adsabs/AstroCLIMB huggingface dataset:
Paper: Examining Uranus’ ζ Ring in Voyager 2 Wide-angle Camera Observations: Quantifying the Ring’s Structure in 1986 and Its Modifications Prior to the Year 2007
Authors: M. M. Hedman, I. Regan, T. Becker, S. M. Brooks, I. de Pater, M. Showalter
Figure caption: Image of Uranus and its rings generated by Ian Regan from a series of low-resolution Voyager 2 images obtained after the spacecraft passed by the planet, along with a line drawing showing the locations of various rings based on renderings provided by the Uranus Viewer on the Ring-Moon Systems Node of the Planetary Data System (PDS). The innermost ring in the image is the ζ ring, and the outermost ring is the μ ring. The middle feature corresponds to a sheet of dust extending between the δ and λ rings, along with the ϵ ring. The ν ring is not obvious in this particular image. Streaks correspond to background stars. Note that this image has been heavily processed to improve the visibility of the faint rings.
Paper: Examining Uranus’ ζ Ring in Voyager 2 Wide-angle Camera Observations: Quantifying the Ring’s Structure in 1986 and Its Modifications Prior to the Year 2007
Authors: M. M. Hedman, I. Regan, T. Becker, S. M. Brooks, I. de Pater, M. Showalter
Figure caption: Voyager image C2684650 of the ζ ring at moderate (90°) phase angles near ring-plane crossing. The left panel shows the image, with the box indicating the region used to derive the ring brightness profile. The locations of the ζ and ϵ rings within this region are indicated by the letters above the box. The right panel shows the resulting profile of the region around the ζ ring derived from this portion of the image. The ζ ring produces the prominent spike centered around 37,500 km, while the peak around 42,000 km is likely due to the combined signal from the 4, 5, and 6 rings. The gray points are sampled every 50 km, while the solid line is binned over 500 km.
Paper: Aerodynamic Roughness Height of Gravel-covered Plains in the Puna of Argentina
Authors: James R. Zimbelman, Mauro G. Spagnuolo, Shanaka L. de Silva
Figure caption: Large (70 cm tall) gravel-covered megaripples at the Purulla site, the largest observed during the 2018 field work. This site was last visited by a member of our team in 2016 March, at which time a large nail placed on the megaripple crest showed no movement since being placed during 2010 November. Photo includes the nail (center), now located 21 cm south of the current crest (see Discussion). Arrow indicates dominant wind direction. Photo by JRZ on 2018 November 21.
Paper: Aerodynamic Roughness Height of Gravel-covered Plains in the Puna of Argentina
Authors: James R. Zimbelman, Mauro G. Spagnuolo, Shanaka L. de Silva
Figure caption: Tower 1 at the CPP West site during data collection. Five recording anemometers are logarithmically spaced with increasing height. Anemometer controllers are mounted on a tripod downwind of the tower. The tower needed to be held in place during data collection because of strong late-afternoon winds blowing almost parallel to the megaripple at left. It is worth noting the flat gravel plain upwind of the tower, continuous to the megaripple approximately 15 m upwind. An arrow indicates the dominant wind direction. Photo by JRZ on 2018 November 20
Paper: Aerodynamic Roughness Height of Gravel-covered Plains in the Puna of Argentina
Authors: James R. Zimbelman, Mauro G. Spagnuolo, Shanaka L. de Silva
Figure caption: Vertical views of gravel particles at the CPP site. Gravels on the crest of a 30 cm tall megaripple (a), and on the surface between megaripples (b), which is also representative of particles on gravel plains in the Puna. Photos by JRZ on 2018 November 19
Paper: Aerodynamic Roughness Height of Gravel-covered Plains in the Puna of Argentina
Authors: James R. Zimbelman, Mauro G. Spagnuolo, Shanaka L. de Silva
Figure caption: Study areas within the Puna of Argentina on a base image from Bing Maps. C—CPP; W—CPP West; L—Lago Purulla; P—Purulla; I—Incahuasi.
