rs i.e. the energetic ion lifetimes due to charge exchange decrease significantly with decreasing distance in the innermost parts of Saturns magnetosphere so that pressure and density drop to minimum inside 8 Rs. We then utilize a technique to retrieve the equatorial H and O pressure density and temperature in Saturns magnetosphere using a modified version of the Roelof and Skinner 2000 model in both local time and Lshell. Roelof E. C. and A. J. Skinner 2000 Space Sci. Rev. 91 437459. | 2015-12-01T00:00:00Z | ['2015AGUFMSH31A2392D'] | ['2756 Planetary magnetospheres', 'MAGNETOSPHERIC PHYSICS', '7827 Kinetic and MHD theory', 'SPACE PLASMA PHYSICS', '7845 Particle acceleration', 'SPACE PLASMA PHYSICS', '7851 Shock waves', 'SPACE PLASMA PHYSICS'] | Ion energetics at Saturns magnetosphere using CassiniMIMI measurements A simple model for the energetic ion integral moments | 2,015 | 0 | 0.12 | null | 0 | null |
2017LPI....48.1982M | LROLAMP observes scattered sunlight within the PSRs. We compare these observations with a model and other LRO datasets. | 2017-03-01T00:00:00Z | ['2017LPI....48.1982M'] | null | LROLAMP Observations of Illumination Conditions in the Lunar South Pole Permanently Shaded Regions | 2,017 | 0 | 0 | ['PUB_PDF'] | 0 | null |
2024STP....10a..54S | The paper presents the results of recording of acoustic waves caused by the Hunga Tonga volcano eruption in the South Pacific Ocean on January 15 2022 in Eastern Siberia at a distance of about 11230 km from the eruption. The received acoustic signal is interpreted as a set of atmospheric waves in a wide range of oscillations. The structure of the signal is similar to signals from the previously known powerful sources the thermonuclear explosion on Novaya Zemlya in 1961 and the explosion of the Tunguska meteorite in 1908. The acoustic signal was preceded by three trains of lowfrequency damped oscillations. We assume that these three trains of oscillations are associated with three important stages in the Hunga Tonga volcano eruption 1 destruction of Tonga island and formation of an underwater caldera 2 release of hot magma from the caldera to the ocean surface and release of a large volume of superheated steam into the atmosphere 3 formation of a layered structure from a mixture of superheated steam ash and tephra on the ocean surface and formation of an eruptive convective column. Successive phases of the eruption might have contributed to the excitation of acoustic vibrations in a wide range of periods including Lamb waves internal gravity waves IGW and infrasound. We compare the structure of the acoustic signal received in Siberia at a distance of more than 11000 km from the volcano and that of the acoustic signal recorded in Alaska at a distance of more than 9300 km. Using the solution of the linearized Korteweg de Vries equation we estimate the energy released during the volcanic eruption. | 2024-03-01T00:00:00Z | ['2024STP....10a..54S', '10.12737/stp-101202408'] | null | Registration of the atmospheric effect of the Hunga Tonga volcano eruption | 2,024 | 0 | 0.22 | ['PUB_HTML'] | 0 | null |
2017IJMPS..4560048T | We consider the analytical Bonnor solution for a relativistic neutron star and discuss about the limit in which this solution satisfies EinsteinMaxwell equations. We study the gravitational redshift for Bonnor solution without electric charge. We find that for stars with magnetic fields up to 1016G in the center the gravitational redshift for Bonnor metric differs from the Schwarzschild solution on a term that depends on magnetic dipole moment and the polar angle of the emission signal. | 2017-01-01T00:00:00Z | ['10.1142/S2010194517600485', '2017IJMPS..4560048T'] | ['Bonnor Solution', 'Gravitational Redshift', 'Neutron Star', '26.60.‑c'] | About Bonnor Solution and Gravitational Redshift | 2,017 | 0 | 0.18 | ['PUB_HTML', 'PUB_PDF'] | 0 | null |
2017IJMPS..4560047A | We study the equation of motion of neutral vector bosons bearing a magnetic moment MM. The effective rest mass of vector bosons is a decreasing function of the magnetic field intensity. Consequently a diffuse condensation of the bosons appears below a critical value of the field. For typical values of densities and magnetic fields the magnetization is positive and the neutral boson system can maintain a magnetic field selfconsistently. A discussion of the relevance in astrophysics is presented. | 2017-01-01T00:00:00Z | ['10.1142/S2010194517600473', '2017IJMPS..4560047A'] | ['Magnetic Field', 'Magnetized Boson Gas', 'Bose-Einstein Condensation', '98.35.Eg', '03.75Nt', '13.40Gp', '03.65Pm', 'Electric and magnetic fields'] | Condensation of Neutral Vector Bosons with Magnetic Moment | 2,017 | 0 | 0.14 | ['PUB_HTML', 'PUB_PDF'] | 4 | null |
