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2020ApJ...896..118C

Plasmaspheric hiss is known to be a major contributor to the dynamic losses of Earths radiation belt electrons. While previous computation attempts of hissdriven electron losses are limited to the cold plasma approximation in this study we find that hot plasma effects will modify the hiss dispersion relation and result in changes in the electron bounceaveraged electron pitch angle diffusion coefficients. Cold plasma approximation tends to overestimate the diffusion coefficients of 100 keV electrons by orders of magnitude while the scattering efficiency of higher energy electrons is not greatly affected. As the Lshell decreases or the parameter alpha rmOmega e2omega mathrmpe2 decreases where rmOmega e is the electron gyrofrequency and omega mathrmpe is the plasma frequency the decrease of diffusion coefficients of low energy electrons caused by hot plasma effects become more pronounced. It is also shown that both the increase of hot electron abundance and temperature anisotropy can weaken the scattering efficiency of 100 keV electrons at almost all pitch angles while the diffusion coefficients of higher energy electrons decrease at large pitch angles. Our study confirms the importance of including hot plasma effects in evaluations of hissdriven scattering loss of radiation belt electrons.

2020-06-01T00:00:00Z

['Van Allen radiation belts', 'Planetary magnetospheres', 'Space plasmas', '1758', '997', '1544']

Hot Plasma Effects on the Pitchangle Scattering Rates of Radiation Belt Electrons Due to Plasmaspheric Hiss

https://ui.adsabs.harvard.edu/link_gateway/2020ApJ...896..118C/EPRINT_PDF

['1758', '997', '1544']

['Van Allen radiation belts', 'Planetary magnetospheres', 'Space plasmas']

['Van Allen radiation belts', 'Planetary magnetospheres', 'Space plasmas']

2020ApJ...888...69B

An analytic model of the timedependent electric and magnetic fields of an astrophysical jet is presented. These fields satisfy the timedependent Faradays law and describe a jet with increasing length. The electric field contains both electrostatic and inductive parts. The electrostatic part corresponds to the rate of injection of toroidal magnetic flux while the sum of the electrostatic and inductive parts results in the electric field parallel to the magnetic field being zero everywhere. The pinch force associated with the electric current provides a peaked pressure on the jet axis and a pressure minimum at the radius where the poloidal magnetic field reverses direction.

2020-01-01T00:00:00Z

['Accretion', 'jets', 'magnetohydrodynamics', 'stellar jets', 'stellar accretion disks', 'young stellar objects', 'Collimation', '14', '870', '1964', '1607', '1579', '1834', '268']

Analytic Model for the Timedependent Electromagnetic Field of an Astrophysical Jet

https://ui.adsabs.harvard.edu/link_gateway/2020ApJ...888...69B/EPRINT_PDF

['14', '870', '1964', '1607', '1579', '1834', '268']

['Accretion', 'Jets', 'Magnetohydrodynamics', 'Stellar jets', 'Stellar accretion disks', 'Young stellar objects', 'Collimation']

['Accretion', 'Jets', 'Magnetohydrodynamics', 'Stellar jets', 'Stellar accretion disks', 'Young stellar objects', 'Collimation']

2022pds..data...54M

Mesick PDART 2019 Mars Odyssey Improved DND Products

2022-01-01T00:00:00Z

['2001', '2019', 'PDS', 'PDS4', 'derived', 'dnd', 'grs', 'improved', 'mars', 'mesick', 'n', 'odyssey', 'pdart', 'product', 'science']

Mesick PDART 2019 Mars Odyssey Improved DND Products Bundle

https://ui.adsabs.harvard.edu/link_gateway/2022pds..data...54M/EPRINT_PDF

['2001', '2019']

['Solar dynamo', 'Reverberation mapping']

['Solar dynamo', 'Reverberation mapping']

2022RNAAS...6..224M

The analysis of high resolution spectra of the HgMn star HD 35548A recorded by the SWP camera on board the International Ultraviolet Explorer reveals no variations of the farultraviolet flux of this star over about 21 hr in 1981. The resonance lines of Ga II and Ga III characteristic of classical HgMn stars are salient features in the mean SWP spectrum of HD 35548A. The TESS lightcurve of the system HD 35548A and HD 35548B has an asymetric structure with a steep descent to the minimum and a slower rise to next maximum. The period measured between two successive maxima is close to 6.07 0.09 days which could be the orbital and rotational period due to synchronization with the companion of HD 35548A.

2022-10-01T00:00:00Z

['Chemically peculiar stars', 'Mercury-manganese stars', '226', '1025']

The Behavior of HgMn Stars in the Far UVPaper 17 HD 35548A

https://ui.adsabs.harvard.edu/link_gateway/2022RNAAS...6..224M/EPRINT_PDF

['226', '1025']

['Chemically peculiar stars', 'Mercury-manganese stars']

['Chemically peculiar stars', 'Mercury-manganese stars']

2020ApJ...900...49P

We derive an equation of state EOS for magnetized chargeneutral nuclear matter relevant for a neutron star NS. The calculations are performed within an effective chiral model based on the generalization of the model with nonlinear selfinteractions of the mesons along with the crosscoupling term. This model is extended by introducing the contributions of a strong magnetic field on the charged particles. The contributions arising from the effects of the magnetic field on the Dirac sea of charged baryons are also included. The resulting EOS for the magnetized dense matter is used to investigate the NS properties like its mass radius and tidal deformability. The magnitude of the magnetic field at the core of the NS considered here is in the range of 10SUP15SUP10SUP18SUP G for which the relative deformation from spherical symmetry turns out to be less than 1 giving a post facto justification for the spherically symmetric treatment of the NS structure. The dimensionless tidal deformability SUB1.4SUB is 526 for an NS with mass 1.4 MSUBSUB which is consistent with the recent observation of GW 170817. The maximum mass of the NS in the presence of a strong magnetic field is consistent with the observational constraints on the mass of the pulsar PSR J03480432 and its radius at a mass of 1.4 MSUBSUB is also in agreement with the empirical bounds.

2020-09-01T00:00:00Z

['Neutron stars', '1108']

An Equation of State for Magnetized Neutron Star Matter and Tidal Deformation in Neutron Star Mergers

https://ui.adsabs.harvard.edu/link_gateway/2020ApJ...900...49P/EPRINT_PDF

['1108']

['Neutron stars']

['Neutron stars']

2024RNAAS...8..241S

Both Christian Huygens and William Derham expressed ideas that are prescient to the concept of a circumstellar habitable zone liquid water is a precondition for life there is a region within the solar system within which liquid surface water can exist upon planets the stars are suns around which planetary systems should be common these extrasolar planetary systems may include habitable worlds. Although neither author explicitly developed the phraseology of an exoplanetary habitable zone based upon liquid water such a concept would follow from their writings.

2024-09-01T00:00:00Z

['Habitable zone', 'Exoplanets', '696', '498']

Christian Huygens and William Derham and 18th Century Precursors to the Habitable Zone

https://ui.adsabs.harvard.edu/link_gateway/2024RNAAS...8..241S/EPRINT_PDF

['696', '498']

['Habitable zone', 'Exoplanets']

['Habitable zone', 'Exoplanets']

2021pds..data..174N

PDS4 Data Providers Handbook DPH version 1.16.0 2021

2021-01-01T00:00:00Z

['1.16.0', '2021', 'PDS', 'PDS4', 'data', 'dph', 'handbook', 'pds4', "provider's", 'version']

PDS4 Planetary Science Data Providers Handbook DPH Version 1.16.0

https://ui.adsabs.harvard.edu/link_gateway/2021pds..data..174N/EPRINT_PDF

['2021']

['Exoplanet atmospheric composition ']

['Exoplanet atmospheric composition ']

2021pds..data..176N

PDS4 Concepts version 1.16.0 2021

2021-01-01T00:00:00Z

['1.16.0', '2021', 'PDS', 'PDS4', 'concept', 'pds4', 'version']

PDS4 Planetary Science Concepts Version 1.16.0

https://ui.adsabs.harvard.edu/link_gateway/2021pds..data..176N/EPRINT_PDF

['2021']

['Exoplanet atmospheric composition ']

['Exoplanet atmospheric composition ']

2022PASP..134k5002L

Since the idea of bionic Lobster eye micropore optics was put forward the possibility of focusing hard Xrays by this new lightweight Xray optics has been proposed. Limited by the technological conditions of the aspect ratio 500 low surface roughness 1 nm and the difficulty of applying metal coatings inside such narrow square channels the high quality of these new optics have not been realized. This work demonstrates the test results for an Ultrahigh aspect ratio 5001 of iridiumcoated with microchannel plate technology and atomic layer deposition technology. The sidewalls of the square channel are smoothed with a special acidbase treatment and the RootMeanSquare of the inner wall was 0.52 0.1 nm in 3 m 3 m scale roughness such that they work well as Xray mirrors. The thickness of the metal iridium film layer was 19 nm. At the working voltage of 2 kV the current was 0.1 mA and the angular resolution of the slumped chip in horizontal and vertical directions was 3.9 and 4.2 respectively. The simulation results were in good agreement with the Xray test results.

2022-11-01T00:00:00Z

['X-ray transient sources', 'X-ray telescopes', 'X-ray astronomy', 'X-ray surveys', 'X-ray identification', '1852', '1825', '1810', '1824', '1817']

Fabrication and Performance of Lobster Eye XRay Micro Pore Optics with the Ultrahigh Aspect Ratio

https://ui.adsabs.harvard.edu/link_gateway/2022PASP..134k5002L/EPRINT_PDF

['1852', '1825', '1810', '1824', '1817']

['X-ray transient sources', 'X-ray telescopes', 'X-ray astronomy', 'X-ray surveys', 'X-ray identification']

['X-ray transient sources', 'X-ray telescopes', 'X-ray astronomy', 'X-ray surveys', 'X-ray identification']

2022ApJ...941...29L

Theoretical absorption oscillator strengths and wavelengths for rotational transitions of the C SUP2SUPv 0X SUP2SUPv bands with v 06 of nitric oxide are reported. The Molecular Quantum Defect Orbital method has been used in the calculations and the known interaction between the C SUP2SUPv 0 Rydberg and the B SUP2SUP v 7 valence states has been dealt with through an appropriate rovibronic energy matrix. We hope that the reported data may be useful in the analysis of the observed ultraviolet nightglow emission from nitric oxide in the upper atmospheres of Earth Venus and Mars.

2022-12-01T00:00:00Z

['Molecular spectroscopy', 'Line intensities', 'Line positions', '2095', '2084', '2085']

Transition Energies and Line Oscillator Strengths of the C SUP2SUP0X SUP2SUP06 Absorption Bands of Nitric Oxide. A Theoretical Study

https://ui.adsabs.harvard.edu/link_gateway/2022ApJ...941...29L/EPRINT_PDF

['2095', '2084', '2085']

['Molecular spectroscopy', 'Line intensities', 'Line positions']

['Molecular spectroscopy', 'Line intensities', 'Line positions']

2022pds..data...25D

Localization position and orientation information for the Mars 2020 Perseverence Rover

2022-01-01T00:00:00Z

['2020', 'PDS', 'PDS4', 'derived', 'information', 'localization', 'mars', 'mission', 'orientation', 'perseverence', 'position', 'rover', 'science']

Mars 2020 Rover PLACES Bundle

https://ui.adsabs.harvard.edu/link_gateway/2022pds..data...25D/EPRINT_PDF

['2020']

['Exoplanet atmospheric variability']

['Exoplanet atmospheric variability']

2021pds..data..149H

This bundle contains crustal magnetic field maps and equivalent source dipole arrays for Mercury based on the MESSENGER magnetic field data. This work was funded by a 2016 NASA ROSES DDAP proposal. Grant number NNH16ZDA001NDDAP.

2021-01-01T00:00:00Z

['2016', 'PDS', 'PDS4', 'array', 'based', 'bundle', 'contains', 'crustal', 'data', 'ddap', 'derived', 'dipole', 'equivalent', 'field', 'funded', 'grant', 'mag', 'magnetic', 'magnetometer', 'map', 'mercury', 'messenger', 'nasa', 'nnh16zda001n-ddap', 'number', 'proposal', 'rose', 'science', 'source', 'work']

MESSENGER MAG Crustal Field Map

https://ui.adsabs.harvard.edu/link_gateway/2021pds..data..149H/EPRINT_PDF

['2016']

['Quenched galaxies']

['Quenched galaxies']

2022RNAAS...6...69M

The analysis of high resolution SWP spectra obtained through the large aperture with the International Ultraviolet Explorer reveals that the farultraviolet flux of Oct did not vary. In particular the flux remained stable in a series of seven spectra taken consecutively over 3 hr and 24 minutes. This time interval is much shorter than the 1.78 days rotational period proposed for this star from its TESS lightcurve which could explain for the absence of variability in the FUV. The comparison of the STIS spectrum of Oct in the range 13001340 with synthetic spectra computed for the fundamental parameters of Oct and a solar composition allows the identification of the strongest absorption features in the farultraviolet as due to resonance lines of O I Si II and C II.

2022-04-01T00:00:00Z

['Pulsating variable stars', '1307']

The Absence of Far UV Variability in the IUE Spectra of Oct HD 215573

https://ui.adsabs.harvard.edu/link_gateway/2022RNAAS...6...69M/EPRINT_PDF

['1307']

['Pulsating variable stars']

['Pulsating variable stars']

2023ApJ...958..159C

In 1972 early August a series of interplanetary shocks were observed in the heliosphere from 0.8 to 2.2 au. These shocks were attributed to a series of brilliant flares and plasma clouds since at that time coronal mass ejections CMEs and their interplanetary counterparts ICMEs were unknown to the scientific community. This paper aims to reinterpret the interplanetary data in light of the current understanding about interplanetary transients and to track the evolution of the ICMEs taking advantage of the alignment of Pioneers 9 and 10 spacecraft. For this purpose we reanalyze in situ data from these two Pioneers and also from Heos Prognoz 1 and 2 and Explorer 41 spacecraft searching for ICMEs and highspeed streams. Then we assemble the interplanetary transients and solar activity and analyze the propagation of the ejections through the heliosphere. The evolution of four ICMEs and a highspeed stream from a lowlatitude coronal hole is followed using the multipoint in situ observations. The first three ICMEs show clear signatures of ICMEICME interaction in the interplanetary medium suggesting the first observations of an ICME which developed into an ICMEinthesheath. For a nonperturbed ICME event we obtain the evolution parameter related to the local expansion of ICMEs getting similar values for Pioneer 9 0.80 and Pioneer 10 0.78. These results support previous findings of being independent of the heliocentric distance and the magnetic field strength decreasing as r SUP2 SUP.