Paper: Aerodynamic Roughness Height of Gravel-covered Plains in the Puna of Argentina
Authors: James R. Zimbelman, Mauro G. Spagnuolo, Shanaka L. de Silva
Figure caption: Wind data record from Tower 1 at the CPP West site. Horizontal axis is local time; vertical axis is wind speed (m s−1).
Paper: The Case for Future Gravity Science Investigations at Saturn with a Planetary Orbiter
Authors: Marzia Parisi
Figure caption: Science questions (National Academies of Sciences, Engineering, and Medicine 2022) for the future robotic exploration of Saturn. From these, we derive related science objectives and realistic requirements on physical measurements.
Paper: The Case for Future Gravity Science Investigations at Saturn with a Planetary Orbiter
Authors: Marzia Parisi
Figure caption: Pericenter distribution as a function of Saturnian longitude and latitude (System III; Archinal et al. 2018) for cases 1 (a) and 2 (b). The color map reflects the altitude of the pericenters. The range of spanned latitudes is 14°N–51°N.
Paper: The Case for Future Gravity Science Investigations at Saturn with a Planetary Orbiter
Authors: Marzia Parisi
Figure caption: Simulation results in terms of spherical harmonic uncertainties (3σ) for different cases (1, 2, and 2+Cassini) and their comparison with the Cassini results (Iess et al. 2019).
Paper: The Case for Future Gravity Science Investigations at Saturn with a Planetary Orbiter
Authors: Marzia Parisi
Figure caption: Pericenter distribution as a function of Saturnian longitude and latitude (System III; Archinal et al. 2018) for case 2 (circles) and Cassini (diamonds).
Paper: The Case for Future Gravity Science Investigations at Saturn with a Planetary Orbiter
Authors: Marzia Parisi
Figure caption: Improvement over the formal uncertainties on the odd zonal harmonics as a function of pericenter number for the reference trajectory (case 1). The circles represent the 3σ uncertainties for the harmonic coefficient output of the current simulations. The dashed lines are the Cassini 3σ uncertainties from Iess et al. (2019).
Paper: The Case for Future Gravity Science Investigations at Saturn with a Planetary Orbiter
Authors: Marzia Parisi
Figure caption: Simulated Doppler residuals (60 s integration time) during one sample tracking pass (2044 February 15–16) that involves the Goldstone, Canberra, and Madrid complexes. The closest approach occurs at 01:23:00 UTC on 2044 February 16, Earth Receive Time. The noise level for the overall Ka bandpass is ∼2.0 mHz or ∼9.3 μm s−1.
Paper: Stable Brine Layers beneath Europa’s Chaos
Authors: C. J. Chivers, J. J. Buffo, B. E. Schmidt
Figure caption: The distinctive thermochemical evolution of melt lenses suggests that, in each salinity scenario, brines beneath chaos terrains will cease appreciable freezing for at least 100 kyr and may be quasi-stabile for tens of thousands of years further. (a)–(c) Time series of bulk thermal and chemical evolution of melt lenses including the fraction of remaining brine V/V 0 (blue), the liquid salinity S (orange), and brine melting temperature T  m  (green), with the salinity scenario labeled. Gray boxes in the top plots show the time domain of (e)–(f). (d) Cross-sectional profiles through the center of the melt lenses for NaCl (red) and MgSO4 (pink) after 350 kyr of evolution (x ∼ 0, in the last plots of Figure 4). (e)–(f) Time series of the last 100 kyr of evolution from plots in (b)–(c) highlighted in the gray box, with the left being NaCl and right MgSO4, same as those directly above.
Paper: Adsorption Kinetics of Water and Argon on Lunar Grains
Authors: Norbert Schörghofer
Figure caption: Measured adsorption isotherm for a lunar sample and various isotherm models. The vertical axis is the adsorbate mass relative to a monolayer of H2O. The horizontal axis is the vapor pressure relative to the saturation vapor pressure of the condensed phase (here the liquid), which equates to relative humidity. CS74 = Cadenhead & Stetter (1974), ST07 = Schorghofer & Taylor (2007), and SA14 = Schorghofer & Aharonson (2014)
Paper: Adsorption Kinetics of Water and Argon on Lunar Grains
Authors: Norbert Schörghofer
Figure caption: Distribution of desorption activation energies according to TPD measurements on lunar samples. The sublimation energy of (bulk) ice is also shown. The ice and TPD measurements assume different prefactors, ν, so the difference between the energies is effectively larger.