2017IJMPD..2650156A | A study of the shadow cast by rotating black holes in different models of modified gravity is presented. It is shown that the size of the shadow cast depends on the modified gravity model used. The distortions of the shadow cast by modified gravity black holes are investigated and the effects are compared with the distortions cast by Kerr black hole. The shadow of a rotating black hole in modified gravity is found to be similar to the shadow cast by Kerr black hole but with different sizes and distortion effects. The naked singularity by rotating modified gravity black hole is discussed. Finally it is shown that some modified gravity models can present a considerable contribution to the size of black hole shadow. | 2017-01-01T00:00:00Z | ['2017IJMPD..2650156A', '10.1142/S0218271817501565'] | ['Modified gravity', 'rotating black hole', 'naked singularity', '04.50.Kd', '04.20.‑q', '04.25.Nx', 'Modified theories of gravity', 'Post-Newtonian approximation', 'perturbation theory', 'related approximations'] | Observing the shadow of modified gravity black hole | 2,017 | 0 | 0.14 | ['PUB_HTML', 'PUB_PDF'] | 3 | null |
2017Ge&Ae..57..512N | The purpose of this work is to draw the readers attention to the problem of possible differences in the generation of magnetic storms by different largescale solar wind types corotating interaction regions CIRs Sheaths and interplanetary coronal mass ejections ICMEs including magnetic clouds MCs and Ejecta. We recently showed that the description of relationships between interplanetary conditions and Dst and Dst indices with the modified formula by Burton et al. gives an 50 higher efficiency of storm generation by Sheath and CIR than that by ICME. Many function couplings FCs between different interplanetary parameters and the magnetosphere state have been suggested in the literature however they have not been analyzed for different solar wind types. In this work we study the generation efficiency of the main phase of a storm by different solar wind streams with the use of 12 FCs on the basis of OMNI data for 19762000. The results show that the Sheath has the highest efficiency for most FCs and MC is the least efficient and this result corresponds to our previous results. The reliability of the results and possible causes of differences for different FCs and solar wind types are to be studied further. | 2017-09-01T00:00:00Z | ['2017Ge&Ae..57..512N', '10.1134/S0016793217050152'] | null | Does magnetic storm generation depend on the solar wind type | 2,017 | 0 | 0.2 | ['PUB_HTML'] | 7 | null |
2017IJMPS..4560036D | Stars known as pulsars are generally modeled as magnetized spheres made of neutrons with high rotation frequency. It is known that such stars are spinning down and this braking is measured by a parameter n known as braking index. For the canonical model such parameter should have a single value for all pulsars n 3. However from observations it is known that n diverges from 3. In this work differently from the canonical model we have hypothesized the existence of a variation of the moment of inertia of the star through a timevarying radius. Using energy conservation we find the values for the variation of the radius of our pulsar sample. Our results indicate that it may be reasonable to consider that the radius of pulsars can be changing with time. | 2017-01-01T00:00:00Z | ['10.1142/S2010194517600369', '2017IJMPS..4560036D'] | ['Pulsars', 'Star Rotation', 'Magnetic Fields', '97.60.Jd', '97.60.Gb', '26.60', 'Neutron stars', 'Pulsars'] | A Model for the Braking Indices of Pulsars | 2,017 | 0 | 0.14 | ['PUB_HTML', 'PUB_PDF'] | 1 | null |
2017IJMPS..4560034G | In this work we have obtained the equation of state to the highly asymmetric dense stellar matter using the nonlinear Walecka model in the mean field approximation. We discussed the implication of changes in coupling constant of the delta baryonic resonance on the observable of the neutron star. A detailed analysis of the equation of state and of the baryonic effective mass in respect to changes in the delta coupling constants is carried out. We focus attention on a new aspect observed for pressure when varying the baryonic density of the medium a first order phase transition like a liquidgas phase transition was observed for an acceptable range of delta coupled constant values. We have explored the implication of this aspect for the neutron star structure and their maximum masses. | 2017-01-01T00:00:00Z | ['10.1142/S2010194517600345', '2017IJMPS..4560034G'] | ['Stars', 'Delta Resonances', 'Nonlinear Walecka Model', 'Equation of State', '21.65.Mn', '26.60.Kp', 'Equations of state of nuclear matter', 'Equations of state of neutron-star matter'] | Delta Resonance Coupling with Waleckas Mesons Implications to Stellar Matter EoS | 2,017 | 0 | 0.06 | ['PUB_HTML', 'PUB_PDF'] | 0 | null |
2017Ge&Ae..57..308C | The broadband electrostatic turbulence generally observed in the highlatitude ionosphere is a superposition of nonlocal waves of ionacoustic and ioncyclotron types. In the presence of a shear of ion parallel velocity ionacoustic modes can be induced by an instability emerging due to an inhomogeneous distribution of energy density. This paper is devoted to the studies of excitation of oblique ionacoustic wave in background configurations with inhomogeneous profiles of both electric field and ion parallel velocity. A numerical algorithm has been developed and instability was simulated at various parameters of background plasma. The general possibility of oblique ionacoustic wave generation by a gradient of ion parallel velocity is shown. In this case the wave spectrum is found to be broadband which agrees with satellite observations. | 2017-05-01T00:00:00Z | ['10.1134/S0016793217030045', '2017Ge&Ae..57..308C'] | null | Excitation of ionacoustic waves in the highlatitude ionosphere | 2,017 | 0 | 0.16 | ['PUB_HTML'] | 4 | null |