2023-12-01T00:00:00Z

['Solar activity', 'Interplanetary shocks', 'Solar flares', 'Solar coronal mass ejections', '1475', '829', '1496', '310']

Interplanetary Signatures during the 1972 Early August Solar Storms

https://ui.adsabs.harvard.edu/link_gateway/2023ApJ...958..159C/EPRINT_PDF

['1475', '829', '1496', '310']

['Solar activity', 'Interplanetary shocks', 'Solar flares', 'Solar coronal mass ejections']

['Solar activity', 'Interplanetary shocks', 'Solar flares', 'Solar coronal mass ejections']

2020ApJ...899...43C

Observations show that particle velocity distributions in space plasmas generally exhibit a nonMaxwellian highenergy tail that can be well fitted with kappa distributions. To better understand the correlation between realistic particle velocity distributions and plasma wave excitation we investigate the linear cyclotron instability of multiband electromagnetic ion cyclotron EMIC waves in a kappa plasma containing hot anisotropic protons which provides the free energy for the wave growth. We find that the effects of superthermal plasmas on EMIC wave instability have a strong dependence on the emission band temperature anisotropy ASUBhpSUB and parallel beta SUBhpSUB of hot protons. For HSUPSUP and HeSUPSUP band EMIC waves the maximum growth rates exhibit distinct behaviors with the variation of the spectral index of kappa distributions for different ASUBhpSUB values. The maximum growth rates decrease with increasing value for low ASUBhpSUB and increase with increasing value for high ASUBhpSUB. For OSUPSUP band waves the effects of superthermal plasmas on the maximum growth rate are strongly controlled by SUBhpSUB. For low SUBhpSUB the growth rate decreases monotonically with increasing value for all ASUBhpSUB. For high SUBhpSUB increase of value tends to enhance the wave growth for intermediate ASUBhpSUB and to suppress the wave growth otherwise. Our results also indicate that the presence of a highenergy tail tends to decrease the real frequency corresponding to the maximum growth rate for all three bands. While the minimum electron resonant energy for OSUPSUP band EMIC waves decreases as the value increases the minimum electron resonant energies for HSUPSUP and HeSUPSUP band waves remain unaffected.

2020-08-01T00:00:00Z

['Van Allen radiation belt', 'Planetary magnetosphere', 'Space plasmas', '1758', '997', '1544']

Effects of Superthermal Plasmas on the Linear Growth of Multiband EMIC Waves

https://ui.adsabs.harvard.edu/link_gateway/2020ApJ...899...43C/EPRINT_PDF

['1758', '997', '1544']

['Van Allen radiation belts', 'Planetary magnetospheres', 'Space plasmas']

['Van Allen radiation belts', 'Planetary magnetospheres', 'Space plasmas']

2020ApJ...888...10T

Electron excitation collision strengths and transition probabilities Avalues for the ironpeak element Cr II lines are of high importance for the stellar and nebular abundance studies. Collision and radiative parameters are presented for all possible inelastic transitions between the Cr II 512 finestructure levels covering infrared to extreme ultraviolet lines. These parameters should allow a detailed modeling and analysis of the available measured stellar and nebular spectra from different astrophysical objects. Accurate target wave functions have been generated using the multiconfiguration HartreeFock method together with termdependent oneelectron orbitals and wellchosen configuration expansions. The wave functions are then used in the calculations of transition probabilities and collision rates. The Bspline BreitPauli Rmatrix method has been employed for the calculation of electron excitation collision strengths. The semiempirical finetuning procedure has been applied to the energies of the local supercluster LS terms prior to transformation of the Hamiltonian matrices to intermediate coupling. The Hamiltonian matrices for the calculation of collision rates also include spinorbit interaction. The 512 finestructure levels of the Cr II 3d SUP5SUP 3d SUP4SUP4s 3dSUP3SUP4sSUP2SUP 3d SUP4SUP4p and 3d SUP3SUP4s4p configurations have been considered in our work. The thermally averaged collision strengths have been determined using a Maxwellian distribution for a wide range of temperatures from 10SUP2SUP to 10SUP5SUP K. The accuracy of our results has been estimated by comparison with other calculated collision rates and available measured radiative rates.

2020-01-01T00:00:00Z

['Atomic spectroscopy', 'Laboratory astrophysics', '2099', '2004']

Collision and Radiative Parameters for Cr II Lines Observed in Stellar and Nebular Spectra

https://ui.adsabs.harvard.edu/link_gateway/2020ApJ...888...10T/EPRINT_PDF

['2099', '2004']

['Atomic spectroscopy', 'Laboratory astrophysics']

['Atomic spectroscopy', 'Laboratory astrophysics']

2020ApJ...892...10J

Energetic ions in Mercurys magnetosphere are very dynamic similar to those in the magnetosphere of Earth. In this study we present two energetic proton observations by MErcury Surface Space ENvironment GEochemistry and Ranging near the cusp region of Mercury. For one case we have observed a large flux of energetic protons while the other case has almost no flux indicating that the nearcusp region may trap energetic particles under particular conditions. In order to understand under what conditions the nearcusp region of Mercury could trap energetic particles we have used test particle simulations to trace the trajectories of single particles of different energies and pitch angles with a magnetic field model KT17 that could closely represent the observed in situ magnetic field. Under different magnetic field geometries the motions of single particles with various energies and pitch angles are different. The test particles can be trapped around the cusp region when the solar disturbance activity that generates the magnetic field local minimum near the cusp region is strong while the particles cannot be trapped and escape along the magnetic field through the dawnside cusp when there is little solar activity.

2020-03-01T00:00:00Z

['Plasma physics', 'Mercury (planet)', 'Planetary magnetospheres', 'Space plasmas', '2089', '1024', '997', '1544']

Energetic Ion Dynamics Near the Cusp Region of Mercury

https://ui.adsabs.harvard.edu/link_gateway/2020ApJ...892...10J/EPRINT_PDF

['2089', '1024', '997', '1544']

['Plasma physics', 'Mercury (planet)', 'Planetary magnetospheres', 'Space plasmas']

['Plasma physics', 'Mercury (planet)', 'Planetary magnetospheres', 'Space plasmas']

2020ApJ...891..100S

Pyroxenes Ca Mg Fe MnSUB2SUBSiSUB2SUBOSUB6SUB belong to the most abundant rock forming minerals that make up the surface of rocky planets and moons. Therefore sputtering of pyroxenes by solar wind ions has to be considered as a very important process for modifying the surface of planetary bodies. This is increased due to potential sputtering by multiply charged ions to quantify this effect sputtering of wollastonite CaSiOSUB3SUB by HeSUP2SUP ions was investigated. Thin films of CaSiOSUB3SUB deposited on a quartz crystal microbalance were irradiated allowing precise in situ real time sputtering yield measurements. Experimental results were compared with SDTrimSP simulations which were improved by adapting the used input parameters. On freshly prepared surfaces HeSUP2SUP ions show a significant increase in sputtering as compared to equally fast HeSUPSUP ions. However the yield decreases exponentially with fluence reaching a lower steady state after sputtering of the first few monolayers. Experiments using ArSUP8SUP ions show a similar behavior which is qualitatively explained by a preferential depletion of surface oxygen due to potential sputtering. A corresponding quantitative model is applied and the observed potential sputtering behaviors of both He and Ar are reproduced very well. The results of these calculations support the assumption that mainly O atoms are affected by potential sputtering. Based on our findings we discuss the importance of potential sputtering for the solar wind eroding the lunar surface. Estimated concentration changes and sputtering yields are both in line with previous modeling for other materials allowing a consistent perspective on the effects of solar wind potential sputtering.

2020-03-01T00:00:00Z

['Solar wind', 'Exosphere', 'The Moon', 'Lunar composition', 'Mercury (planet)', 'Laboratory astrophysics', '1534', '499', '1692', '948', '1024', '2004']

Dynamic Potential Sputtering of Lunar Analog Material by Solar Wind Ions

https://ui.adsabs.harvard.edu/link_gateway/2020ApJ...891..100S/EPRINT_PDF

['1534', '499', '1692', '948', '1024', '2004']

['Solar wind', 'Exosphere', 'The Moon', 'Lunar composition', 'Mercury (planet)', 'Laboratory astrophysics']

['Solar wind', 'Exosphere', 'The Moon', 'Lunar composition', 'Mercury (planet)', 'Laboratory astrophysics']

2021pds..data..144R

This collection contains electron browse data from the Plasma experiment PLS on Voyager 1 from the Saturn encounter. The data includes 96 second averages of the electron 105950 eV density and temperature measurements.

2021-01-01T00:00:00Z

['1', '10-5950', '96', 'PDS', 'PDS4', 'average', 'browse', 'collection', 'contains', 'data', 'density', 'electron', 'encounter', 'ev', 'experiment', 'includes', 'measurement', 'plasma', 'pls', 'saturn', 'science', 'second', 'temperature', 'titan', 'voyager']

Voyager 1 Plasma Science Experiment PLS Saturn Derived Electron Browse 96 Second Data Collection

https://ui.adsabs.harvard.edu/link_gateway/2021pds..data..144R/EPRINT_PDF

['1', '96']

['Unknown', 'Particle astrophysics']

['Unknown', 'Particle astrophysics']

2020ApJ...893...83T

Recent numerical simulations of rotating stellar convection have suggested the possible existence of retrograde slow equator fast poles or socalled antisolar differential rotation states in slowly rotating stars possessing a large Rossby number. We aim to understand whether such rotational states exist from the onset of convective instability or are the outcome of complex nonlinear interactions in the turbulent convective envelope. To this end we have made a systematic linear analysis of the critical state of convection in a series of 15 numerical simulations published in Brun et al. We have assessed their degree of supercriticality and mostunstable mode properties and computed the secondorder mean zonal flow response. We find that none of the linear critical cases show a retrograde state at the onset of convection even when their nonlinear counterparts do. We also find that the presence of a stably stratified layer coupled to the convectively unstable upper layer leads to interesting gravitywave excitation and angular momentum transport. We conclude that retrograde states of differential rotation are probably the outcome of complex modemode interactions in the turbulent convection layer and are as a consequence likely to exist in real stars.

2020-04-01T00:00:00Z

['Stellar convective zones', 'Stellar interiors', 'Astrophysical fluid dynamics', 'Internal waves', 'Stellar rotation', '301', '1606', '101', '819', '1629']

Assessment of Critical Convection and Associated Rotation States in Models of Sunlike Stars Including a Stable Layer

https://ui.adsabs.harvard.edu/link_gateway/2020ApJ...893...83T/EPRINT_PDF

['301', '1606', '101', '819', '1629']

['Stellar convective zones', 'Stellar interiors', 'Astrophysical fluid dynamics', 'Internal waves', 'Stellar rotation']

['Stellar convective zones', 'Stellar interiors', 'Astrophysical fluid dynamics', 'Internal waves', 'Stellar rotation']

2020ApJ...894...41R

It has been suggested by Weinberg et al. that an instability due to the nonlinear coupling of a neutron stars tide to its p and gmodes could affect the gravitationalwave phase evolution of a neutron star binary. Weinberg suggests that this instability can turn on as the gravitational waves pass through the sensitive band of groundbased detectors although the size of the effect is not known. The discovery of the binary neutron star merger GW170817 provides an opportunity to look for evidence of nonlinear tides from pg mode coupling. We compute Bayesian evidences that compare waveform models that include the pg mode coupling with models that do not. We find that the consistency between GW170817 signal and the pg mode model reported by Abbott et al. is due to a degeneracy between the phenomenological waveform used to model the effect of nonlinear tides and the standard postNewtonian waveform. We investigate the consistency of the GW170817 signal with regions of the parameter space where the effect of nonlinear tides is not degenerate with the standard model. Regions of the nonlinear tide parameter space that have a fitting factor of less than 99 98.5 are disfavored by a Bayes factor of 15 25. We conclude that regions of the parameter space where nonlinear tides produce a measurable effect are strongly disfavored and improved theoretical modeling will be needed if future observations are to constrain nonlinear tides from pg mode coupling in neutron stars.

2020-05-01T00:00:00Z

['Neutron stars', 'Close binary stars', 'Gravitational waves', 'Compact binary stars', '1108', '254', '678', '283']

Constraints on Nonlinear Tides due to pg Mode Coupling from the Neutron Star Merger GW170817

https://ui.adsabs.harvard.edu/link_gateway/2020ApJ...894...41R/EPRINT_PDF

['1108', '254', '678', '283']

['Neutron stars', 'Close binary stars', 'Gravitational waves', 'Compact binary stars']

['Neutron stars', 'Close binary stars', 'Gravitational waves', 'Compact binary stars']

2023RNAAS...7..113S

Photometric H observations of the young open cluster King 16 have been used to search for emissionline stars. Seven cluster members with enhanced H emission are identified of which five are new discoveries. Three of these newly found objects have a nearinfrared excess which suggests they may be Herbig AeBe stars. H emission is also present in three field stars of which two are new detections.

2023-06-01T00:00:00Z

['Be stars', 'Herbig Ae/Be stars', 'Open star clusters', '142', '723', '1160']

A Photometric H Survey of the Open Cluster King 16

https://ui.adsabs.harvard.edu/link_gateway/2023RNAAS...7..113S/EPRINT_PDF

['142', '723', '1160']

['Be stars', 'Herbig Ae/Be stars', 'Open star clusters']

['Be stars', 'Herbig Ae/Be stars', 'Open star clusters']

2021pds..data..153V

This collection contains Voyager 2 Jupiter CRS derived pulse height ion one hour averaged data

2021-01-01T00:00:00Z

['2', 'PDS', 'PDS4', 'averaged', 'collection', 'contains', 'cosmic', 'cr', 'data', 'derived', 'ganymede', 'height', 'hour', 'ion', 'jupiter', 'one', 'pulse', 'ray', 'subsystem', 'voyager']

Voyager 2 Jupiter CRS Derived Pulse Height Ion Averaged Data Collection

https://ui.adsabs.harvard.edu/link_gateway/2021pds..data..153V/EPRINT_PDF

['2']

['53 Persei stars']

['53 Persei stars']

2021pds..data..152V

This collection contains Voyager 2 Jupiter CRS 15 minute averaged ion data.

2021-01-01T00:00:00Z

['15', '2', 'PDS', 'PDS4', 'averaged', 'collection', 'contains', 'cosmic', 'cr', 'data', 'ganymede', 'ion', 'jupiter', 'minute', 'ray', 'subsystem', 'voyager']

Voyager 2 Jupiter CRS Derived Ion Averaged Data Collection

https://ui.adsabs.harvard.edu/link_gateway/2021pds..data..152V/EPRINT_PDF

['15', '2']

['Achondrites', '53 Persei stars']

['Achondrites', '53 Persei stars']

2021pds..data..141R

This collection contains electron fit data from the Plasma experiment PLS on Voyager 1 from the Saturn encounter. The data includes 96 second res. density and temperature measurements for various types of electrons 105950 eV.