Paper: Adsorption Kinetics of Water and Argon on Lunar Grains
Authors: Norbert Schörghofer
Figure caption: Molecular residence times for argon. Residence time on solid argon are calculated from data in Shakeel et al. (2018). Dohnalek et al. (2002) measured argon adsorption on MgO(100). Argon adsorption on terrestrial labradorite and lunar sample 15415 as measured by Bernatowicz & Podosek (1991). Hodges (1982), Grava et al. (2015), and Kegerreis et al. (2017) derived their estimates from exospheric models. The residence times from Grava et al. (2015) include time for subsurface diffusion. Smith et al. (2016) measured adsorption of argon on amorphous solid water (ASW) as a function of coverage.
Paper: Adsorption Kinetics of Water and Argon on Lunar Grains
Authors: Norbert Schörghofer
Figure caption: Depth profiles of adsorbate concentration between the surface and a buried ice deposit at 1 m depth for static temperature profiles. The left panel shows the temperature profile with and without a geothermal heat flux F  g . The right panel shows numerical solutions for the adsorbate concentration (dots) and an analytical solution for constant temperature (line), Equations (B2), (B5), and (B6).
Paper: Adsorption Kinetics of Water and Argon on Lunar Grains
Authors: Norbert Schörghofer
Figure caption: Molecular residence times as a function of inverse temperature for ice (blue), a monolayer of adsorbed water according to the BET isotherm (purple), and several energies from TPD measurements for lunar samples (orange and green). The dash orange line, compared to the full orange line, shows the change that occurs if the frequency prefactor is changed from 1013 s−1 to 1016 s−1, and the energy increased correspondingly. The horizontal dotted lines indicate several physically relevant timescales.
Paper: Adsorption Kinetics of Water and Argon on Lunar Grains
Authors: Norbert Schörghofer
Figure caption: Model surface temperatures (top) and adsorbate retention (bottom) as a function of time for several latitudes. Solid lines are without photodestruction, and dashed lines are with photodestruction. The dotted line is for a smaller initial adsorbate mass, but the result quickly becomes insensitive to the initial mass.
Paper: Adsorption Kinetics of Water and Argon on Lunar Grains
Authors: Norbert Schörghofer
Figure caption: Simple model for the distribution of desorption energies. Due to grain surface diffusion, sites with the highest binding energies are occupied first.
Paper: Adsorption Kinetics of Water and Argon on Lunar Grains
Authors: Norbert Schörghofer
Figure caption: Molecular residence times according to several parameterizations of the desorption rate S as a function of coverage (a) and as a function of temperature (b). The residence times are calculated as ﹩\tau =\min (\theta ,{\theta }_{m})/S﹩.
Paper: Evidence for Fine-grained Material at Lunar Red Spots: Insights from Thermal Infrared and Radar Data Sets
Authors: Benjamin D Byron, Catherine M. Elder, Timothy D. Glotch, Paul O. Hayne, Lori M. Pigue, Joshua T. S. Cahill
Figure caption: Rock abundance (left), H-parameter (center), and Mini-RF CPR (right) maps covering CBVC. The white outlines represent the boundaries of the red spot locations determined by our study. The white box in the center image is the red spot location analyzed in Figure 15. Note that the color scale for the H-parameter map is inverted. The southeastern part of CBVC and extending beyond the boundary (white arrows) is a high-albedo area that has low RA, high H-parameter, and low CPR. All maps are overlain on LROC NAC image NAC_ROI_COMPBELKLOE_E613N0993_5M. The Mini-RF CPR data are overlain on the S1 total backscatter data.
Paper: Evidence for Fine-grained Material at Lunar Red Spots: Insights from Thermal Infrared and Radar Data Sets
Authors: Benjamin D Byron, Catherine M. Elder, Timothy D. Glotch, Paul O. Hayne, Lori M. Pigue, Joshua T. S. Cahill
Figure caption: Histograms of H-parameter for selected areas within the red spot boundaries (white boxes in Figures 3, 4, 7, 8, 9, 11, 12; orange histograms) and areas outside the red spot boundaries (blue histograms). Selected regions within a number of red spots have a noticeably higher H-parameter than nearby mare regolith.