2017GeCoA.207...19S | Heterogeneous modally banded kyanitebearing and bimineralic eclogites from the lithospheric mantle collected at the Roberts Victor Diamond mine South Africa show a reaction texture in which kyanite is consumed. Geothermobarometric calculations using measured mineral compositions in PerpleX allowed the construction of a PT path showing a steep cool prograde metamorphic gradient of 2 Ckm to reach peak conditions of 5.8 GPa and 890 C for the kyanite eclogite. The kyaniteout reaction formed bimineralic eclogite and is probably an integral part of the mineralogical evolution of most archetypal bimineralic eclogites at Roberts Victor and potentially elsewhere. The kyaniteout reaction occured at close to peak pressure 5.3 GPa and was associated with a rise in temperature to 1380 C. Mass balance calculations show that upon breakdown the kyanite component is fully accommodated in garnet and omphacite via a reaction system with low water fugacity that required restricted fluid influx from metasomatic sources. The SUP18SUPO values of garnets are consistently higher than normal mantle values. Each sample has its characteristic trend of SUP18SUPO variance between garnets in the kyanitebearing sections and those in the bimineralic parts covering a range between 5.1 and 6.8. No systematic change in Oisotope signature exists across the sample population. Differences in garnet trace element signatures between differing lithologies in the eclogites are significant. Grossularrich garnets coexisting with kyanite have strong positive Euanomalies and low GdYb ratios while more pyroperich garnets in the bimineralic sections have lost their positive Euanomaly have higher GdYb ratios and generally higher heavy rare earth element contents. Garnets in the original kyanitebearing portions thus reflect the provenance of the rocks as metamorphosed gabbrostroctolites. The kyaniteout reaction was most likely triggered by a heating event in the subcratonic lithosphere. As kyanite contains around 100 ppm of HSUB2SUBO it is suggested that the kyaniteout reaction once initiated by heating and restricted metasomatic influx was promoted by the release of water contained in the kyanite. The steep highP lowT prograde PT path defining rapid compression at low heating rates is atypical for subduction transport of eclogites into the lithospheric mantle. Such a trajectory is best explained in a model where strong lateral compression forces eclogites downward to higher pressures supporting models of cratonic lithosphere formation by lateral collision and compression. | 2017-06-01T00:00:00Z | ['10.1016/j.gca.2017.03.017', '2017GeCoA.207...19S'] | ['Kaapvaal craton', 'Cratonic lithosphere', 'Perple_X', 'Kyanite', 'Oxygen isotopes', 'Eclogite'] | Fluidinduced transition from banded kyanite to bimineralic eclogite and implications for the evolution of cratons | 2,017 | 0 | 0.21 | ['PUB_HTML'] | 10 | null |
2017Ge&Ae..57.1009C | For electron acceleration during solar flares it is very important to determine the pitchangle and energy dependences of the electron distribution function. At present this cannot be done directly from observations. Therefore it is necessary to perform a numerical simulation of the propagation of accelerated electrons in the magnetic field of the flare loop loops and calculate the Xray and radio emissions. For the solar flare of November 10 2002 we have obtained qualitative and quantitative agreements of modeled Xray and radio maps with the RHESSI satellite and Nobeyama Radioheliograph data. We have determined the flare model parameters that agree with observations. The pitchangle anisotropy of electrons determined by highly directional functions of the S cosSUP8SUP type the energy spectrum consist of two electron populations the lowenergy part of the spectrum up to an energy of break of 350 keV is characterized by a power law with the exponent SUB1SUB 2.72.9 and the energy spectrum is more rigid above 420 keV SUB2SUB 22.3. | 2017-12-01T00:00:00Z | ['2017Ge&Ae..57.1009C', '10.1134/S0016793217080060'] | null | Modeling of Physical Processes by Analysis of Hard XRay and Microwave Radiations in the Solar Flare of November 10 2002 | 2,017 | 0 | 0.19 | ['PUB_HTML'] | 4 | null |
2024STP....10a..19K | We present the results of Auroral Kilometric Radiation AKR measurements near the plasmapause on the ERG Arase satellite. The apogee of the satellites orbit is located near the ecliptic plane at latitudes 30. According to the generally accepted point of view AKR observation is impossible in this region since it is shielded by the plasmasphere. Simultaneous measurements of AKR and local plasma density made it possible to determine that AKR in nearequatorial regions occur in plasma channels density inhomogeneities elongated along magnetic field lines. AKR from sources located in the auroral magnetosphere is transferred by these channels to the equatorial region. This work analyzes the conditions for the capture and propagation of AKR in low plasma density channels. In the geometrical optics approximation we have simulated the conditions for the radiation capture and propagation. The calculation results show that the proposed scheme for AKR capture into plasma channels can explain the measurement results the radiation transfer from the auroral region to the nearequatorial region. | 2024-03-01T00:00:00Z | ['2024STP....10a..19K', '10.12737/stp-101202403'] | null | Transfer of auroral kilometric radiation through lowdensity channels at the boundary of plasmasphere | 2,024 | 0 | 0.3 | ['PUB_HTML'] | 0 | null |