2021-01-01T00:00:00Z

['1', '10-5950', '96', 'PDS', 'PDS4', 'collection', 'contains', 'data', 'density', 'electron', 'encounter', 'ev', 'experiment', 'fit', 'includes', 'measurement', 'plasma', 'pls', 're', 'saturn', 'science', 'second', 'temperature', 'titan', 'type', 'various', 'voyager']

Voyager 1 Plasma Science Experiment PLS Saturn Derived Electron Parameters 96 Second Data Collection

https://ui.adsabs.harvard.edu/link_gateway/2021pds..data..141R/EPRINT_PDF

['1', '96']

['Unknown', 'Particle astrophysics']

['Unknown', 'Particle astrophysics']

2021pds..data..139R

This collection contains ion browse data from the Plasma experiment PLS on Voyager 1 from the Saturn encounter. The data includes 96 second density temperature and velocity components for proton and heavy ions.

2021-01-01T00:00:00Z

['1', '96', 'PDS', 'PDS4', 'browse', 'collection', 'component', 'contains', 'data', 'density', 'encounter', 'experiment', 'heavy', 'includes', 'ion', 'plasma', 'pls', 'proton', 'saturn', 'science', 'second', 'temperature', 'titan', 'velocity', 'voyager']

Voyager 1 Plasma Science Experiment PLS Saturn Derived Ion Fits Browse 96 Second Data Collection

https://ui.adsabs.harvard.edu/link_gateway/2021pds..data..139R/EPRINT_PDF

['1', '96']

['Unknown', 'Particle astrophysics']

['Unknown', 'Particle astrophysics']

2021pds..data..137R

This collection contains Voyager 1 Plasma PLS ion data from the Saturns magnetosheath. The data includes 96 second data of the ion mass charge density velocity and thermal speed for the first and second ion species.

2021-01-01T00:00:00Z

['1', '96', 'PDS', 'PDS4', 'charge', 'collection', 'contains', 'data', 'density', 'experiment', 'first', 'includes', 'ion', 'magnetosheath', 'mass', 'plasma', 'pls', 'saturn', "saturn's", 'science', 'second', 'specie', 'speed', 'thermal', 'titan', 'velocity', 'voyager']

Voyager 1 Plasma Science Experiment PLS Saturn Derived Ion Magnetosheath 96 Second Data Collection

https://ui.adsabs.harvard.edu/link_gateway/2021pds..data..137R/EPRINT_PDF

['1', '96']

['Unknown', 'Particle astrophysics']

['Unknown', 'Particle astrophysics']

2021pds..data..138N

This collection contains Voyager 1 Saturn encounter ephemeris data in Kronographic L1 coordinates covering the period 19801110 to 19801118. The data was generated by the Voyager MAG team from Voyager SEDR. Due to inaccuracies in Voyager SEDR as well as changes in the values of some key parameters e.g. Saturnian radius the timing is improved for the SPICE generated data which is also included in this bundle.

2021-01-01T00:00:00Z

['1', '1980-11-10', '1980-11-18', 'PDS', 'PDS4', 'also', 'bundle', 'change', 'collection', 'contains', 'coordinate', 'covering', 'data', 'due', 'e.g', 'encounter', 'ephemeris', 'generated', 'improved', 'inaccuracy', 'included', 'key', 'kronographic', 'l1', 'mag', 'parameter', 'period', 'radius', 'saturn', 'saturnian', 'sedr', 'spice', 'team', 'timing', 'titan', 'value', 'voyager', 'well']

Voyager 1 Saturn POS Ephemeris Kronographic L1 Coords Browse SEDR Data Collection

https://ui.adsabs.harvard.edu/link_gateway/2021pds..data..138N/EPRINT_PDF

['1']

['Unknown']

['Unknown']

2018GeoRL..45.3615K

Here we demonstrate that changes of the North Atlantic subtropical high and its regional rainfall pattern during midHolocene precessional changes and idealized 4xCOSUB2SUB increase can both be understood as a remote response to increased land heating near North Africa. Despite different sources and patterns of radiative forcing increase in COSUB2SUB concentration versus changes in orbital parameters we find that the pattern of energy circulation and rainfall responses in the Northern Hemisphere summer subtropics are remarkably similar in the two forcing scenarios because both are dominated by the same landsea heating contrast in response to the forcing. An increase in energy input over arid land drives a westward displacement of the coupled North Atlantic subtropical highmonsoon circulation consistent with increased precipitation in the AfroAsia region and decreased precipitation in the AmericaAtlantic region. This study underscores the importance of land heating in dictating remote drying through zonal shifts of the subtropical circulation.

2018-04-01T00:00:00Z

['3305', '3373', '3344', '3337', '3322']

Remote Drying in the North Atlantic as a Common Response to Precessional Changes and COSUB2SUB Increase Over Land

https://ui.adsabs.harvard.edu/link_gateway/2018GeoRL..45.3615K/EPRINT_PDF

['3305', '3373', '3344', '3337', '3322']

['Unknown', 'Unknown', 'Unknown', 'Unknown', 'Unknown']

['Unknown', 'Unknown', 'Unknown', 'Unknown', 'Unknown']

2019ApJ...885...25B

The relativistic mean field RMF model is considered as one of the best methods to study the nuclear system that has a high degree of isospin asymmetry and baryon density. In the present contribution we take 25 wellknown parameter sets of the RMF model to discuss the parametric dependence of the neutron and hyperon star properties. Various properties of the canonical star are discussed and only a few parameter sets are found to satisfy both the astrophysical and nuclear matter constraints. We add both and strange mesons to the model. Effects of the meson on the equation of state and maximum mass of the hyperon star are discussed in detail. meson affects the threshold density of hyperon production and pushes the hyperon production to a higher density. Effects of the hyperonmeson coupling constants on the maximum massradius profile and strangeness content of the hyperon star are discussed in the model.

2019-11-01T00:00:00Z

['Neutron stars', 'Compact objects', 'Nuclear astrophysics', 'Neutron star cores', '1108', '288', '1129', '1107']

Effects of meson on the EOS Maximum Masses and Radii of Hyperon Stars

https://ui.adsabs.harvard.edu/link_gateway/2019ApJ...885...25B/EPRINT_PDF

['1108', '288', '1129', '1107']

['Neutron stars', 'Compact objects', 'Nuclear astrophysics', 'Neutron star cores']

['Neutron stars', 'Compact objects', 'Nuclear astrophysics', 'Neutron star cores']

2021ApJ...909..132N

Faraday cups can measure velocity distribution functions of space plasmas and are frequent instruments on heliophysics missions. A new version of a Faraday cup instrument is in development for the Luna 26 mission and will be used for fast monitoring of the solar wind plasma parameters. The prototype of this instrument is exposed to dust impacts in a velocity range of 0.260 km sSUP1SUP using an electrostatic dust accelerator. The collected data are used to evaluate the sensitivity and detection efficiency of dust particles on two different surfaces. The results indicate that the sensitivity is sufficient for detection of the interplanetary dust as well as for the registration of the dust lifted from the lunar surface. A simple modification of the FC electronics would increase the detection efficiency by an order of magnitude.

2021-03-01T00:00:00Z

['Interplanetary dust', 'Interstellar dust', 'Solid matter physics', '821', '836', '2090']

Detection of Dust Particles Using Faraday Cup Instruments

https://ui.adsabs.harvard.edu/link_gateway/2021ApJ...909..132N/EPRINT_PDF

['821', '836', '2090']

['Interplanetary dust', 'Interstellar dust', 'Solid matter physics']

['Interplanetary dust', 'Interstellar dust', 'Solid matter physics']

2020PSJ.....1...76C

Acetylene and benzene are two common molecules formed in Titans atmosphere and are likely components of the lake evaporites. It is known that these two molecules can form a cocrystal a molecule with a structure that is unique from that of the component molecules. Thus we sought to study this cocrystal using an experimental setup that simulates Titan surface conditions 90 K 1.5 bar. Using Fourier transform infrared FTIR spectroscopy we characterize new spectral absorptions band shifts and morphological sample changes associated with this cocrystal from 1 to 2.6 m which overlaps with Cassini VIMS wavelength range 0.355.1 m. This is the first study of the resulting acetylenebenzene cocrystal under Titanrelevant temperature and pressure. The cocrystal forms at 135 K and is stable down to 90 K. Our findings can be applied to the cocondensation process in Titans atmosphere as well as the ongoing effort to better characterize the composition and spectral properties of Titans lake evaporites. These results can also provide a stepping stone to future surface missions such as Dragonfly which will closely examine relevant surface materials on Titan.

2020-12-01T00:00:00Z

['Molecular spectroscopy', 'Experimental techniques', 'Surface ices', '2095', '2078', '2117']

Experimental Investigation of the AcetyleneBenzene Cocrystal on Titan

https://ui.adsabs.harvard.edu/link_gateway/2020PSJ.....1...76C/EPRINT_PDF

['2095', '2078', '2117']

['Molecular spectroscopy', 'Experimental techniques', 'Surface ices']

['Molecular spectroscopy', 'Experimental techniques', 'Surface ices']

2020pds..data..138M

Raw data products for the Mars 2020 Perseverance Rover Hazard Cameras.

2020-01-01T00:00:00Z

['2020', 'PDS', 'PDS4', 'calibrated', 'camera', 'data', 'derived', 'engineering', 'hazard', 'instrument', 'mars', 'mission', 'partially', 'perseverance', 'processed', 'product', 'raw', 'rover', 'science', 'suite']

Mars 2020 Hazard Cameras Bundle raw products

https://ui.adsabs.harvard.edu/link_gateway/2020pds..data..138M/EPRINT_PDF

['2020']

['Exoplanet atmospheric variability']

['Exoplanet atmospheric variability']

2022ApJ...925..102G

We present analytic integral solutions for the secondorder induced gravitational waves GWs. After presenting all the possible secondorder source terms we calculate explicitly the solutions for the GWs induced by the linear scalar and tensor perturbations during matter and radiationdominated epochs.

2022-01-01T00:00:00Z

['343', '902', '678']

Analytic Integral Solutions for Induced Gravitational Waves

https://ui.adsabs.harvard.edu/link_gateway/2022ApJ...925..102G/EPRINT_PDF

['343', '902', '678']

['Cosmology', 'Large-scale structure of the universe', 'Gravitational waves']

['Cosmology', 'Large-scale structure of the universe', 'Gravitational waves']

2023RNAAS...7..207M

Analysis of coadded high resolution spectra of the chemically peculiar star HD 53929 recorded by the SWP and LWR cameras on board the International Ultraviolet Explorer yields estimates of the abundances of silicon and manganese respectively 1.5 and 6 times the solar abundances in the atmosphere of this star. The synthesis of the 44004500 range allows the determination of the abundances of helium magnesium phosphorus and iron. Compared to solar abundances helium is very underabundant 0.05 solar magnesium is also underabundant by a factor of 0.20 times the solar abundances. Phosphorus is overabundant by a factor of 20.

2023-10-01T00:00:00Z

['Chemically peculiar stars', 'Manganese stars', '226', '1004']

New Abundance Determinations for the B9 Mn Star HD 53929

https://ui.adsabs.harvard.edu/link_gateway/2023RNAAS...7..207M/EPRINT_PDF

['226', '1004']

['Chemically peculiar stars', 'Manganese stars']

['Chemically peculiar stars', 'Manganese stars']

2020ApJ...898...92C

The abundance of methyl formate MF HCOOCHSUB3SUB in starforming regions of the interstellar medium ISM suggests the presence of protonated MF HSUPSUPMF. However no spectroscopic data exist for isolated HSUPSUPMF. Here we address the vibrational properties of HSUPSUPMF and its HSUPSUPMFLSUBn2SUB clusters L ArNSUB2SUB by infrared photodissociation IRPD spectroscopy and density functional theory calculations. Protonation of MF occurs at the CO oxygen resulting in four different isomers arising from the synanti sa and cistrans ct orientation between OCHSUB3SUB and the excess proton. HSUPSUPMF photofragments into protonated methanol by CO elimination. The IRPD spectrum exhibits redshifted OH stretch bands of the most stable HSUPSUPMFts and HSUPSUPMFca conformers because of the high internal energy required for dissociation. Tagging of HSUPSUPMF with inert ligands drastically reduces both the internal energy and the dissociation threshold. The resulting higherresolution IRPD spectra allow determination of the most stable HSUPSUPMF rotamers as ts and ca. In the cold HSUPSUPMFL dimers the ligand forms an OH...L hydrogen bond while bonding to the positively charged 2pSUBzSUB orbital of the carbonyl C atom is less favorable. The latter allows estimation of the free OH stretch fundamental of the most stable HSUPSUPMFts rotamer as 3545 5 cmSUP1SUP. While for neutral MF the more stable syn rotamer MFs dominates the population in both the laboratory and the ISM gt99 the anti conformer is substantially populated for HSUPSUPMF 30 which is rationalized by protonationinduced isomerization. This mechanism may lead to an enhanced abundance of MFa in certain regions of the ISM.

2020-07-01T00:00:00Z

['Astrochemistry', 'Laboratory astrophysics', 'Interstellar medium', 'Molecular spectroscopy', 'Chemical abundances', 'Electron impact ionization', 'Molecule destruction', '75', '2004', '847', '2095', '224', '2059', '2075']

Vibrational Spectroscopy of a Potential Interstellar Ion Protonated Methyl Formate

https://ui.adsabs.harvard.edu/link_gateway/2020ApJ...898...92C/EPRINT_PDF

['75', '2004', '847', '2095', '224', '2059', '2075']

['Astrochemistry', 'Laboratory astrophysics', 'Interstellar medium', 'Molecular spectroscopy', 'Chemical abundances', 'Electron impact ionization', 'Unknown']

['Astrochemistry', 'Laboratory astrophysics', 'Interstellar medium', 'Molecular spectroscopy', 'Chemical abundances', 'Electron impact ionization', 'Unknown']

2021pds..data..183P

PRIMASSL at the Small Bodies Node SBN of the NASA Planetary Data System PDS is a spectral library that contains the results of the PRIMitive Asteroids Spectroscopic Survey PRIMASS. As of June 2021 this library gathers spectra of about 642 asteroids from 10 families and two groups of asteroids that had been sparsely studied before 85 of our targets did not have published spectra and only 40 had visible photometry. PRIMASSL contains spectra from a variety of groundbased facilities this survey is ongoing and is expected to contain about 800 spectra by the end of 2022.