Paper: Evidence for Fine-grained Material at Lunar Red Spots: Insights from Thermal Infrared and Radar Data Sets
Authors: Benjamin D Byron, Catherine M. Elder, Timothy D. Glotch, Paul O. Hayne, Lori M. Pigue, Joshua T. S. Cahill
Figure caption: Evidence for pyroclastic material at the Lassell Massif and Mons Hansteen red spots. Left: oblique view of the irregular craters G and K on the Lassell Massif. Black arrows point out exposures of low albedo material that may be related to pyroclastic deposits, as described in Ashley et al. (2016). Right: oblique view of the Pitted Unit on Mons Hansteen. Black arrows point out rock exposures at higher topography areas of the Pitted Unit. The higher thermal inertia rocky exposures may be obscuring any low thermal inertia materials that preferentially accumulate in the lower-lying areas on top of Mons Hansteen. Images are from LROC NAC mosaics M1108311369 and M1154506530LR, respectively.
Paper: Evidence for Fine-grained Material at Lunar Red Spots: Insights from Thermal Infrared and Radar Data Sets
Authors: Benjamin D Byron, Catherine M. Elder, Timothy D. Glotch, Paul O. Hayne, Lori M. Pigue, Joshua T. S. Cahill
Figure caption: Close-up views of craters on the Gruithuisen domes. Left: Diviner H-parameter map of the Gruithuisen Gamma dome. The white arrow points out the crater where Ivanov et al. (2016) found evidence for possible pyroclastic material. Center: Diviner H-parameter map of the Gruithuisen Delta dome. The white arrow points out a small area of high H-parameter on the maria just west of the dome. Right: LROC NAC images (M155499183L and M155499183R) showing the ∼120 m diameter fresh crater west of the Delta dome that is likely associated with the cold spot seen in the H-parameter map. Note that the H-parameter color scale is inverted. The Diviner maps are overlain on LROC NAC image NAC_ROI_GRUITHSNLOB_E362N3197_5M.
Paper: Evidence for Fine-grained Material at Lunar Red Spots: Insights from Thermal Infrared and Radar Data Sets
Authors: Benjamin D Byron, Catherine M. Elder, Timothy D. Glotch, Paul O. Hayne, Lori M. Pigue, Joshua T. S. Cahill
Figure caption: Histograms of rock abundance for areas within the red spot boundaries (white polygons in Figures 3–12; orange histograms) and outside the red spot boundaries (blue histograms). Red spots generally have similar or slightly lower RA than nearby regions.
Paper: Evidence for Fine-grained Material at Lunar Red Spots: Insights from Thermal Infrared and Radar Data Sets
Authors: Benjamin D Byron, Catherine M. Elder, Timothy D. Glotch, Paul O. Hayne, Lori M. Pigue, Joshua T. S. Cahill
Figure caption: Clementine color-ratio maps of Mons La Hire (left) and Montes Spitzbergen (right). The reddest area of Mons La Hire is mostly surrounding a crater on the east side of the feature, and the reddest areas of Montes Spitzbergen are found in the lower-lying areas surrounding the peaks.
Paper: Evidence for Fine-grained Material at Lunar Red Spots: Insights from Thermal Infrared and Radar Data Sets
Authors: Benjamin D Byron, Catherine M. Elder, Timothy D. Glotch, Paul O. Hayne, Lori M. Pigue, Joshua T. S. Cahill
Figure caption: Diviner H-parameter map (left) and Mini-RF S1 Return map (right) for Darney-chi. White arrows show the radar-dark and low thermal inertia area in northwestern Darney-chi.
Paper: Evidence for Fine-grained Material at Lunar Red Spots: Insights from Thermal Infrared and Radar Data Sets
Authors: Benjamin D Byron, Catherine M. Elder, Timothy D. Glotch, Paul O. Hayne, Lori M. Pigue, Joshua T. S. Cahill
Figure caption: Histograms of the H-parameter for areas within the red spot boundaries (white polygons in Figures 3–12; orange histograms) and outside the red spot boundaries (blue histograms).