2017LPI....48.2378B | We present an update on ExoMars2020 landing site selection and characterisation. | 2017-03-01T00:00:00Z | ['2017LPI....48.2378B'] | null | Selection and Characterisation of the ExoMars 2020 Rover Landing Sites | 2,017 | 0 | 0.16 | ['PUB_PDF'] | 4 | null |
2017LPI....48.1310J | ChemCam spectra of recent drill fines consistent with hematite but also suggest variable ferric phases oxidation crystallinity grain size andor mixing. | 2017-03-01T00:00:00Z | ['2017LPI....48.1310J'] | null | ChemCam Passive Reflectance Spectroscopy of Recent Murray Formation Drill Tailings Oudam Marimba Quela Sebina | 2,017 | 0 | 0.1 | ['PUB_PDF'] | 0 | null |
2017LPI....48.1504M | Petrogenesis of gabbroic shergottite NWA 6963 interpreted from pyroxene zoning profiles. | 2017-03-01T00:00:00Z | ['2017LPI....48.1504M'] | null | Crystallization History of Gabbroic Shergottite NWA 6963 as Revealed by Pyroxene Zoning | 2,017 | 0 | 0.06 | ['PUB_PDF'] | 0 | null |
2017LPI....48.1987B | Apollo 16 and 17 landing sites are investigated with Kaguya data to define units of crater counting. Results are used to reevaluate crater statistics. | 2017-03-01T00:00:00Z | ['2017LPI....48.1987B'] | null | Apollo Landing Sites 16 and 17 Spectral Mapping and Crater Statistics Reevaluated | 2,017 | 0 | 0 | ['PUB_PDF'] | 0 | null |
2017LPI....48.1122L | Multiple sampling geometries and a diverse set of rock types are used to quantify variability in LIBS spectra due to changes in ablation and collection angle. | 2017-03-01T00:00:00Z | ['2017LPI....48.1122L'] | null | LaserInduced Breakdown Spectroscopy of Rock Powders Performed at Variable Angles of Ablation and Collection | 2,017 | 0 | 0.06 | ['PUB_PDF'] | 0 | null |
2017LPI....48.1411K | Based on the CTXscale mapping and dating we summarize how the floor of the Harmakhis Vallis channel has been modified after its formation. | 2017-03-01T00:00:00Z | ['2017LPI....48.1411K'] | null | Modification History of the Harmakhis Vallis Outflow Channel Mars | 2,017 | 0 | 0 | ['PUB_PDF'] | 0 | null |
2017LPI....48.2081P | Deciphering why water contents in nominally anhydrous minerals of martian meteorites are low compared to terrestrial equivalents. | 2017-03-01T00:00:00Z | ['2017LPI....48.2081P'] | null | Hydrogen in Martian Meteorites | 2,017 | 0 | 0 | ['PUB_PDF'] | 0 | null |
2017LPI....48.2382H | Undergraduates can learn about planetary science while making maps to answer scientific questions. Xanthe Terra on Mars is a good place to start. | 2017-03-01T00:00:00Z | ['2017LPI....48.2382H'] | null | Satellite Data Fusion to Better Understand Martian Structure and Volcanics | 2,017 | 0 | 0 | ['PUB_PDF'] | 0 | null |
2015LPICo1861.1079W | A recently developed software tool allows for the prediction of the impact crater record based on a given history of erosion and deposition. A first application to pedestal craters in the Medusae Fossae formation on Mars yields promising results. | 2015-09-01T00:00:00Z | ['2015LPICo1861.1079W'] | null | The Potential of Crater Size Frequency Distributions for Deriving Erosion Histories A Case Study on Mars | 2,015 | 0 | 0 | ['PUB_PDF'] | 0 | null |
2017LPI....48.2183S | The next generation of CRISM mapping observation mosaic data products will incorporate noise remediation and radiometric reconciliation. | 2017-03-01T00:00:00Z | ['2017LPI....48.2183S'] | null | Next Generation CRISM Multispectral Map of Mars Noise Reduction and Radiometric Reconciliation | 2,017 | 0 | 0.1 | ['PUB_PDF'] | 0 | null |
2017LPI....48.1311X | We report the new ages 320340Ma of the basement granites of the Chicxulub Crater in the Yucatan block and discuss its tectonic implications. | 2017-03-01T00:00:00Z | ['2017LPI....48.1311X'] | null | Ages and Geochemistry of the Basement Granites of the Chicxulub Impact Crater Implications for Peak Ring Formation | 2,017 | 0 | 0.19 | ['PUB_PDF'] | 0 | null |
2017LPI....48.1788K | We investigated mineral compositions of lunar mare basalts erupted at the late stage of volcanic activity. | 2017-03-01T00:00:00Z | ['2017LPI....48.1788K'] | null | Compositional Analysis of Young Mare Basalts in the Procellarum KREEP Terrane Using Kaguya Data | 2,017 | 0 | 0.06 | ['PUB_PDF'] | 0 | null |
2017LPI....48.1886B | HfW systematics define a CR chondrule formation age of 3.7 Ma after CAIs. CR metal and silicate have complementary nucleosynthetic W and Mo isotope anomalies. | 2017-03-01T00:00:00Z | ['2017LPI....48.1886B'] | null | HafniumTungsten Chronology of CR Chondrites | 2,017 | 0 | 0.06 | ['PUB_PDF'] | 1 | null |