2021-01-01T00:00:00Z

['Asteroids', '72']

PRIMASSL Spectra Bundle V1.0

https://ui.adsabs.harvard.edu/link_gateway/2021pds..data..183P/EPRINT_PDF

['72']

['Asteroids']

['Asteroids']

2021pds..data..178R

This collection contains ancillary data describing configuration of the Voyager 1 PLS Faraday detector cups.

2021-01-01T00:00:00Z

['1', 'PDS', 'PDS4', 'experiment', 'plasma', 'saturn', 'science', 'titan', 'voyager']

Voyager 1 Plasma Science Experiment PLS Saturn Faraday Cup Data Collection

https://ui.adsabs.harvard.edu/link_gateway/2021pds..data..178R/EPRINT_PDF

['1']

['Unknown']

['Unknown']

2021pds..data..172N

PDS4 Standards Reference version 1.16.0 2021

2021-01-01T00:00:00Z

['1.16.0', '2021', 'PDS', 'PDS4', 'pds4', 'reference', 'standard', 'version']

PDS4 Planetary Science Standards Reference Version 1.16.0

https://ui.adsabs.harvard.edu/link_gateway/2021pds..data..172N/EPRINT_PDF

['2021']

['Exoplanet atmospheric composition ']

['Exoplanet atmospheric composition ']

2019ApJ...885..122Z

Our recent investigations indicate that interplanetary magnetic clouds MCs have a hightwist core and a weaktwist outer shell. Utilizing the velocitymodified uniformtwist forcefree flux rope model we further investigate the relationship between the twist profile of magnetic field lines and the distribution of the plasma poloidal angular velocity inside an MC. The poloidal velocity in the MC is 11 km sSUP1SUP. There are evidently positive correlations between the absolute value of the twist and the plasma poloidal angular velocity in peeled flux ropes or flux rope layers although the correlation coefficients in flux rope layers are less than those in peeled flux ropes. This finding suggests that plasma flows are frozenin magnetic field lines as we expected for interplanetary medium of which the magnetic Reynolds number is large. Furthermore based on this picture we infer the axial velocity in the MC frame which is less than 10 km sSUP1SUP and almost uniform in the cross section of the MC. Besides it is inferred that the plasma flows velocity in the MC is much less than the local Alfvn speed.

2019-11-01T00:00:00Z

['Interplanetary magnetic fields', '824']

The Relationship of Magnetic Twist and Plasma Motion in a Magnetic Cloud

https://ui.adsabs.harvard.edu/link_gateway/2019ApJ...885..122Z/EPRINT_PDF

['824']

['Interplanetary magnetic fields']

['Interplanetary magnetic fields']

2021pds..data..166B

Terrain mesh data products for the Mars 2020 Perseverance Rover Mast Camera Zoom Camera created by the operations team.

2021-01-01T00:00:00Z

['2020', 'PDS', 'PDS4', 'calibrated', 'camera', 'created', 'data', 'derived', 'instrument', 'mars', 'mast', 'mastcam-zoom', 'mesh', 'mission', 'operation', 'partially', 'perseverance', 'processed', 'product', 'raw', 'rover', 'science', 'suite', 'team', 'terrain', 'zoom']

Mars 2020 Mast Camera Zoom Bundle from Operations Team terrain mesh products

https://ui.adsabs.harvard.edu/link_gateway/2021pds..data..166B/EPRINT_PDF

['2020']

['Exoplanet atmospheric variability']

['Exoplanet atmospheric variability']

2021RNAAS...5..239M

Evidence is presented that lanthanides are present and overabundant in the atmosphere of the sharplined A1 V star HR 4138. This interesting object needs to be reclassified as a Chemically Peculiar star.

2021-10-01T00:00:00Z

['Chemical abundances', 'Chemically peculiar stars', '224', '226']

The Occurrence of Lanthanides in the Atmosphere of the A1 V Star HR 4138

https://ui.adsabs.harvard.edu/link_gateway/2021RNAAS...5..239M/EPRINT_PDF

['224', '226']

['Chemical abundances', 'Chemically peculiar stars']

['Chemical abundances', 'Chemically peculiar stars']

2020ApJ...897L..39N

The solar wind nonradial velocity components observed beyond the Alfvn point are usually attributed to waves the interaction of different streams or other transient phenomena. However Earthorbiting spacecraft as well as monitors at L1 indicate systematic deviations of the wind velocity from the radial direction. Since these deviations are of the order of several degrees the calibration of the instruments is often questioned. This paper investigates for the first time the evolution of nonradial components of the solar wind flow along the path from 0.17 to 10 au. A comparison of observations at 1 au with those closer to or farther from the Sun based on measurements of many spacecraft at different locations in the heliosphere Parker Solar Probe Helios 1 and 2 Wind Advanced Composition Explorer SpektrR Acceleration Reconnection Turbulence and Electrodynamics of the Moons Interaction with the Sun ARTEMIS probes Mars Atmosphere and Volatile Evolution MAVEN Voyagers 1 and 2 shows that I the average values of nonradial components are not zero and vary in a systematic manner with the distance from the Sun and II their values significantly depend on the solar wind radial velocity.

2020-07-01T00:00:00Z

['Heliosphere', 'Solar wind', 'Fast solar wind', '711', '1534', '1872']

Nonradial Solar Wind Propagation through the Heliosphere

https://ui.adsabs.harvard.edu/link_gateway/2020ApJ...897L..39N/EPRINT_PDF

['711', '1534', '1872']

['Heliosphere', 'Solar wind', 'Fast solar wind']

['Heliosphere', 'Solar wind', 'Fast solar wind']

2022pds..data..114T

This version of the Photopolarimeter Radiometer PPR for GO bundle was created by the PDS Atmospheres node in 2022

2022-01-01T00:00:00Z

['2022', 'PDS', 'PDS4', 'amalthea', 'atmosphere', 'bundle', 'callisto', 'created', 'europa', 'galileo', 'ganymede', 'gll', 'go', 'io', 'jupiter', 'node', 'orbiter', 'pct', 'pds', 'photopolarimeter', 'ppr', 'radiometer', 'rct', 'version']

Galileo Orbiter Photopolarimeter Radiometer PPR for GO Bundle

https://ui.adsabs.harvard.edu/link_gateway/2022pds..data..114T/EPRINT_PDF

['2022']

['Exoplanet surface composition']

['Exoplanet surface composition']

2021pds..data...85H

This bundle contains the MESSENGER Energetic Particle and Plasma Spectrometer EPPS calibrated observations also known as DDRs. The system encompasses 2 instrument subsystems the Energetic Particle Spectrometer EPS and the Fast Imaging Plasma Spectrometer FIPS. This data set contains FIPS instrument data. FIPS covers the energycharge range of less than 46 eVq to 13 keVq. There are six FIPS DDR data products. These data were previously released as a PDS data set MESSEVHSWEPPS3FIPSDDRV1.0 httpsdoi.org10.171891519743

2021-01-01T00:00:00Z

['13', '2', '46', 'PDS', 'PDS4', 'also', 'bundle', 'calibrated', 'contains', 'cover', 'data', 'ddr', 'ddrs', 'earth', 'encompasses', 'energetic', 'energy/charge', 'epps', 'eps', 'ev/q', 'fast', 'fips', 'https://doi.org/10.17189/1519743', 'imaging', 'instrument', 'kev/q', 'known', 'le', 'mercury', 'mess-e/v/h/sw-epps-3-fips-ddr-v1.0', 'messenger', 'observation', 'particle', 'pds', 'plasma', 'previously', 'product', 'range', 'released', 'set', 'six', 'solar', 'spectrometer', 'subsystem', 'system', 'venus', 'wind']

Messenger Epps Fips DDR Bundle

https://ui.adsabs.harvard.edu/link_gateway/2021pds..data...85H/EPRINT_PDF

['13', '2', '46']

['Unknown', '53 Persei stars', 'Antapex']

['Unknown', '53 Persei stars', 'Antapex']

2021pds..data...78H

This bundle contains MESSENGER Energetic Particle and Plasma Spectrometer EPPS advanced data products also known as DDRDAPs. This bundle contains data from the Energetic Particle Spectrometer EPS subsystem. EPS covers the energy range of 25 to gt 500 keV for electrons and 10 keVnucleon to 3 MeV total energy for ions. These data were previously released as a PDS data set MESSEVHSWEPPS3EPSDDRV1.0 httpsdoi.org10.171891519741.

2021-01-01T00:00:00Z

['10', '25', '3', '500', 'PDS', 'PDS4', 'advanced', 'also', 'bundle', 'contains', 'cover', 'data', 'ddr/daps', 'earth', 'electron', 'energetic', 'energy', 'epps', 'eps', 'https://doi.org/10.17189/1519741', 'ion', 'kev', 'kev/nucleon', 'known', 'mercury', 'mess-e/v/h/sw-epps-3-eps-ddr-v1.0', 'messenger', 'mev', 'particle', 'pds', 'plasma', 'previously', 'product', 'range', 'released', 'set', 'solar', 'spectrometer', 'subsystem', 'total', 'venus', 'wind']

Messenger Epps EPS DDR Bundle

https://ui.adsabs.harvard.edu/link_gateway/2021pds..data...78H/EPRINT_PDF

['10', '25', '3', '500']

['Absolute magnitude', 'All-sky cameras', 'A dwarf stars', 'Exozodiacal dust']

['Absolute magnitude', 'All-sky cameras', 'A dwarf stars', 'Exozodiacal dust']

2021pds..data...69R

This bundle contains MESSENGER Energetic Particle and Plasma Spectrometer EPPS calibrated observations also known as CDRs. This bundle contains Fast Imaging Plasma Spectrometer FIPS instrument data. FIPS covers the energycharge range of less than 50 eVq to 20 keVq. These data were previously released as a PDS3 data set MESSEVHSWEPPS3FIPSCDRV1.0 httpsdoi.org10.171891519742.

2021-01-01T00:00:00Z

['20', '50', 'PDS', 'PDS4', 'also', 'bundle', 'calibrated', 'cdrs', 'contains', 'cover', 'data', 'earth', 'energetic', 'energy/charge', 'epps', 'ev/q', 'fast', 'fips', 'https://doi.org/10.17189/1519742', 'imaging', 'instrument', 'kev/q', 'known', 'le', 'mercury', 'mess-e/v/h/sw-epps-3-fips-cdr-v1.0', 'messenger', 'observation', 'particle', 'pds3', 'plasma', 'previously', 'range', 'released', 'set', 'solar', 'spectrometer', 'venus', 'wind']

MESSENGER EPPS Calibrated FIPS Data Bundle

https://ui.adsabs.harvard.edu/link_gateway/2021pds..data...69R/EPRINT_PDF

['20', '50']

['Ae stars', 'Ap stars']

['Ae stars', 'Ap stars']

2022RNAAS...6...90O

We use a nearest neighbor algorithm combined with the machine learning clustering function DensityBased Spatial Clustering of Applications with Noise to analyze a subset of quasars from the Sloan Digital Sky Survey. Our analysis shows evidence of clustering up to z 2 with evidence of an increase in clustering at lower redshifts z lt 0.5. Our findings may suggest that over time the gravitational interaction between quasars has led to more clustering at low redshifts.

2022-05-01T00:00:00Z

['Quasars', 'Clustering', '1319', '1908']

The Study of Quasar Clustering at Low Redshifts

https://ui.adsabs.harvard.edu/link_gateway/2022RNAAS...6...90O/EPRINT_PDF

['1319', '1908']

['Quasars', 'Clustering']

['Quasars', 'Clustering']

2021pds..data..145R

This collection contains ion fit data from the Plasma experiment PLS on Voyager 1 in Saturns magnetosphere. The data includes 96 second ion mass charge number of ion species density thermal speed velocity for the first and second ion species.

2021-01-01T00:00:00Z

['1', '96', 'PDS', 'PDS4', 'charge', 'collection', 'contains', 'data', 'density', 'experiment', 'first', 'fit', 'includes', 'ion', 'magnetosphere', 'mass', 'number', 'plasma', 'pls', 'saturn', "saturn's", 'science', 'second', 'specie', 'speed', 'thermal', 'titan', 'velocity', 'voyager']

Voyager 1 Plasma Science Experiment PLS Saturn Derived Ion Fits 96 Second Data Collection

https://ui.adsabs.harvard.edu/link_gateway/2021pds..data..145R/EPRINT_PDF

['1', '96']

['Unknown', 'Particle astrophysics']

['Unknown', 'Particle astrophysics']

2023RNAAS...7...66W

Our knowledge about the multiplicity of intermediate mass A and Btype stars is still incomplete in particular for high 3 multiplicity systems. Here we report the discovery of a new companion to the nearby roAp star HIP 47145 HR 3831 with a K band flux ratio of 4 based on a VLTIGRAVITY interferometric observation. This new 0.64M SUBSUB companion at a projected separation 187.5 mas 13.40 au explains the HipparcosGaiaDR2 proper motion change of HR 3831. Together with the previously known M 1M SUBSUB companion at 3 214 au this makes HR 3831 a hierarchical triple and a very likely progenitor for a system similar to 40 Eridani. Based on observations collected at the European Southern Observatory Chile Program ID 110.241W.002.

2023-04-01T00:00:00Z

['Multiple stars', 'Ap stars', 'Optical interferometry', '1081', '50', '1168']

Discovery of a 0.64 M SUBSUB 13.4 au Companion to the roAp Star HIP 47145 HR 3831 IM Vel

https://ui.adsabs.harvard.edu/link_gateway/2023RNAAS...7...66W/EPRINT_PDF

['1081', '50', '1168']

['Multiple stars', 'Ap stars', 'Optical interferometry']

['Multiple stars', 'Ap stars', 'Optical interferometry']

2023RNAAS...7..208V

We discuss the discovery of a significant meteoric event over Don Benito Spain described in two news reports from the regional newspaper Extremadura. These reports detail intense light loud noises and shattered windows in Don Benito during 1926 December. Despite limited information this research note aims to share the findings with the scientific community for further investigation.

2023-10-01T00:00:00Z

['Bolides', '172']

A Possible Superbolide Over Don Benito Spain in 1926 December 27

https://ui.adsabs.harvard.edu/link_gateway/2023RNAAS...7..208V/EPRINT_PDF

['172']

['Bolides']

['Bolides']

2023RNAAS...7...84D

In this study we used archival supernova data from a publicly available database to look for a blue excess in the early light curves of SN Ia. This blue excess represents a simple proposed method to differentiate between single and doubledegenerate formation scenarios. Our search found 2 candidates out of 40 SN Ia and including selection effects implies an upper limit of 50 of the supernovae in the sample originated in a binary with a nondegenerate companion.