Paper: The Importance of Isentropic Mixing in the Formation of the Martian Polar Layered Deposits
Authors: E. R. Ball, W. J. M. Seviour, D. M. Mitchell
Figure caption: The percentage of tracer remaining above 75° N/S at 30 sols after initialization. The concentration, given as a percentage, is given to be ﹩{c}_{{\mathrm{pole}}_{30}}/{c}_{{\mathrm{pole}}_{0}}﹩ in the NH, where ﹩{c}_{{\mathrm{pole}}_{t}}﹩ is an area-weighted polar average of tracer concentration at 300 K t sols after initialization. Corresponding L  s  values for initialization (﹩{{L}_{s}}_{0}﹩) and 30 sols after initialization (﹩{{L}_{s}}_{30}﹩) are given in the legend. As the tracer is initialized with a sinusoidal profile (Equation (1)), typically it is transported into the southern polar region; hence, we take the inverse ﹩{c}_{{\mathrm{pole}}_{0}}/{c}_{{\mathrm{pole}}_{30}}﹩ in the SH, for comparability. Lower percentages indicate greater transport, as more tracer has been transported into/away from the polar region over 30 sols. Solid lines show γ = 0.093, and dashed lines show γ = 0.
Paper: The Importance of Isentropic Mixing in the Formation of the Martian Polar Layered Deposits
Authors: E. R. Ball, W. J. M. Seviour, D. M. Mitchell
Figure caption: Winter anomaly of the latitude of the jet on the 50 Pa surface (﹩{\phi }_{{u}_{\max }}﹩) for (a, b) γ = 0.093; (c, d) γ = 0; and (e, f) dust-scale simulations. Panels (g) and (h) show ϕ HC for ε = 25° and λ = 1, and panels (a)–(f) show the anomaly from this value in the corresponding suite of simulations. The left column shows the winter NH, and the right column shows the winter SH.
Paper: The Importance of Isentropic Mixing in the Formation of the Martian Polar Layered Deposits
Authors: E. R. Ball, W. J. M. Seviour, D. M. Mitchell
Figure caption: Top: northern winter mean meridional streamfunction (shading; 108 kg s−1), zonal-mean zonal wind (thick contours; m s−1); bottom: zonal-mean PV (orange; MPVU) and effective diffusivity (blue) on the 300 K level. The latitudes of our metrics (ϕ HC, ﹩{\phi }_{{u}_{\max }}﹩, ϕ PV, ﹩{\kappa }_{{\mathrm{eff}}_{300}}﹩) are indicated either by crosses or, if the calculation is based on an integral or mean, by bars across the region in question. The data used are from the present-day simulation (γ = 0.093, ε = 25°).
Paper: The Importance of Isentropic Mixing in the Formation of the Martian Polar Layered Deposits
Authors: E. R. Ball, W. J. M. Seviour, D. M. Mitchell
Figure caption: Constant contours of tracer c* = c on a sphere of radius r. Left: an example of tracer geometry with large effective diffusivity. Right: an example with small effective diffusivity. In each, the red contour represents a contour of tracer c* = c enclosing the same area A. The blue contour is the shortest possible contour enclosing A, sits at latitude ϕ  e , and has length ﹩{L}_{\min }=2\pi r\cos {\phi }_{e}﹩. In the left panel ﹩{L}_{e}\gg {L}_{\min }﹩, whereas in the right panel ﹩{L}_{e}\approx {L}_{\min }﹩.
Paper: The Importance of Isentropic Mixing in the Formation of the Martian Polar Layered Deposits
Authors: E. R. Ball, W. J. M. Seviour, D. M. Mitchell
Figure caption: Winter anomaly of the strength of the jet on the 50 Pa surface (﹩{u}_{\max }﹩) for (a, b) γ = 0.093; (c, d) γ = 0; and (e, f) dust-scale simulations. Panels (g) and (h) show ϕ HC for ε = 25° and λ = 1, and panels (a)–(f) show the anomaly from this value in the corresponding suite of simulations. The left column shows the winter NH, and the right column shows the winter SH.