2017LPI....48.1312L | Many basin rings are composed of or contain troctolitic anorthosite or anorthositic troctolite such rocks also feature widespread exposure on the farside. | 2017-03-01T00:00:00Z | ['2017LPI....48.1312L'] | null | Global and Local Distribution of Troctolitic Rocks Using Kaguya Multiband Imager Data and Radiative Transfer Mineral Mapping | 2,017 | 0 | 0.12 | ['PUB_PDF'] | 0 | null |
2017LPI....48.2181M | Thermal models of CM parent bodies provide an explanation for the early formation ages of CM carbonates. | 2017-03-01T00:00:00Z | ['2017LPI....48.2181M'] | null | CM Carbonates Should Be Old Insights from Parent Body Thermal Modeling | 2,017 | 0 | 0.12 | ['PUB_PDF'] | 0 | null |
2017LPI....48.1599K | Solid ejecta experience gas drag heat exchange and radiative interaction with a disturbed atmosphere and a cloud of target and impactor vapors. | 2017-03-01T00:00:00Z | ['2017LPI....48.1599K'] | null | Thermal Evolution of Impact Ejecta in Fireball | 2,017 | 0 | 0.06 | ['PUB_PDF'] | 0 | null |
2017LPI....48.1219B | The origin of CaPlagioclase clasts in polymict ureilites are similar to plagioclase in NWA 7325 may represent pieces of a previously unrecognized parent body | 2017-03-01T00:00:00Z | ['2017LPI....48.1219B'] | null | Calcic PlagioclaseRich Clasts Resembling the NWA 7325 Ungrouped Achondrite in Polymict Ureilites | 2,017 | 0 | 0 | ['PUB_PDF'] | 0 | null |
2017LPI....48.2282Y | The goal of this work is to determine the spectroscopic detection limits of additional evaporite minerals in halitesilicate mixtures. | 2017-03-01T00:00:00Z | ['2017LPI....48.2282Y'] | null | Spectroscopic Detection Limits of Minor Phases in ChlorideBearing Mineral Mixtures | 2,017 | 0 | 0 | ['PUB_PDF'] | 0 | null |
2017LPI....48.1698C | We compare the reflectance and submicroscopic iron produced for minerals weathered by laser irradiation at room temperature and temperatures comparable to PSRs. | 2017-03-01T00:00:00Z | ['2017LPI....48.1698C'] | null | The Effect of Temperature on the Reflectance Spectra of Pyroxene and a Highlands Analog Weathered by Laser Irradiation | 2,017 | 0 | 0.17 | ['PUB_PDF'] | 2 | null |
2017LPI....48.1409D | We report about Luna 20 rocks containing Pbearing olivine and suggest a possible presence of P3 in its structure. | 2017-03-01T00:00:00Z | ['2017LPI....48.1409D'] | null | PBearing Olivines in Rocks from the Luna 20 Site | 2,017 | 0 | 0 | ['PUB_PDF'] | 0 | null |
2017LPI....48.1217N | We have restored large parts of the data from the Apollo 15 heat flow experiment for the period of 1975 through 1977 that were not previously archived. | 2017-03-01T00:00:00Z | ['2017LPI....48.1217N'] | null | Restoration of the Apollo 15 Heat Flow Experiment Data from 1975 to 1977 | 2,017 | 0 | 0 | ['PUB_PDF'] | 0 | null |
2017LPI....48.1120T | We have detected and studied a depression of the 787 nm ammonia absorption band in the Northern hemisphere at low latitudes on Jupiter. | 2017-03-01T00:00:00Z | ['2017LPI....48.1120T'] | null | Jupiter LowLatitude Depression of the Ammonia Absorption in Northern Hemisphere | 2,017 | 0 | 0.12 | ['PUB_PDF'] | 0 | null |
2017LPI....48.1696G | We present a deep generative model for predicting and interpreting data from laserinduced breakdown spectroscopy. | 2017-03-01T00:00:00Z | ['2017LPI....48.1696G'] | null | Deep Learning Models for Spectroscopic Data SemiSupervised Generative Models Applied to LaserInduced Breakdown Spectroscopic Data | 2,017 | 0 | 0.06 | ['PUB_PDF'] | 0 | null |
2017LPI....48.2179T | A summary and some highlights based on the creation and analysis of simulated ExoMars TGOCaSSIS image cubes used to assess colour and spatial capabilities. | 2017-03-01T00:00:00Z | ['2017LPI....48.2179T'] | null | Colour and Stereo Surface Imaging System on the ExoMars Trace Gas Orbiter An Assessment of Colour and Spatial Capabilities Through Image Simulations | 2,017 | 0 | 0.06 | ['PUB_PDF'] | 0 | null |
2017LPI....48.2483V | We present the petrography and chemistry of lunar meteorite NWA 10656 which is an olivine gabbro distinct from the other members of the NWA 773 clan. | 2017-03-01T00:00:00Z | ['2017LPI....48.2483V'] | null | Petrography and Chemistry of Lunar Diabasic Meteorite Northwest Africa NWA 10656 | 2,017 | 0 | 0 | ['PUB_PDF'] | 0 | null |
2016cosp...41E1827S | Perturbing forces on spacecraft are a challenge for the establishment and maintenance of satellite formations. For large satellites the use of thrusters is a practical means of countering perturbing forces. However longterm thrusting is not currently feasible for miniaturised satellites due to volume and mass constraints. Astrodynamics effects in particular passive aerodynamic lift and drag forces are possible means for miniaturised satellites to maintain a formation in Low Earth Orbit LEO. Currently lift and drag for rendezvous have been considered in the presence of simplified orbital models namely two body motion with the J2 effect. Given the small magnitude of lift and drag in LEO it is unclear as to the control effectiveness of these aerodynamic forces under all orbital perturbations including solar radiation pressure third body gravitation and the nonspherical gravity. The work presented here will explore the extent to which aerodynamic lift and drag can be utilised for formation establishment and maintenance under changing operating conditions including altitude orbital inclination space weather sensor errors and allencompassing orbital perturbations. This work applies an inhouse developed orbital propagation code to simulate the motion of formation flying spacecraft under differing conditions. The results will help miniaturised satellite formation flight planners better plan and operate future formation missions and will also feed into improved understanding of the 6DOF motion of nearEarth orbit objects including that of uncontrolled objects such as space debris. | 2016-07-01T00:00:00Z | ['2016cosp...41E1827S'] | null | The impact of lift and drag on 6DOF motion of LEO objects formation control and debris behaviour | 2,016 | 0 | 0.22 | null | 0 | null |