2023-05-01T00:00:00Z

['Type Ia supernovae', 'White dwarf stars', 'Degenerate matter', 'Optical astronomy', 'Light curves', 'Astronomy databases', '1728', '1799', '367', '1776', '918', '83']

Looking for the Blue Bump in the Early Light Curve of SN Ia using an Open Supernovae Catalog

https://ui.adsabs.harvard.edu/link_gateway/2023RNAAS...7...84D/EPRINT_PDF

['1728', '1799', '367', '1776', '918', '83']

['Type Ia supernovae', 'White dwarf stars', 'Degenerate matter', 'Optical astronomy', 'Light curves', 'Astronomy databases']

['Type Ia supernovae', 'White dwarf stars', 'Degenerate matter', 'Optical astronomy', 'Light curves', 'Astronomy databases']

2021PSJ.....2...28C

The Mars Reconnaissance Orbiters Shallow Radar SHARAD emits radar signals and records their reflections from layer boundaries within the Martian north polar ice cap. Previous studies have suggested that the ice cap is composed of thin dustrich layers between thicker layers of nearly pure water ice. The prevailing hypotheses suggest that each dustrich layer represents either a period of ice sublimation at the poles or a period of reduced ice deposition relative to dust deposition. To test whether thin dust beds are a plausible hypothesis for the observed SHARAD reflectors we use RadSPy radar sounding simulator in Python httpsgithub.comscourvilRadSPy.git an opensource Nlayer radar sounder forwardmodeling software that we have developed and describe herein. We forward model radar data from thin dustrich beds interspersing pure ice and compare them to observed radar reflection data over Gemina Lingula in the north polar layered deposits NPLD. We consider two endmember cases 1 thin beds composed entirely of dust but with thickness varying from 0.05 m to 0.4 m and 2 dust beds all with the same thickness but with varying dust content. We find that the observed reflections can be explained by either scenario i.e. varying thickness or varying dust content and we conclude that a combination of both is likely. More importantly our results provide lower bounds on the layer thickness and dust fraction for the flatlying reflectors of Gemina Lingula in the NPLD. Our findings support the thin dust layer hypothesis providing new constraints on layer composition and geometry for Mars climate researchers.

2021-02-01T00:00:00Z

['Planetary science', '1255']

Lower Bounds on the Thickness and Dust Content of Layers within the North Polar Layered Deposits of Mars from Radar Forward Modeling

https://ui.adsabs.harvard.edu/link_gateway/2021PSJ.....2...28C/EPRINT_PDF

['1255']

['Planetary science']

['Planetary science']

2021RNAAS...5...59M

Evidence is reported for the first time for the presence of the Hg II line in a Narval I profile of Maia the fourth brightest member of the Pleiades open cluster. The Hg II line in Maia absorbs about 2 of the local continuum and can be reproduced with an overabundance of mercury of about 4000 times the solar mercury abundance. This line is probably variable suggesting that mercury might be distributed in spots over the surface of Maia. Maia is currently classified as a Heweak Mn star it should probably be reclassified as a HgMn star.

2021-03-01T00:00:00Z

['Chemically peculiar stars', 'Mercury-manganese stars', '226', '1025']

Detection of the Hg II Line at 3983.93 in One Optical Spectrum of Maia

https://ui.adsabs.harvard.edu/link_gateway/2021RNAAS...5...59M/EPRINT_PDF

['226', '1025']

['Chemically peculiar stars', 'Mercury-manganese stars']

['Chemically peculiar stars', 'Mercury-manganese stars']

2021RNAAS...5...37M

The farUV spectral energy distribution of Dor recorded by IUE is compared to that of the constant and normal star Dra which has similar fundamental parameters. Dor has much less flux than Dra shortwards of 1800 due to the accumulation of very strong absorption lines of Si II in particular autoionization lines around 1400 . Two spectra of Dor separated by 9 hr i.e. much less than the rotational period show evidence of modest variability shortwards of 1800 .

2021-02-01T00:00:00Z

['Bp stars', '178']

The Large Farultraviolet Flux Deficiency of Doradus B8 IIIp Si

https://ui.adsabs.harvard.edu/link_gateway/2021RNAAS...5...37M/EPRINT_PDF

['178']

['Bp stars']

['Bp stars']

2021RNAAS...5...81M

Evidence is presented that the far ultraviolet flux of Maia recorded by the International Ultraviolet Explorer is variable over a timescale of a few hours. In contrast the radial velocity of the Si II doublet near 1530 does not vary on short timescales.

2021-04-01T00:00:00Z

['Chemically peculiar stars', '226']

The Rapid Farultraviolet Variability of Maia Recorded by IUE

https://ui.adsabs.harvard.edu/link_gateway/2021RNAAS...5...81M/EPRINT_PDF

['226']

['Chemically peculiar stars']

['Chemically peculiar stars']

2020ApJ...901..167M

The stability of the pickup ions in the outer heliosheath is a vital factor in the generation of the energetic neutral atom ENA ribbon observed by the Interstellar Boundary EXplorer according to the secondary ENA mechanism. Most previous studies of the pickup ion stability assumed simple idealized velocity distributions of the pickup ions and focused on the parallelpropagating modes only. This paper takes a more realistic multicomponent pickup ion velocity distribution given by the global modeling of neutral atoms in the heliosphere and investigates the role of the oblique mirror waves in addition to the parallel modes. Both linear kinetic instability analysis and hybrid simulations are performed. In contrast to a recent investigation using the same distribution that demonstrated the growth of parallel waves but reported an insignificant contribution of oblique modes our study reveals substantial growth of the oblique mirror instability. The oblique mirror modes and the parallelquasiparallel ion cyclotron waves grow simultaneously with different growth rates. The pickup ion scattering by two types of excited waves together is more pronounced than by either type of wave alone. More importantly our twodimensional hybrid simulation results demonstrate that the development of the mirror instability not only produces its own pickup ion scattering but also leads to the growth of extra ion cyclotron waves in a quasilinear manner which further enhances the pickup ion scattering. The results suggest an important role of the mirror modes that should not be ignored in the stability study of the outer heliosheath pickup ions.

2020-10-01T00:00:00Z

['Heliosphere', 'Heliosheath', 'Heliopause', 'Pickup ions', '711', '710', '707', '1239']

Mirror Instability Driven by Pickup Ions in the Outer Heliosheath

https://ui.adsabs.harvard.edu/link_gateway/2020ApJ...901..167M/EPRINT_PDF

['711', '710', '707', '1239']

['Heliosphere', 'Heliosheath', 'Heliopause', 'Pickup ions']

['Heliosphere', 'Heliosheath', 'Heliopause', 'Pickup ions']

2020ApJ...893...55Z

We carried out a statistical study on the effects of strong geomagnetic activity on the mesopause over the auroral region from 2002 to 2018. When the auroral electrojet index increased significantly the energetic electron precipitation from the Medium Energy Proton and Electron Detector was enhanced by several multiples of 10 for the 5570 geomagnetic latitude band. The temperatures measured by the Sounding of the Atmosphere using Broadband Emission Radiometry instrument increased immediately in the mesopause region together with a descent of the mesopause of about 0.52 km. Due to the depth that the precipitation can affect we conclude that the mesopause is mainly influenced by electrons in the energy range 30100 keV. The maximum temperature increment at 95 km can reach 4 K and the delay of the response can be up to 1 day. In general we find that the temperatures significantly respond to the electron precipitation at as low as 93 km within the mesopause region in most of a year.

2020-04-01T00:00:00Z

['Earth atmosphere', 'Mesopause', 'Mesosphere', 'Aeronomy', '437', '1029', '1030', '22']

Response of the Highlatitude Upper Mesosphere to Energetic Electron Precipitation

https://ui.adsabs.harvard.edu/link_gateway/2020ApJ...893...55Z/EPRINT_PDF

['437', '1029', '1030', '22']

['Earth atmosphere', 'Mesopause', 'Mesosphere', 'Aeronomy']

['Earth atmosphere', 'Mesopause', 'Mesosphere', 'Aeronomy']

2022pds..data...39P

This bundle contains raw radio data that can be used to determine the position and velocity of the MESSENGER spacecraft during flybys of Venus and Mercury and during orbital operations around Mercury. The bundle also contains measurements of occultation times and calibrations for the effects of Earths ionosphere and troposphere meteorological conditions at stations of the NASA Deep Space Network thruster activity and changes in spacecraft antenna selection. The data were used to determine the gravity field and shape of Mercury and to improve solar system ephemerides. The bundle is a migration of data from the original PDS3 archive with minor improvements and corrections.

2022-01-01T00:00:00Z

['14', '15', '24', '25', '26', '34', '35', '43', '45', '54', '55', '63', '65', 'PDS', 'PDS4', 'activity', 'also', 'antenna', 'archive', 'around', 'bundle', 'calibration', 'change', 'condition', 'contains', 'correction', 'data', 'deep', 'determine', 'ds', 'dsn', 'earth', "earth's", 'effect', 'environment', 'ephemeris', 'field', 'flybys', 'geochemistry', 'gravity', 'improve', 'improvement', 'instrumentation', 'ionosphere', 'measurement', 'medium', 'mercury', 'messenger', 'meteorological', 'migration', 'minor', 'mission', 'nasa', 'network', 'occultation', 'operation', 'orbital', 'original', 'pds3', 'position', 'r', 'radio', 'ranging', 'raw', 'science', 'selection', 'shape', 'solar', 'space', 'spacecraft', 'station', 'surface', 'system', 'thruster', 'time', 'troposphere', 'used', 'velocity', 'venus']

MESSENGER RSS Raw Data Bundle

https://ui.adsabs.harvard.edu/link_gateway/2022pds..data...39P/EPRINT_PDF

['14', '15', '24', '25', '26', '34', '35', '43', '45', '54', '55', '63', '65']

['Accretion', 'Achondrites', 'Algol variable stars', 'All-sky cameras', 'Almanacs', 'Amateur astronomers', 'Amateur astronomy', 'Annular eclipses', 'Ansae', 'Apex', 'Aphelion', 'Apsides', 'Argument of perigee']

['Accretion', 'Achondrites', 'Algol variable stars', 'All-sky cameras', 'Almanacs', 'Amateur astronomers', 'Amateur astronomy', 'Annular eclipses', 'Ansae', 'Apex', 'Aphelion', 'Apsides', 'Argument of perigee']

2022pds..data...97G

This collection contains the documents associated with the Galileo Heavy Ion Counter Derived Ion Fluxes October 89 Solar Event Calibrated Bundle.

2022-01-01T00:00:00Z

['89', 'PDS', 'PDS4', 'associated', 'bundle', 'calibrated', 'collection', 'contains', 'counter', 'derived', 'document', 'event', 'flux', 'galileo', 'heavy', 'ion', 'october', 'orbiter', 'solar', 'system']

Galileo HIC Derived Ion Fluxes October 89 Solar Event Document Collection

https://ui.adsabs.harvard.edu/link_gateway/2022pds..data...97G/EPRINT_PDF

['89']

['Astronomical radiation sources']

['Astronomical radiation sources']

2022pds..data..117N

This document collection contains all the standards documentation for the NASA PDS Version 3 Standards including all known versions of the PDS3 Standards Reference SR Data Dictionary DD Data Providers Handbook DPH and Design Document.

2022-01-01T00:00:00Z

['3', 'PDS', 'PDS4', 'collection', 'contains', 'data', 'dd', 'design', 'dictionary', 'document', 'documentation', 'dph', 'handbook', 'including', 'known', 'nasa', 'pds', 'pds3', "provider's", 'reference', 'sr', 'standard', 'version']

PDS3 Standards Collection

https://ui.adsabs.harvard.edu/link_gateway/2022pds..data..117N/EPRINT_PDF

['3']

['A dwarf stars']

['A dwarf stars']

2022pds..data..123N

PDS4 Standards Reference version 1.18.0 2022

2022-01-01T00:00:00Z

['1.18.0', '2022', 'PDS', 'PDS4', 'pds4', 'reference', 'standard', 'version']

PDS4 Planetary Science Standards Reference Version 1.18.0

https://ui.adsabs.harvard.edu/link_gateway/2022pds..data..123N/EPRINT_PDF

['2022']

['Exoplanet surface composition']

['Exoplanet surface composition']

2022pds..data..129G

2020 PDART NEAR MSI updated deblurr algorithm.

2022-01-01T00:00:00Z

['433', 'PDS', 'PDS4', 'asteroid', 'earth', 'eros', 'imager', 'multi-spectral', 'near', 'raw', 'rendezvous', 'science']

NEAR MSI Deblurred Images

https://ui.adsabs.harvard.edu/link_gateway/2022pds..data..129G/EPRINT_PDF

['433']

['Early astronomical instruments']

['Early astronomical instruments']

2022pds..data..128N

PDS4 Concepts version 1.18.0 2022

2022-01-01T00:00:00Z

['1.18.0', '2022', 'PDS', 'PDS4', 'concept', 'pds4', 'version']

PDS4 Planetary Science Concepts Version 1.18.0

https://ui.adsabs.harvard.edu/link_gateway/2022pds..data..128N/EPRINT_PDF

['2022']

['Exoplanet surface composition']

['Exoplanet surface composition']

2022pds..data..127N

PDS4 Concepts version 1.19.0 2022

2022-01-01T00:00:00Z

['1.19.0', '2022', 'PDS', 'PDS4', 'concept', 'pds4', 'version']

PDS4 Planetary Science Concepts Version 1.19.0

https://ui.adsabs.harvard.edu/link_gateway/2022pds..data..127N/EPRINT_PDF

['2022']

['Exoplanet surface composition']

['Exoplanet surface composition']

2022pds..data..126N

PDS4 Data Providers Handbook DPH version 1.18.0 2022

2022-01-01T00:00:00Z

['1.18.0', '2022', 'PDS', 'PDS4', 'data', 'dph', 'handbook', 'pds4', "provider's", 'version']

PDS4 Planetary Science Data Providers Handbook DPH Version 1.18.0

https://ui.adsabs.harvard.edu/link_gateway/2022pds..data..126N/EPRINT_PDF

['2022']

['Exoplanet surface composition']

['Exoplanet surface composition']

2023ApJ...955...14G

Recent spacecraft observations have shown that magnetic reconnection occurs commonly in turbulent environments at shocks. At quasiperpendicular shocks magnetic field lines are bent by the backstreaming reflected ions which form a current sheet in the foot region and then electronscale reconnection occurs when the current sheet is fragmented at the shock front. Here we study magnetic reconnection at a quasiperpendicular shock by using a twodimensional particleincell simulation. Collective properties of the reconnection sites from the shock transition to the downstream region are analyzed by adopting a statistical approach to the simulation data. Reconnecting current sheets are found to be densely distributed near the shock front with a reconnection electric field larger than those in the downstream region. By tracing a reconnection site from its formation until it is convected downstream we show the reconnection proceeds intermittently after an active stage near the shock front. Our tracing further shows that in addition to being originated from the shock front reconnection in the downstream region can also occur locally driven by turbulent flows therein. The results help us better understand the evolution of electronscale reconnection at a perpendicular shock.