Paper: The Importance of Isentropic Mixing in the Formation of the Martian Polar Layered Deposits
Authors: E. R. Ball, W. J. M. Seviour, D. M. Mitchell
Figure caption: Winter anomaly of the strength of the PV maximum (﹩{\mathrm{PV}}_{\max }﹩) for (a, b) γ = 0.093; (c, d) γ = 0; and (e, f) dust-scale simulations. Panels (g) and (h) show ϕ HC for ε = 25° and λ = 1, and panels (a)–(f) show the anomaly from this value in the corresponding suite of simulations. The left column shows the winter NH, and the right column shows the winter SH.
Paper: The Importance of Isentropic Mixing in the Formation of the Martian Polar Layered Deposits
Authors: E. R. Ball, W. J. M. Seviour, D. M. Mitchell
Figure caption: Winter anomaly of the latitude of the descending branch of the Hadley circulation (ϕ HC) for (a, b) γ = 0.093; (c, d) γ = 0; and (e, f) dust-scale simulations. Panels (g) and (h) show ϕ HC for ε = 25° and λ = 1, and panels (a)–(f) show the anomaly from this value in the corresponding suite of simulations. The left column shows the winter NH, and the right column shows the winter SH.
Paper: The Importance of Isentropic Mixing in the Formation of the Martian Polar Layered Deposits
Authors: E. R. Ball, W. J. M. Seviour, D. M. Mitchell
Figure caption: Winter anomaly of the latitude of the maximum PV value on the 300 K level (ϕ PV) for (a, b) γ = 0.093; (c, d) γ = 0; and (e, f) dust-scale simulations. Panels (g) and (h) show ϕ HC for ε = 25° and λ = 1, and panels (a)–(f) show the anomaly from this value in the corresponding suite of simulations. The left column shows the winter NH, and the right column shows the winter SH.
Paper: The Importance of Isentropic Mixing in the Formation of the Martian Polar Layered Deposits
Authors: E. R. Ball, W. J. M. Seviour, D. M. Mitchell
Figure caption: Winter anomaly of the strength of the Hadley circulation (﹩{\psi }_{\max }﹩) for (a, b) γ = 0.093; (c, d) γ = 0; and (e, f) dust-scale simulations. Panels (g) and (h) show ϕ HC for ε = 25° and λ = 1, and panels (a)–(f) show the anomaly from this value in the corresponding suite of simulations. The left column shows the winter NH, and the right column shows the winter SH.
Paper: Validation of the Survey Simulator Tool for the NEO Surveyor Mission Using NEOWISE Data
Authors: Joseph R. Masiero, Dar W. Dahlen, Amy K. Mainzer, William F. Bottke, Jennifer C. Bragg, James. M. Bauer, Tommy Grav
Figure caption: Validation of the NSS thermal model is done through comparison of the predicted magnitude to the WISE-measured magnitudes for W3 (top) and W4 (bottom). Columns show a density plot of the comparison between the prediction and the measurement in gray, along with a best-fit linear trend in red (left); a density plot of the measured magnitude against the difference between the simulation and the measurement, with the vertical red line showing the approximate transition into a background-impacted regime (middle); and histograms of the magnitude differences for all objects in black and those brighter than the background cutoff in red (right). The spatial bins in the density plots are shaded following a logarithmic scale to emphasize the bright tail.
Paper: Validation of the Survey Simulator Tool for the NEO Surveyor Mission Using NEOWISE Data
Authors: Joseph R. Masiero, Dar W. Dahlen, Amy K. Mainzer, William F. Bottke, Jennifer C. Bragg, James. M. Bauer, Tommy Grav
Figure caption: Comparison of NSS-predicted positions for 1000 known NEOs with well-determined orbits (i.e., numbered asteroids) to the JPL Horizons position of each object. The errors for each object are plotted as a blue point at each time step evaluated. Errors for individual objects will grow well above the rms value and then decrease in cases where an object has a close pass with the telescope. The black line shows the rms error for the population evaluated at each time step.