2017GCN.21736....1L | MASTER OT J033744.97723159.0 lipunov Gorbovskoy Kornilov et al. GCN LVC GCN 21719 21780 is cheked recently by MASTERIAC Tenerife Spain. Our photometrical results are Date Time JD Filter Mag A Magcor 20170827 224616 2457993.4487963 B 18.12 1.41 16.71 20170827 225010 2457993.4515046 V 16.81 1.07 15.74 20170827 225010 2457993.4515046 R 16.04 0.80 15.24 20170827 224616 2457993.4487963 I 15.94 0.51 15.43 for EBV 0.3436 and Av 3.1 EBV 1.065 Uncorrected magnitude B 18.1226 V 16.8078 R 16.0422 I 15.9435 EBV 0.3436 httpirsa.ipac.caltech.eduapplicationsDUST Av 3.1 EBV gt Av 1.06516 httpwww.astro.ncu.edu.twwchenCoursesISM11.Extinction.pdf page 17 gt httpwww.astro.ncu.edu.twwchenCoursesISM11.Extinction.pdf page 22 So MASTER OT J033744.97723159.0 is reddening cf Im et al LVC GCN 21723. The spectroscopic observations are requared. This message can be citted. | 2017-08-01T00:00:00Z | ['2017GCN.21736....1L'] | null | LIGOVirgo G299232PGWB170825.55 MASTER OT J033744.97723159.0 inside 25m isophota of the NGC1343 galaxy is reddening | 2,017 | 0 | 0 | ['PUB_HTML'] | 0 | null |
2017GCN.21740....1L | Following Lynch et al. LVC GCN 21670 we observed a third epoch of NGC 4993 with the Australia Telescope Compact Array at 8.5 and 10.5 GHz. Observations started at 20170827 232624.9 UT and ended at 20170828 90000 UT with approximately 2.3 hours of onsource time. We fit and subtracted a pointsource at the optical position of NGC 4993 130947.71 232301.79 Skrutskie et al. 2003 2MASS Extended Source Catalog. From this we set a 3sigma upper limit of 54 uJy and 39 uJy on radio emission from SSS17a at 8.5 and 10.5 GHz respectively. Subsequent epochs are planned. Thank you to CSIRO staff for supporting these observations. | 2017-08-01T00:00:00Z | ['2017GCN.21740....1L'] | null | LIGOVirgo G298048 Further ATCA followup of SSS17a in NGC 4993 | 2,017 | 0 | 0.06 | ['PUB_HTML'] | 0 | null |
2024E&PSL.63718726W | Waveform modeling constrains earthquake source parameters in Mentawai Sumatra. Two trenchparallel earthquake belts located at great earthquakes rupture areas. Downdip belt indicates bending of the megathrust. Updip belt marks the frictional boundary of seismogenic zones. Lateral variations in updip belt indicate diverse seismogenic widths and coupling. | 2024-07-01T00:00:00Z | ['10.1016/j.epsl.2024.118726', '2024E&PSL.63718726W'] | ['Slab geometry', 'Earthquake source parameters', 'Ramp structures', 'Coupling', 'Sumatra'] | Plate interface geometry complexity and persistent heterogenous coupling revealed by a highresolution earthquake focal mechanism catalog in Mentawai Sumatra | 2,024 | 0 | 0.22 | ['PUB_HTML'] | 0 | null |
2016SPIE10012E..0DR | The design of astronomical instrument is growing in dimension and complexity following ELT class telescopes. The availability of new structural material like composite ones is asking for more robust and reliable designing numerical tools. This paper wants to show a new optomechanical optimization approach developed starting from a previously developed integrated design framework. The Idea is to reduce number of iteration in a multi variable structural optimization taking advantage of the embedded sensitivity routines that are available both in FEA software and in raytracing ones. This approach provide reduced iteration number mainly in case of high number of structural variable parameters. | 2016-07-01T00:00:00Z | ['10.1117/12.2203355', '2016SPIE10012E..0DR'] | null | Integrated optomechanical structural optimization through coupling of sensitivity matrixes | 2,016 | 0 | 0 | ['PUB_HTML'] | 0 | null |
2016SPIE10000E..1UK | Aerospace Research Department of the Institute of Applied Physical Problems at Belarusian State University has developed a prototype of the optical payload intended for a space experiment on the ISS board. The prototype includes four optical modules for the night glows observation in particular spatialbrightness and spectral characteristics in the altitude range of 80320 km. Objects of the interest are emitting top layers of the atmosphere including exited OH radicals atomic and molecular oxygen and sodium layers. The goal of the space experiment is a research of night glows over different regions of the Earth and a connection with natural disasters like earthquakes cyclones etc. Two optical modules for spatial distribution of atomic oxygen layers along the altitude consist of input lenses spectral interferential filters and line CCD detectors. The optical