2023-09-01T00:00:00Z

['Space plasmas', 'Plasma physics', 'Solar magnetic reconnection', 'Planetary bow shocks', '1544', '2089', '1504', '1246']

Properties of Electronscale Magnetic Reconnection at a Quasiperpendicular Shock

https://ui.adsabs.harvard.edu/link_gateway/2023ApJ...955...14G/EPRINT_PDF

['1544', '2089', '1504', '1246']

['Space plasmas', 'Plasma physics', 'Solar magnetic reconnection', 'Planetary bow shocks']

['Space plasmas', 'Plasma physics', 'Solar magnetic reconnection', 'Planetary bow shocks']

2021PSJ.....2..180N

While it has long been known that Titans haze and atmosphere are dynamic on seasonal timescales recent results have revealed that they also exhibit significant subseasonal variations. Here we report on observations of Titan acquired over an eightmonth period between 2014 April and 2015 March with the Spectrograph for Integral Field Observations in the Near Infrared instrument on the Very Large Telescope using adaptive optics. These observations have an average fiveday cadence permitting interrogation of the shortperiod variability of Titans atmosphere. Diskresolved spectra in the H and K bands 1.42.4 m were analyzed with the PyDISORT radiative transfer model to determine the spatial distribution and variation of stratospheric haze opacity over subseasonal timescales. We observed a uniform decrease in haze opacity at 20N and an increase in haze opacity at 250300E and 40N over the span of our observations. Globally we found variations on the order of 510 on timescales of weeks as well as a steady global increase in the amount of haze over timescales of months. The observed variations in haze opacity over the short timescales of our observations were of similar magnitude to longperiod variations attributed to seasonal variation suggesting rapid dynamical processes that may take part in the distribution of hazes in Titans atmosphere.

2021-10-01T00:00:00Z

['Ground-based astronomy', 'Atmospheric variability', 'Saturnian satellites', '686', '2119', '1427']

Tracking Shortterm Variations in the Haze Distribution of Titans Atmosphere with SINFONI VLT

https://ui.adsabs.harvard.edu/link_gateway/2021PSJ.....2..180N/EPRINT_PDF

['686', '2119', '1427']

['Ground-based astronomy', 'Atmospheric variability', 'Saturnian satellites']

['Ground-based astronomy', 'Atmospheric variability', 'Saturnian satellites']

2024ApJ...963...64Y

Space plasmas are turbulent and maintain different types of critical points or flow nulls. Electron vortex as one type of flow null structure is crucial in the energy cascade in turbulent plasmas. However due to the limited time resolution of the spacecraft observations one can never analyze the threedimensional properties of the electron vortex. In the present study with the advancement of the FOTEV method and the unprecedented highresolution measurements from four Magnetospheric Multiscale spacecraft we successfully identify the electron vortex and then reconstruct its threedimensional topology of the surrounding electron flow field. The results of the reconstruction show that the configuration of the electron vortex is elliptical. Comparison between the observation and reconstruction scales of the vortex indicates the reliable reconstruction of the flow velocity. Our study sheds light on the understanding of the topology and property of the electron vortex and its relationship with kineticscale magnetic holes.

2024-03-01T00:00:00Z

['Plasma physics', 'Space plasmas', 'Plasma astrophysics', '2089', '1544', '1261']

Reconstruction of Electron Vortex in Space Plasmas

https://ui.adsabs.harvard.edu/link_gateway/2024ApJ...963...64Y/EPRINT_PDF

['2089', '1544', '1261']

['Plasma physics', 'Space plasmas', 'Plasma astrophysics']

['Plasma physics', 'Space plasmas', 'Plasma astrophysics']

2024PSJ.....5...27P

We analyze the polarization observations of the DidymosDimorphos system before and after the impact by the NASA Double Asteroid Redirection Test spacecraft on Dimorphos. We fit empirical polarization phase curve models and statistically confirm the discovery by Gray et al. about the degree of linear polarization of the system decreasing on the impact and remaining altered for at least 30 days postimpact. With numerical simulations of particles in the geometric optics domain we estimate the dominant size of the particles either in the regolith of Didymos and Dimorphos or in the impactdriven ejecta cloud to be several hundred micrometers. The observed change between the preimpact and postimpact systems indicates either a decrease in average particle size of some tens of micrometers or a decreased level of space weathering.

2024-01-01T00:00:00Z

['Asteroid surfaces', 'Near-Earth objects', 'Polarimetry', '2209', '1092', '1278']

Modeling Linear Polarization of the DidymosDimorphos System before and after the DART Impact

https://ui.adsabs.harvard.edu/link_gateway/2024PSJ.....5...27P/EPRINT_PDF

['2209', '1092', '1278']

['Asteroid surfaces', 'Near-Earth objects', 'Polarimetry']

['Asteroid surfaces', 'Near-Earth objects', 'Polarimetry']

2022pds..data...55H

An Examination of Soil Crusts on the Floor of Jezero crater Mars

2022-01-01T00:00:00Z

['2020', 'PDS', 'PDS4', 'crater', 'crust', 'derived', 'examination', 'floor', 'jezero', 'mars', 'pixl', 'science', 'soil', 'spectrometer']

An Examination of Soil Crusts on the Floor of Jezero crater Mars

https://ui.adsabs.harvard.edu/link_gateway/2022pds..data...55H/EPRINT_PDF

['2020']

['Exoplanet atmospheric variability']

['Exoplanet atmospheric variability']

2022pds..data...50K

This bundle contains the Voyager 2 Plasma Wave Spectrometer spectrum analyzer data from the entire mission in calibrated CDF files

2022-01-01T00:00:00Z

['2', 'PDS', 'PDS4', 'analyzer', 'bundle', 'calibrated', 'cdf', 'contains', 'data', 'entire', 'file', 'jupiter', 'mission', 'neptune', 'plasma', 'saturn', 'science', 'solar', 'spectrometer', 'spectrum', 'system', 'uranus', 'voyager', 'wave']

Voyager 2 PWS Low Rate Spectrum Analyzer Data Bundle

https://ui.adsabs.harvard.edu/link_gateway/2022pds..data...50K/EPRINT_PDF

['2']

['53 Persei stars']

['53 Persei stars']

2022pds..data...51K

This bundle contains Voyager 1 Plasma Wave Spectrometer PWS raw waveform data and documentation for all available telemetry frames from SCET 19780821T054136.299Z through 20220205T081807.031Z.

2022-01-01T00:00:00Z

['1', '1978-08-21t05:41:36.299z', '2022-02-05t08:18:07.031z', 'PDS', 'PDS4', 'available', 'bundle', 'contains', 'data', 'documentation', 'frame', 'interstellar', 'jupiter', 'medium', 'partially', 'particle', 'plasma', 'processed', 'pws', 'raw', 'saturn', 'scet', 'science', 'solar', 'spectrometer', 'telemetry', 'voyager', 'wave', 'waveform', 'wind']

Voyager 1 Plasma Wave Science Uncalibrated Waveforms Entire Mission Bundle

https://ui.adsabs.harvard.edu/link_gateway/2022pds..data...51K/EPRINT_PDF

['1']

['Unknown']

['Unknown']

2022pds..data...47S

Data from the Ultraviolet Spectrometer instruments on the Mariner 6 and Mariner 7 spacecrafts.

2022-01-01T00:00:00Z

['6', '69', '7', 'PDS', 'PDS4', 'data', 'instrument', 'mariner', 'mars', 'spacecraft', 'spectrometer', 'ultraviolet']

Mariner 6 and 7 Ultraviolet Spectrometer Bundle

https://ui.adsabs.harvard.edu/link_gateway/2022pds..data...47S/EPRINT_PDF

['6', '69', '7']

['A subdwarf stars', 'Ascending node', 'A subgiant stars']

['A subdwarf stars', 'Ascending node', 'A subgiant stars']

2022pds..data...43K

These are reprocessed measurements by the Engergetic Particle Detector EPD instrument onboard the Galileo spacecraft that orbited Jupiter and measured intensities of ion and electron radiation in the keV and MeV energy range. This set is version 31 of reprocessing and version 1.0 of PDS delivery. The TOFxE and DeltaExE files include event data of ion measurements. Event data are different than the channelized data in the high medium and low resolution files. Event data record the full information of a measured particle. Every event is the measurement of a time of flight TOF within the instrument and energy deposited within a detector TOFxE file or two energy values deposited within the two detector layers DeltaExE file. The deposited energy values are generally different from the energy the particle has in the ambient space. Event data provides measured values in the native resolution of the instrument. Because such high resolution increases data volume event data cannot be taken continuously and downlinked all the time. Only the provided subset of this data was kept. The files are comma separated. Invalid entries will have values of 1.000000E38. Times are provided in the format Year.DOYHHMMSSM first column and fractional year second column More information can be found in the User Guide. This file includes measurements by the EPDCMSTOFxE instrument. For each counted event the energy deposited in the one solid state detector EnergykeV column and the time of flight TOFns within the instrument are recorded.

2022-01-01T00:00:00Z

['1.0', '1.000000e+38', '31', 'PDS', 'PDS4', 'ambient', 'cannot', 'channelized', 'column', 'comma', 'continuously', 'counted', 'data', 'delivery', 'deltaexe', 'deposited', 'detector', 'different', 'downlinked', 'electron', 'energetic', 'energy', 'energy_kev', 'engergetic', 'entry', 'epd', 'epd/cms/tofxe', 'event', 'every', 'file', 'first', 'flight', 'format', 'found', 'fractional', 'full', 'galileo', 'generally', 'guide', 'high', 'include', 'includes', 'increase', 'information', 'instrument', 'intensity', 'invalid', 'ion', 'jupiter', 'kept', 'kev', 'layer', 'low', 'measured', 'measurement', 'medium', 'mev', 'native', 'onboard', 'one', 'orbited', 'orbiter', 'particle', 'pds', 'provided', 'provides', 'radiation', 'range', 'record', 'recorded', 'reprocessed', 'reprocessing', 'resolution', 'second', 'separated', 'set', 'solid', 'space', 'spacecraft', 'state', 'subset', 'taken', 'time', 'tof', 'tof_ns', 'tofxe', 'two', 'user', 'value', 'version', 'volume', 'within', 'year', 'year.doyhhmmssm']

Galileo EPD Calibrated Corrected TimeofFlight Event Data Collection

https://ui.adsabs.harvard.edu/link_gateway/2022pds..data...43K/EPRINT_PDF

['31']

['AM Canum Venaticorum stars']

['AM Canum Venaticorum stars']

2022pds..data...15N

This collection contains Voyager 2 Jupiter encounter magnetometer data given in Heliographic coordinates and averaged from the 60 ms instrument sample rate to a 1.92 second resampled rate. All magnetic field observations are measured in nanoTesla. All of the magnetic field data are calibrated.

2022-01-01T00:00:00Z

['1.92', '2', '60', 'PDS', 'PDS4', 'averaged', 'calibrated', 'collection', 'contains', 'coordinate', 'data', 'encounter', 'field', 'fluxgate', 'ganymede', 'given', 'heliographic', 'instrument', 'jupiter', 'm', 'magnetic', 'magnetometer', 'measured', 'nanotesla', 'observation', 'rate', 'resampled', 'sample', 'second', 'triaxial', 'voyager']

Voyager 2 Magnetometer Jupiter Resampled Heliographic RTN Coords 1.92 Second Data Collection

https://ui.adsabs.harvard.edu/link_gateway/2022pds..data...15N/EPRINT_PDF

['2', '60']

['53 Persei stars', 'Apparent position']

['53 Persei stars', 'Apparent position']

2022pds..data...11R

This bundle contains Venus Express cleaned highresolution 128 Hz magnetic field data acquired by the fluxgate magnetometer gradiometer onboard the Venus Express spacecraft. The data are expressed in Venus Solar Orbital VSO coordinates and RadialEastNorth coordinates. This work was funded by a 2017 NASA ROSES SSW proposal. Grant number NNH17ZDA001NSSW.

2022-01-01T00:00:00Z

['128', '2017', 'PDS', 'PDS4', 'acquired', 'bundle', 'cleaned', 'contains', 'coordinate', 'data', 'express', 'expressed', 'field', 'fluxgate', 'funded', 'gradiometer', 'grant', 'high-resolution', 'hz', 'magnetic', 'magnetometer', 'nasa', 'nnh17zda001n-ssw', 'number', 'onboard', 'orbital', 'proposal', 'radial-east-north', 'rose', 'solar', 'spacecraft', 'ssw', 'venus', 'vso', 'work']

Venus Express Cleaned HighResolution 128 Hz Magnetic Field Data Bundle

https://ui.adsabs.harvard.edu/link_gateway/2022pds..data...11R/EPRINT_PDF

['128', '2017']

['B stars', 'AGN host galaxies']

['B stars', 'AGN host galaxies']

2022pds..data...16N

This collection contains Voyager 2 Jupiter encounter magnetometer data given in Heliographic coordinates and averaged from the 60 ms instrument sample rate to a 9.6 second resampled rate. All magnetic field observations are measured in nanoTesla. All of the magnetic field data are calibrated.

2022-01-01T00:00:00Z

['2', '60', '9.6', 'PDS', 'PDS4', 'averaged', 'calibrated', 'collection', 'contains', 'coordinate', 'data', 'encounter', 'field', 'fluxgate', 'ganymede', 'given', 'heliographic', 'instrument', 'jupiter', 'm', 'magnetic', 'magnetometer', 'measured', 'nanotesla', 'observation', 'rate', 'resampled', 'sample', 'second', 'triaxial', 'voyager']

Voyager 2 Magnetometer Jupiter Resampled Heliographic RTN Coords 9.60 Second Data Collection

https://ui.adsabs.harvard.edu/link_gateway/2022pds..data...16N/EPRINT_PDF

['2', '60']

['53 Persei stars', 'Apparent position']

['53 Persei stars', 'Apparent position']

2022pds..data...31L

This bundle contains the results from the simulation study presented in Lapenta G. Schriver D. Walker R. J. Berchem J. Echterling N. F. El Alaoui M. Travnicek P. Do we need to consider electrons kinetic effects to properly model a planetary magnetosphere the case of Mercury JGR 2022. httpsdoi.org The data includes fully kinetic global PIC simulations of Mercurys magnetosphere that include both ion and electron kinetic effects along with MESSENGER data. The energy conserving version of the ipic3D simulation code ECSIM Lapenta 2017 doi10.1016j.jcp.2017.01.002 was used to study the evolution of Mercurys magnetosphere. This work was funded by NASA grants HSR 80NSSC19K0841 and HSR 80NSSC19K0846 and NASA SSW 80NSSC19K0789 and 80NSSC21K0053. Resources supporting this work were provided by the NASA HighEnd Computing HEC program through the NASA Advanced Supercomputing NAS Division at Ames Research Center and NCCS at NASA Goddard Space Flight Center.