module for registration of exited OH radical emissions is formed from CCD array spectrometer. The payload includes also a panchromatic 400900 nm high sensitive imaging camera for observing of the glows general picture. The optical modules of the prototype have been tested and general optical characteristics were determined in laboratory conditions. A solution of an astigmatism reducing of a concave diffraction grating and a method of the second diffraction order correction were applied and improved spectrometers optical characteristics. Laboratory equipment and software were developed to imitate a dynamic scene of the night glows in laboratory conditions including an imitation of linear spectra and the spatial distribution of emissions. | 2016-10-01T00:00:00Z | ['2016SPIE10000E..1UK', '10.1117/12.2241791'] | null | The multisensor payload Structura for the observation of atmospheric night glows from the ISS board | 2,016 | 0 | 0.1 | ['PUB_HTML'] | 0 | null |
2024ESS.....562411K | A primary motivation behind measuring the composition of exoplanetary atmospheres is to understand planet formation and evolution. However confidently determining a single planets formation and evolution history from its atmospheric composition is prevented by the uncertainties and degeneracies inherent to protoplanetary disc composition and planetary evolution. To bypass these uncertainties and learn how a planets formation and evolution influence its current day atmospheric composition we are undertaking a survey with JWST that is comparing a sample of planets that we know underwent very different evolutionary histories due to their different orbital alignments. Specifically we are comparing the composition of three hot Jupiters whose orbits are aligned with their host stars spin axes with three hot Jupiters that are misaligned. It is believed that aligned hot Jupiters are the outcome of disc migration while misaligned ones arise from higheccentricity migration. This dichotomy in their formation and migration pathways leads to differences in the material they accrete during their evolution which in turn should lead to measurable differences in their atmospheric carbon to oxygen ratio. By comparing the relative composition of an aligned and misaligned hot Jupiter sample we will test if atmospheric composition depends on planet migration and thus if atmospheric composition can be used to make inferences about formation. I will give an overview of our medium category program GO 3838 and present new theoretical predictions from our stateoftheart disc chemistry models. | 2024-04-01T00:00:00Z | ['2024ESS.....562411K'] | null | Does atmospheric composition actually trace formation Observing aligned vs misaligned hot Jupiters as a testbed | 2,024 | 0 | 0.3 | ['PUB_HTML'] | 0 | null |
2024ESS.....562407L | XUVdriven photoevaporation is a leading hypothesis on the astrophysical processes that sculpt the observed distribution of shortperiod planetary radii. In recent years direct evidence of atmospheric escape has been detected via intransit transmission of the metastable He triplet near 10830 . Dozens of planets have been probed with this tracer mostly as singleepoch snapshots. Since the stellar XUV that underlies planetary massloss is timevariable it is necessary to understand the outflows responses to changes in the incident flux. Here we report results from an ongoing longitudinal study to characterize the timevariability of WASP69bs atmospheric outflow. We obtained contemporaneous metastable He data from PalomarWIRC along with Xray and midUV data from the Swift Observatory. Together these data lead to a comprehensive characterization of WASP69bs hydrodynamical state in the epoch of observation. By comparison to archival metastable He data and archival highenergy data from XMMNewton we assess the time variability of WASP69bs massloss rate on timescales commensurate with typical stellar activity cycles. | 2024-04-01T00:00:00Z | ['2024ESS.....562407L'] | null | Searching for Atmospheric Outflow Variability in WASP69b | 2,024 | 0 | 0.31 | ['PUB_HTML'] | 0 | null |
2024E&PSL.63718722M | During sealevel rise an alluvialdeltaic system has a critical spatial dimension. The overexpanded system is subjected to nondeltaic transgression with shrinkage. Shrinkage can be normalized by autostratigraphic length and time scales. During shrinkage the alluvial channels change their intrinsic behavior. The shrinkage concept can account for some alluvial features on Earth and Mars. | 2024-07-01T00:00:00Z | ['2024E&PSL.63718722M', '10.1016/j.epsl.2024.118722'] | ['Alluvial', 'Autostratigraphy', 'Channel stability', 'Morphodynamic equilibrium', 'Non-deltaic transgression', 'Relative sea level rise'] | Autogenic shrinkage and channel destabilization of an overexpanded downstream alluvial system under steady rise of relative sea level An experimental study | 2,024 | 0 | 0.12 | ['PUB_HTML'] | 0 | null |