2022-01-01T00:00:00Z

['2017', '2022', '80nssc19k0789', '80nssc19k0841', '80nssc19k0846', '80nssc21k0053', 'PDS', 'PDS4', 'advanced', 'alaoui', 'along', 'ames', 'berchem', 'bundle', 'case', 'center', 'code', 'computer', 'computing', 'conserving', 'consider', 'contains', 'data', 'derived', 'division', 'doi:10.1016/j.jcp.2017.01.002', 'echterling', 'ecsim', 'effect', 'el', 'electron', 'energy', 'evolution', 'f', 'flight', 'fully', 'funded', 'g', 'global', 'goddard', 'grant', 'hec', 'high-end', 'hsr', 'https://doi.org', 'include', 'includes', 'ion', 'ipic3d', 'j', 'jgr', 'kinetic', 'lapenta', 'magnetosphere', 'mercury', "mercury's", 'messenger', 'model', 'n', 'na', 'nasa', 'nccs', 'need', 'p', 'pic', 'planetary', 'presented', 'program', 'properly', 'provided', 'r', 'research', 'resource', 'result', 'schriver', 'science', 'simulation', 'space', 'ssw', 'study', 'supercomputing', 'supporting', 'travnicek', 'used', 'version', 'walker', 'work']

Do we need to consider electrons kinetic effects to properly model a planetary magnetosphere the case of Mercury simulation data bundle

https://ui.adsabs.harvard.edu/link_gateway/2022pds..data...31L/EPRINT_PDF

['2017', '2022']

['AGN host galaxies', 'Exoplanet surface composition']

['AGN host galaxies', 'Exoplanet surface composition']

2023ApJ...953....8S

The expandingbox model of the solar wind has been adopted in the literature within the context of magnetohydrodynamics hybrid and full particleincell simulations to investigate the dynamic evolution of the solar wind. The present paper extends such a method to the framework of selfconsistent quasilinear kinetic theory. It is shown that the expandingbox quasilinear methodology is largely equivalent to the inhomogeneous steadystate quasilinear model discussed earlier in the literature but a distinction regarding the description of wave dynamics between the two approaches is also found. The expandingbox quasilinear formalism is further extended to include the effects of a spiraling solarwind magnetic field as well as collisional age effects. The present finding shows that the expandingbox quasilinear approach and the steadystate globalkinetic models may be employed interchangeably in order to address other more complex problems associated with the solarwind dynamics.

2023-08-01T00:00:00Z

['Solar wind', '1534']

Expandingbox Quasilinear Model of the Solar Wind

https://ui.adsabs.harvard.edu/link_gateway/2023ApJ...953....8S/EPRINT_PDF

['1534']

['Solar wind']

['Solar wind']

2022ApJS..261...18G

The Interstellar Boundary Explorer IBEX is a NASA satellite in Earth orbit dedicated to observing both interstellar neutral atoms entering the heliosphere and energetic neutral atoms ENAs from the interstellar boundaries from roughly 10 eV to 6 keV. This work presents the averaged maps energy spectra and temporal variability of heliospheric ENA intensities measured with the IBEXLo instrument at 1 au at energies between 10 eV and 2 keV covering one entire solar cycle from 2009 through 2019. These results expand the range in time and energy for studying the globally distributed ENA flux and the IBEX Ribbon. The observed ENA intensities exceed model predictions in particular below 500 eV. Moreover the ENA intensities between 50200 eV energy show an unexpected rise and fall around the year 2015 in most sky regions.

2022-08-01T00:00:00Z

['Heliosphere', 'Heliosheath', '711', '710']

One Solar Cycle of Heliosphere Observations with the Interstellar Boundary Explorer Energetic Neutral Hydrogen Atoms Observed with IBEXLo from 10 eV to 2 keV

https://ui.adsabs.harvard.edu/link_gateway/2022ApJS..261...18G/EPRINT_PDF

['711', '710']

['Heliosphere', 'Heliosheath']

['Heliosphere', 'Heliosheath']

2022pds..data..115S

This version of the Ultraviolet Spectrometer UVS for GO bundle was created by the PDS Atmospheres node in 2022

2022-01-01T00:00:00Z

['2022', 'PDS', 'PDS4', 'atmosphere', 'bundle', 'callisto', 'created', 'europa', 'galileo', 'ganymede', 'go', 'io', 'jupiter', 'node', 'orbiter', 'pds', 'plasma', 'spectrometer', 'star', 'torus', 'ultraviolet', 'uv', 'version']

Galileo Orbiter Ultraviolet Spectrometer UVS for GO Bundle

https://ui.adsabs.harvard.edu/link_gateway/2022pds..data..115S/EPRINT_PDF

['2022']

['Exoplanet surface composition']

['Exoplanet surface composition']

2024RNAAS...8...97B

This paper employs machine learning to estimate stellar temperatures using photometric data focusing on the GAIA ESA Archive Data Release 3 data set. The study underscores the effectiveness of neural networks in deciphering intricate relationships within the data. Notably the addition of metallicity improves model accuracy in characterizing stellar properties. The study also investigates outlier removal techniques specifically favoring the Isolation Forest method showcasing its efficacy in refining model performance. Automated machine learning facilitated by PyCaret Regressor emerges as a valuable tool identifying topperforming models and highlighting feature importance. The implications of this research extend beyond the specifics of stellar temperature estimation. In contemplating future directions this study suggests the exploration of diverse data sources to ensure balanced distributions of stellar temperatures and the potential incorporation of deep learning architectures for heightened accuracy in addressing astrophysical inquiries.

2024-04-01T00:00:00Z

['Photometric systems', 'Photometry', 'Stellar effective temperatures', 'Neural networks', 'Outlier detection', '1233', '1234', '1597', '1933', '1934']

Enhancing Stellar Temperature Estimation through Machine Learning and Multifaceted Data Exploration

https://ui.adsabs.harvard.edu/link_gateway/2024RNAAS...8...97B/EPRINT_PDF

['1233', '1234', '1597', '1933', '1934']

['Photometric systems', 'Photometry', 'Stellar effective temperatures', 'Neural networks', 'Outlier detection']

['Photometric systems', 'Photometry', 'Stellar effective temperatures', 'Neural networks', 'Outlier detection']

2020AJ....160...48C

The subject of the present paper is the analysis of the orbital solutions for eight binaries WDS 024020436 HDS 347 WDS 025525950 MLR 520 WDS 031196131 HDS 407 WDS 045707350 YSC 145 WDS 052024105 HDS 701 WDS 064670822 HDS 940AB WDS 082591623 HDS 1199 and WDS 225505132 HU 785. Seven orbits are determined for the first time and the remaining orbit is a revision. The five binaries are HDS discovered during the Hipparcos mission two binaries were discovered before 1902 and 1974 and one binary was discovered afterwards 2009. All measured separations are less than 1 arcsecond and in most studied pairs they are less than 0.4 arcseconds. The number of measurements is relatively small from 9 to 16 except for one pair which has only been measured six times so far. The median orbital period is 95.1 yr the shortest period is 12.5 yr and the longest period is 362.7 yr. In addition to the orbital elements we also give absolute magnitudes spectral types estimates of the masses dynamical parallaxes and OC residuals in and .

2020-07-01T00:00:00Z

['Fundamental parameters of stars', 'Visual binary stars', '555', '1777']

Orbits for Eight Binaries

https://ui.adsabs.harvard.edu/link_gateway/2020AJ....160...48C/EPRINT_PDF

['555', '1777']

['Fundamental parameters of stars', 'Visual binary stars']

['Fundamental parameters of stars', 'Visual binary stars']

2020ApJ...895....8C

The deexcitation ray lines in solar flares result from energetic ions e.g. protons particles interacting with the ambient nuclei in the solar atmosphere. The centroid and width of lines contain a wealth of information on the directionality composition and spectra of energetic ions as well as properties of the interaction sites. New calculations for the deexcitation ray line shape analysis were done to study the properties of these ions. We calculate the shapes of the most intense deexcitation ray lines in the solar flares including the SUP12SUPC 4.439 MeV SUP16SUPO 6.129 MeV SUP24SUPMg 1.369 MeV and SUP28SUPSi 1.779 MeV lines and explore the profiles of these line shapes as a function of the accelerated ions energy spectra and composition as well as the heliocentric angle of flare location. The merits of deexcitation ray line shape analysis include 1 only a relatively small number of parameters being required in the fitting process and 2 the characteristics of accelerated ions with joint multiline shape analysis being well constrained. We conclude that the measurement of the width and centroid of lines is an effective method for determining the properties of flareaccelerated ions.

2020-05-01T00:00:00Z

['The Sun', 'Solar flares', 'Solar gamma-ray emission', 'Solar energetic particles', '1693', '1496', '1497', '1491']

A Spectroscopic Method Based on the Shapes of Nuclear Deexcitation Ray Lines in Solar Flares

https://ui.adsabs.harvard.edu/link_gateway/2020ApJ...895....8C/EPRINT_PDF

['1693', '1496', '1497', '1491']

['The Sun', 'Solar flares', 'Solar gamma-ray emission', 'Solar energetic particles']

['The Sun', 'Solar flares', 'Solar gamma-ray emission', 'Solar energetic particles']

2019ApJ...882L..17M

Lunar indigenous Xe isotopic abundances provide crucial information on relationships not only between gas reservoirs in the solar protoplanetary disk but also regarding planetary fractionation processes and possible space weather effects due to an active young Sun. The indigenous lunar Xe isotopic composition is not yet firmly established. A verification of previously inferred lunar Xe signatures using rocks of varying compositions from Apollo 16 and 17 missions is made here. Ancient lunar highland rocks carry cosmicrayproduced spallation and neutroncapture products fission components due to SUP244SUPPu and SUP238SUPU as well as terrestrial contamination gas all complicating the identification of the indigenous lunar Xe component. The present study reveals light and heavy isotopic abundances compatible with terrestrial Xe composition. We conclude that in order to firmly establish indigenous lunar Xe signatures in situ Xe measurements on the moon in interior samples of anorthositic ejecta from very recent craters should be performed.

2019-09-01T00:00:00Z

['Lunar origin', 'Solar abundances', 'Planetary atmospheres', 'Isotopic abundances', '966', '1474', '1244', '867']

Lunar Xenon and the Origin of the Indigenous Component

https://ui.adsabs.harvard.edu/link_gateway/2019ApJ...882L..17M/EPRINT_PDF

['966', '1474', '1244', '867']

['Lunar origin', 'Solar abundances', 'Planetary atmospheres', 'Isotopic abundances']

['Lunar origin', 'Solar abundances', 'Planetary atmospheres', 'Isotopic abundances']

2021RNAAS...5...54M

The abundances of several elements in the atmosphere of the HgMn star 14 Sge HR 7664 are derived from the analysis of highresolution spectra obtained recently with the spectropolarimeter NeoNarval. A large phosphorus overabundance about 60 times the solar abundance is found. This study is the beginning of a systematic survey of all northern HgMn stars aiming at deriving their abundances in a consistent manner.

2021-03-01T00:00:00Z

['Chemically peculiar stars', '226']

The Abundance of Phosphorus in the HgMn Star 14 Sge

https://ui.adsabs.harvard.edu/link_gateway/2021RNAAS...5...54M/EPRINT_PDF

['226']

['Chemically peculiar stars']

['Chemically peculiar stars']

2022RNAAS...6..267M

The analysis of two spectra of the Mn Hg star HD 29589 recorded by the SWP camera on board the International Ultraviolet Explorer does not reveal variations of the farultraviolet flux over a thirteen years time interval. The TESS lightcurve of HD 29589 shows a complex pattern of oscillations with variable amplitudes and probably several periods. A very strong resonance line of Ga II is present at 1414.40 and confirms the Hg Mn status of HD 29589. A P Cygni profile at 1793.20 on SWP04948 could correspond to the resonance line of Sr II at 1793.09 and indicate transient mass loss.

2022-12-01T00:00:00Z

['Chemically peculiar stars', 'Mercury-manganese stars', '226', '1025']

The Behavior of HgMn Stars in the Far UVPaper 21 HD 29589

https://ui.adsabs.harvard.edu/link_gateway/2022RNAAS...6..267M/EPRINT_PDF

['226', '1025']

['Chemically peculiar stars', 'Mercury-manganese stars']

['Chemically peculiar stars', 'Mercury-manganese stars']

2022RNAAS...6..238M

The analysis of the coadded high resolution SWP spectrum of the Hg star HD 209459 recorded by the International Ultraviolet Explorer reveals the presence of two resonance lines of Hg II at 1649.92 and 1942.28 . The line synthesis of the least blended resonance line at 1942.28 yields a mercury abundance of about 1000 times the solar mercury abundance. The abundances of other element are found to agree fairly well with previous determinations. These results suggest that HD 209459 might be a mild HgMn star. However more abundance determinations from high resolution high signaltonoise optical spectra are necessary to clarify the status of this interesting object.

2022-11-01T00:00:00Z

['Chemically peculiar stars', 'Mercury-manganese stars', '226', '1025']

The Mercury Lines in the Mean Far Ultraviolet Spectrum of HD 209459

https://ui.adsabs.harvard.edu/link_gateway/2022RNAAS...6..238M/EPRINT_PDF

['226', '1025']

['Chemically peculiar stars', 'Mercury-manganese stars']

['Chemically peculiar stars', 'Mercury-manganese stars']

2020ApJ...901...20L

Recently an electronscale coherent structure known as a magnetic hole MH was observed in the Earths magnetosheath. It has been found that the MH is characterized by decreasing magnetic field strength and increasing parameters such as electron density temperature and temperature anisotropy. Observations suggest that electron temperature anisotropy within an MH structure provides free energy to generate whistler waves. In this study a smallscale MH formed in the downstream region of the magnetic reconnection indicating that the region far away from the Xline may be another important electron heating channel. A strong energydissipating current layer is observed near the boundary within MH implying that boundary may be the energy source for MH heating electrons. These characteristics indicate that the observed MH is still highly dynamic and has multiscale coupling processes.

2020-09-01T00:00:00Z

['Magnetic fields', 'Space plasmas', 'Plasma jets', '994', '1544', '1263']

In Situ Evidence of a Magnetic Hole Downstream of the Magnetic Reconnection in the Magnetopause Reconnection

https://ui.adsabs.harvard.edu/link_gateway/2020ApJ...901...20L/EPRINT_PDF

['994', '1544', '1263']

['Magnetic fields', 'Space plasmas', 'Plasma jets']

['Magnetic fields', 'Space plasmas', 'Plasma jets']

2023RNAAS...7...11M

The analysis of five spectra of the Hg Mn spectroscopic binary star HD 77350 recorded by the SWP camera on board the International Ultraviolet Explorer reveals one instance of variation of the farultraviolet flux of this star shortwards of 1800 . The analysis of the coadded SWP spectrum built from the high resolution SWP spectra obtained through the small aperture shows the importance of low excitation and resonance Si II lines shortwards of 1540 of the Ga II and Ga III resonance lines at 1414 and 1495 and of the Al II resonance line at 1670 . A very rough estimate of a period from the currently available Transiting Exoplanet Survey Satellite lightcurves yields a value of 9.63 0.18 days which could be the rotation period but this needs confirmation.

2023-01-01T00:00:00Z

['Chemically peculiar stars', 'Mercury-manganese stars', '226', '1025']

The Behavior of HgMn Stars in the Far UVPaper 25 HD 77350

https://ui.adsabs.harvard.edu/link_gateway/2023RNAAS...7...11M/EPRINT_PDF

['226', '1025']

['Chemically peculiar stars', 'Mercury-manganese stars']

['Chemically peculiar stars', 'Mercury-manganese stars']

2023RNAAS...7...49M

The analysis of seventeen spectra of the Bp Heweak star HD 125823 recorded by the SWP camera on board the International Ultraviolet Explorer reveals no variations of the farultraviolet spectral energy distribution of this star over a time interval of three years. However line variations are present in the range 1400 up to 1600 which can be partly attributed to variations of lines of Si II and Si III. This confirms that silicon is not distributed in a uniform manner over the surface but the horizontal gradients of the silicon abundance are probably not large.

2023-03-01T00:00:00Z

['Chemically peculiar stars', 'Helium-weak stars', '226', '717']

The Behavior of Bp Heweak Stars in the Far UVPaper 2 HD 125823

https://ui.adsabs.harvard.edu/link_gateway/2023RNAAS...7...49M/EPRINT_PDF

['226', '717']

['Chemically peculiar stars', 'Helium-weak stars']

['Chemically peculiar stars', 'Helium-weak stars']

2020ApJ...888L..16C

Both magnetic reconnection and turbulence can play crucial roles in space plasmas. The current layers developing during magnetic reconnection can collapse into various smallscale coherent structures such as current filaments. These current filaments can significantly modulate the kineticscale turbulence. However the quantitative correlation between the current filaments and turbulence remains unknown so far. In this study we statistically analyze such a relation during a turbulent reconnection in the magnetotail. We find that the kineticscale turbulence has a good correlation with the currentdensity variation ftJSUPprimeSUP fttfracdJdtrightright. Specifically 1 the slope of the kineticscale power spectral density PSD denoted as S SUBPSDSUB decreases with J exhibiting an empirical relation S SUBPSDSUB 0.54lnJ 1.36 2 the correlation between turbulence intensity PSD and J is best at the frequency range 0.020.32 SUBceSUB electron cyclotron frequency 3 the turbulence intensity PSD increases with J exhibiting an empirical relation PSD JSUP k SUP e SUP b SUP and 4 the k of these fitting functions roughly decreases with frequency. These results can advance our understanding of the interplay between magnetic reconnection and turbulence.

2020-01-01T00:00:00Z

['Interplanetary turbulence', 'Space plasmas', 'Plasma jets', '830', '1544', '1263']

Relationship between Current Filaments and Turbulence During a Turbulent Reconnection

https://ui.adsabs.harvard.edu/link_gateway/2020ApJ...888L..16C/EPRINT_PDF

['830', '1544', '1263']

['Interplanetary turbulence', 'Space plasmas', 'Plasma jets']

['Interplanetary turbulence', 'Space plasmas', 'Plasma jets']

2020ApJ...888...25M

The first laboratory evidence of a radiative shock RS decelerating during its free expansion phase in an optically thick medium is presented. A shock is generated in a multilayer solid target under the irradiation of a highpower laser at the GEKKO XII laser facility. The rear surface of the target is connected to a gas cell filled with Xe. Upon breakout an RS characterized by low Boltzmann number Bo 1 and Mihalas number R 10 is generated. Experimental results reveal that radiative losses through the radiative precursor cause the shock to lose energy and decelerate. A model is developed that describes the shock propagation as a function of time. The model is in agreement with both numerical simulations and experimental results. These results have tremendous consequences for astrophysical systems such as SN 1987A where radiative deceleration may play a role in the formation of the observed hotspots in the circumstellar ring.

2020-01-01T00:00:00Z

['Laboratory astrophysics', 'Experimental techniques', 'Shocks', '2004', '2078', '2086']

Laboratory Observation of Radiative Shock Deceleration and Application to SN 1987A

https://ui.adsabs.harvard.edu/link_gateway/2020ApJ...888...25M/EPRINT_PDF

['2004', '2078', '2086']

['Laboratory astrophysics', 'Experimental techniques', 'Shocks']

['Laboratory astrophysics', 'Experimental techniques', 'Shocks']

2020ApJ...897...75G

A newly calculated ab initio potential energy surface is used to compute collisiondriven statechanging cross sections and rate coefficients over a range from 5 to 100 K for CNSUPSUPSUP1SUP the smallest anion detected in the interstellar medium interacting with He an abundant species in this environment. We compare our presently computed rate coefficients with those previously published for the similar and important systems CNHe CNHSUB2SUB and CNSUPSUPHSUB2SUB to illustrate the broader network of inelastic statechanging processes for these four systems. We also discuss the sizescaling effects that occur when changing partners from He to HSUB2SUB. We further analyze the differences in size between collisiondriven rate coefficients when going from neutral CN to its anion. All the present results are discussed in detail to provide accurate and realistic data for chemical networks that wish to include the CNSUPSUP anion in their modeling of astrochemical environments.

2020-07-01T00:00:00Z

['Diffuse molecular clouds', 'Molecular clouds', 'Molecular physics', 'Collision processes', 'Radiative processes', 'De-excitation rates', 'Excitation rates', '2058', '2065', '1072', '2055', '381', '2066', '2067']

Rotationally Inelastic Collisions of CNSUPSUP with He Computing Cross Sections and Rates in the Interstellar Medium

https://ui.adsabs.harvard.edu/link_gateway/2020ApJ...897...75G/EPRINT_PDF

['2058', '2065', '1072', '2055', '381', '2066', '2067']

['Molecular physics', 'Collision physics', 'Molecular clouds', 'Radiative processes', 'Diffuse molecular clouds', 'De-excitation rates', 'Excitation rates']

['Molecular physics', 'Collision physics', 'Molecular clouds', 'Radiative processes', 'Diffuse molecular clouds', 'De-excitation rates', 'Excitation rates']

2020ApJ...896..103B

The migrations of solid objects throughout the solar system are thought to have played key roles in disk evolution and planet formation. However our understanding of these migrations is limited by a lack of quantitative constraints on their timings and distances recovered from laboratory measurements of meteorites. The protoplanetary disk supported a magnetic field that decreased in intensity with heliocentric distance. As such the formation distances of the parent asteroids of ancient meteorites can potentially be constrained by paleointensity measurements of these samples. Here we find that the WIS 91600 ungrouped C2 chondrite experienced an ancient field intensity of 4.4 2.8 T. Combined with the thermal history of this meteorite magnetohydrodynamical models suggest the disk field reached 4.4 T at 9.8 au indicating that the WIS 91600 parent body formed in the distal solar system. Because WIS 91600 likely came to Earth from the asteroid belt our recovered formation distance argues that this body previously traveled from 10 au to 23 au supporting the migration of asteroidsized bodies throughout the solar system. WIS 91600 also contains chondrules calciumaluminumrich inclusions and amoeboid olivine aggregates indicating that some primitive millimetersized solids that formed in the innermost solar system migrated outward to 10 au within 34 Myr of solar system formation. Moreover the oxygen isotopic compositions of proposed distal meteorites WIS 91600 Tagish Lake and CI chondrites argue that the CM CO and CR chondrites contain micrometerscale dust and ice that originated in the distal solar system.

2020-06-01T00:00:00Z

['Meteorites', 'Magnetic fields', 'Primordial magnetic fields', 'Asteroid belt', 'Kuiper belt', 'Protoplanetary disks', 'Chondrules', 'Chondrites', '1038', '994', '1294', '70', '893', '1300', '229', '228']

Constraints on the Distances and Timescales of Solid Migration in the Early Solar System from Meteorite Magnetism

https://ui.adsabs.harvard.edu/link_gateway/2020ApJ...896..103B/EPRINT_PDF

['1038', '994', '1294', '70', '893', '1300', '229', '228']

['Meteorites', 'Magnetic fields', 'Primordial magnetic fields', 'Asteroid belt', 'Kuiper belt', 'Protoplanetary disks', 'Chondrules', 'Chondrites']

['Meteorites', 'Magnetic fields', 'Primordial magnetic fields', 'Asteroid belt', 'Kuiper belt', 'Protoplanetary disks', 'Chondrules', 'Chondrites']

2022RNAAS...6...19J

In this work I estimate the number of close stellar encounters on a specific crosssectional area that may contain a planetary disk in a crowded star formation cluster. The approximation employs Monte Carlo runs to estimate the most likely value of the number of encounters as a function of stellar densities from 1.6 10SUP5SUP to 6.2 10SUP5SUP pcSUP3SUP velocity dispersions from 0.7 to 1.5 km sSUP1SUP and the lifetime of a typical star formation environment. I found that the most likely number of encounters on crosssectional areas with a radius of 400 au goes from one to three. Although four encounters are also likely to happen. This means that multiple strong stellar could happen on planetary disks in the early epoch of the star formation clusters.

2022-01-01T00:00:00Z

['363', '490', '1184', '1300', '1596']

Estimation of the Number of Stellar Encounters on a Crosssectional Area containing a Planetary Disk in Birth Clusters of Stars

https://ui.adsabs.harvard.edu/link_gateway/2022RNAAS...6...19J/EPRINT_PDF

['363', '490', '1184', '1300', '1596']

['Debris disks', 'Exoplanet dynamics', 'Orbits', 'Protoplanetary disks', 'Stellar dynamics']

['Debris disks', 'Exoplanet dynamics', 'Orbits', 'Protoplanetary disks', 'Stellar dynamics']

2020RNAAS...4...93G

We analyze the environmental features and growth history of highredshift halos from cosmological simulation data to determine the conditions that lead to Population III star formation. We use supportvector classification SVC to determine the separation in featurespace between Population III halos and halos that form no stars. We perform hyperparameter tuning but are unable to produce an SVC model that reliably classifies Population III halos. We perform feature selection and determine that among our included features LymanWerner radiation and halo mass have the most significant impact on an SVC models effectiveness.

2020-06-01T00:00:00Z

['Population III stars', 'Galaxy formation', '1285', '595']

Halo Environment for Population III Star Formation

https://ui.adsabs.harvard.edu/link_gateway/2020RNAAS...4...93G/EPRINT_PDF

['1285', '595']

['Population III stars', 'Galaxy formation']

['Population III stars', 'Galaxy formation']

2020ApJ...888...39L

The synthesis of chlorinebearing species in CO ice was studied by the irradiation of CHSUB3SUBClCO ice at 10 K with vacuumultraviolet VUV light and energetic electrons. In contrast to the photochemical behavior of CHSUB3SUBFCO ice photolysis of CHSUB3SUBClCO ice with Ly or broadband VUV light afforded various products. This discrepancy was attributed to the abundant absorption bands of CHSUB3SUBCl in the VUV region particularly in the Ly region. The Clbearing species including ClSUB2SUBO ClCO CSUB3SUBClSUB2SUB CSUB3SUBHCl and HOOCl were characterized by observing their IR features. In contrast electron bombardment of ice mixtures produced various carbon oxides and primary products such as CHSUB2SUBCl and HCO. In addition the mechanism of energetic processes in electron bombardment was discussed.

2020-01-01T00:00:00Z

['Astrochemistry', 'Molecular spectroscopy', 'Line positions', 'Molecule formation', 'Galaxy chemical evolution', 'Chemical abundances', '75', '2095', '2085', '2076', '580', '224']

Formation of Halogenbearing Species. II. Irradiation of Chloromethane in Carbon Monoxide Ice with VUV Light and Electrons

https://ui.adsabs.harvard.edu/link_gateway/2020ApJ...888...39L/EPRINT_PDF

['75', '2095', '2085', '2076', '580', '224']

['Astrochemistry', 'Molecular spectroscopy', 'Line positions', 'Unknown', 'Galaxy chemical evolution', 'Chemical abundances']

['Astrochemistry', 'Molecular spectroscopy', 'Line positions', 'Unknown', 'Galaxy chemical evolution', 'Chemical abundances']

2020ApJ...889...40S

The deuteriumhydrogen DH ratio of primordial water partitioned into a planetary interior seems to be different on Earth and Mars. Water from volcanic rocks originating from Earths deep mantle has a low DH ratio with high SUP3SUPHeSUP4SUPHe ratios implying that it was inherited partially from the solar nebula. In contrast the DH ratio of water in the Martian meteorites considered to represent the mantle does not trend toward that of the solar nebula. These differences may be owing to differences in the types of atmospheric structures formed on protoplanets accreting in the solar nebula. Using a 1D radiativeequilibrium model we analyze the thermal structure of a hybridtype protoatmosphere in which the solar nebula component dominates the upper layer while a degassed component dominates the lower layer. Our analysis implies Marssized protoplanets maintain a hybridtype protoatmosphere and the DH ratio of the lower atmosphere resembles that of the building blocks. Conversely when the mass is larger than Marssized the compositional stratification is collapsed by convective mixing of the solar nebula component with the degassed component and the DH ratio approaches that of the solar nebula. This tendency becomes stronger when the planetary mass is larger. If water vapor is distributed through a magma ocean into the planetary interior Marssized protoplanets are likely to reflect the DH ratios of the building blocks while larger protoplanets are likely to have acquired a solarnebulalike DH ratio.

2020-01-01T00:00:00Z

['Mars', 'Planet formation', 'Earth (planet)', 'Planetary atmospheres', 'Planetary science', '1007', '1241', '439', '1244', '1255']

DH Ratio in the Interiors of Rocky Protoplanets Accreting in the Solar Nebula

https://ui.adsabs.harvard.edu/link_gateway/2020ApJ...889...40S/EPRINT_PDF

['1007', '1241', '439', '1244', '1255']

['Mars', 'Planet formation', 'Earth (planet)', 'Planetary atmospheres', 'Planetary science']

['Mars', 'Planet formation', 'Earth (planet)', 'Planetary atmospheres', 'Planetary science']