2024E&SS...1103538K | Microphysical observations of precipitating particles are critical data sources for numerical weather prediction models and remote sensing retrieval algorithms. However obtaining coherent data sets of particle microphysics is challenging as they are often unindexed distributed across disparate institutions and have not undergone a uniform quality control process. This work introduces a unified comprehensive Northern Hemisphere particle microphysical data set from the National Aeronautics and Space Administration precipitation imaging package PIP accessible in a standardized data format and stored in a centralized public repository. Data is collected from 10 measurement sites spanning 34 latitude 37N71N over 10 years 20142023 which comprise a set of 1070000 precipitating minutes. The provided data set includes measurements of a suite of microphysical attributes for both rain and snow including distributions of particle size vertical velocity and effective density along with higherorder products including an approximation of volumeweighted equivalent particle densities liquid equivalent snowfall and rainfall rate estimates. The data underwent a rigorous standardization and quality assurance process to filter out erroneous observations to produce a selfdescribing scalable and achievable data set. Case study analyses demonstrate the capabilities of the data set in identifying physical processes like precipitation phasechanges at high temporal resolution. Bulk precipitation characteristics from a multisite intercomparison also highlight distinct microphysical properties unique to each location. This curated PIP data set is a robust database of highquality particle microphysical observations for constraining future precipitation retrieval algorithms and offers new insights toward better understanding regional and seasonal differences in bulk precipitation characteristics. | 2024-05-01T00:00:00Z | ['10.1029/2024EA003538', '2024E&SS...1103538K'] | ['precipitation', 'microphysics', 'disdrometer', 'particle size distribution', 'data set', 'precipitation imaging package'] | A Comprehensive Northern Hemisphere Particle Microphysics Data Set From the Precipitation Imaging Package | 2,024 | 0 | 0.17 | ['PUB_HTML'] | 0 | null |
2023yCat..36740025H | As part of this paper the table variSUBspuriousSUBs is published in the Gaia DR3 archive for all 11754237 sources with published photometric time series i.e. sources in gaiasource with hasSUBepochSUBphotometrytrue. Of these 10509536 sources are variables Eyer et al. 2022 arXiv2206.06416 and 1257319 are part of the Gaia Andromeda Photometric Survey GAPS Evans et al. 2022 arXiv2206.05591 which one can identify in gaiasource by their photSUBvariableSUBflagVARIABLE and inSUBandromedaSUBsurveytrue flags respectively. Note that 12618 sources overlap between the two. P 1 data file. | 2023-03-01T00:00:00Z | ['2023yCat..36740025H'] | ['Gaia'] | VizieR Online Data Catalog Gaia DR3. spurious signals Holl 2023 | 2,023 | 0 | 0.28 | null | 0 | null |
2016SPIE.9906E..5PS | The 25 European antennas of ALMA were delivered by ESO to the ALMA project in Chile between April 2011 and September 2013. Their combined time of operation is already significant and allows us to draw conclusions regarding their ability to fulfil the original specification in terms of both scientific performance and operational availability. In this paper we will summarize the experience gained during the past five years of operation. We will characterize the performance of the antennas in routine operation and compare with the data obtained during acceptance testing. We will also describe the few technical issues experienced while operating at 5000m and the way in which these were treated during these first years of operation. We will evaluate the effective reliability obtained in service based on field data and draw some conclusions as to the way in which reliability and maintainability aspects were covered during the process which led to the final design of the antenna. We will discuss the smart use of software to handle redundancy in a flexible way and to exclude failed components without affecting overall antenna operability. The use of lowlevel diagnostics enabled by remote access allows us to shorten the troubleshooting cycle and to optimise physical interventions on the antennas. Finally the paper will cover Antenna maintenance manuals edited using an industrial interactive standard. It will be explained why this advanced and innovative concept has not achieved the success that was expected and why the traditional form is preferred at the ALMA Observatory. | 2016-07-01T00:00:00Z | ['2016SPIE.9906E..5PS', '10.1117/12.2232622'] | null | Experience with the operation of the European ALMA antennas | 2,016 | 0 | 0.06 | ['PUB_HTML'] | 0 | null |
2024E&PSL.64318921H | Key processes of the 2006 Pingtung cascading hazards are better constrained. Intraplate earthquakes near coastlines may pose underrated submarine geohazard. Tsunami phenomena associated with complex sources challenge current warning system. | 2024-10-01T00:00:00Z | ['10.1016/j.epsl.2024.118921', '2024E&PSL.64318921H'] | ['Tsunami', 'Earthquake source characteristic', 'Hydrodynamic', 'Cascading marine geohazards'] | Source characteristics of the 2006 Pingtung earthquake doublet off southern Taiwan and the possible contribution of submarine landslides to the Tsunami | 2,024 | 0 | 0.06 | ['PUB_HTML'] | 1 | null |
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