adsabs/AstroCLIMB huggingface dataset:
Paper: Numerical Simulations of Drainage Grooves in Response to Extensional Fracturing: Testing the Phobos Groove Formation Model
Authors: Bin Cheng, Erik Asphaug, Ronald-Louis Ballouz, Yang Yu, Hexi Baoyin
Figure caption: Tidal deformation and internal stresses of the granular regolith. Tension is positive and compression negative. The patches represent the RVEs used for the stress evaluation. Data are from the simulation case of c  p  = 36 kPa. Note that only part of the width of the simulation is shown.
Paper: Numerical Simulations of Drainage Grooves in Response to Extensional Fracturing: Testing the Phobos Groove Formation Model
Authors: Bin Cheng, Erik Asphaug, Ronald-Louis Ballouz, Yang Yu, Hexi Baoyin
Figure caption: Different regimes of granular failure pattern of subsurface cohesive substrates.
Paper: Numerical Simulations of Drainage Grooves in Response to Extensional Fracturing: Testing the Phobos Groove Formation Model
Authors: Bin Cheng, Erik Asphaug, Ronald-Louis Ballouz, Yang Yu, Hexi Baoyin
Figure caption: Orbital evolution of Phobos within two possible in situ accreting formation scenarios.
Paper: The “Snow Line” on Venus’s Maxwell Montes: Varying Elevation Implies a Dynamic Atmosphere
Authors: Andriana Strezoski, Allan H. Treiman
Figure caption: (a) Left-look SAR mosaic of Maxwell Montes, in Mercator projection (61–71.4°N; 351–13°E); the center of the image is at 66.2°N, 2.0°E, and the center of Cleopatra crater is at 65.90°N, 6.94°E. The snow line was drawn manually at the strong contrast in SAR backscatter; segments of the snow line colored for clarity. Inset shows equal area projection, centered on Maxwell Montes. (b) Profile graph of the snow line elevation on Maxwell Montes vs. distance along the snow line, clockwise from its NW corner. Each colored segment corresponds to the color outline in Figure 1(a). Distance is somewhat arbitrary, being dependent on the number of points chosen and the spacing between them (Kappraff 1986). The lowest snow line elevation, ∼4.5 km above the datum, is near the SE corner of Maxwell Montes, and the highest snow line elevation, near 8 km, is near the NW corner of Maxwell Montes. The extreme variations in snow line elevation on the west flank of Maxwell (blue line) are interpreted to represent elevation errors related to its steep and rough topography.
Paper: The “Snow Line” on Venus’s Maxwell Montes: Varying Elevation Implies a Dynamic Atmosphere
Authors: Andriana Strezoski, Allan H. Treiman
Figure caption: (a). Locations of emissivity-reflectivity profile lines 1 and 2. b. Radar emissivity, Fresnel reflectivity, and elevation vs. distance along the profile lines. Data for the profiles was obtained from the JMARS web interface, and is at lower spatial resolution than the original data. Emissivity and Fresnel reflectivity are from JMARS (both ranging from 0.0 to 1.0) are multiplied by 10 to show them on the same scale as the topography (in km). The western gap in SAR radar data (Figure 3(a), left white stripe) is also a gap in the emissivity data, and is filled by interpolation (dashed lines). The eastern gap in SAR radar data (Figure 3(a), right white stripe) is not a gap in emissivity data; its coverage is continuous.
Paper: The “Snow Line” on Venus’s Maxwell Montes: Varying Elevation Implies a Dynamic Atmosphere
Authors: Andriana Strezoski, Allan H. Treiman
Figure caption: (a). Locations of emissivity profiles on left-look SAR image of Maxwell Montes, Mercator projection (61–71.4°N; 351–13°E); the center of the image is at 66.2°N, 2.0°E, and the center of Cleopatra crater is at 65.90°N, 6.94°E. Inset shows equal area projection, centered on Maxwell Montes. Profiles A (orange) and B (purple) to compare emissivity vs. elevation. (b) Profile graphs of elevation vs. emissivity overlain on a recreation of Figure 2(a) of Klose et al. (1992), their data shown as gray dots. Traverses A and B show that emissivity is systematically lower at Maxwell's SE than its NW.
Paper: Thermal Properties of 1847 WISE-observed Asteroids
Authors: Denise Hung, Josef Hanuš, Joseph R. Masiero, David J. Tholen
Figure caption: The thermal inertia, diameters, and albedos of our selected 1722 asteroids are shown with their uncertainties plotted against the reduced χ 2 of their TPM fits. The distributions of each parameter, ignoring their uncertainties, are shown in the accompanying histograms. The visible geometric albedos are calculated from the Bond albedos using Equation (3). Asteroids with a best-fit thermal inertia of 0 J m−2 s−0.5 K−1 are instead represented here with a value of 0.1 for the sake of the logarithmic scale. Error bars are only plotted for a best-fit thermal inertia of 50 J m−2 s−0.5 K−1 or above in order to avoid visual clutter. Our distributions of diameter and albedo are similar in shape to the NEATM-derived distributions found by Masiero et al. (2011) with a set of over 100,000 WISE-observed asteroids. We see in the top right panel that there appears to be a χ 2 boundary that decreases with diameter, but this is primarily a consequence of the larger relative flux uncertainties in observations of smaller asteroids. The albedo distribution is clearly bimodal, with a sharp peak at around A = 0.03/p  V  = 0.06 and a second peak at A = 0.09/p  V  = 0.23. While there are a few thermal inertia values recorded over 1000 J m−2 s−0.5 K−1, such cases should be treated with caution, as they are physically unrealistic and exceed nearly all other literature thermal inertia estimates.
Paper: Thermal Properties of 1847 WISE-observed Asteroids
Authors: Denise Hung, Josef Hanuš, Joseph R. Masiero, David J. Tholen
Figure caption: Example outputs of period searches conducted for (272) Antonia, (64) Angelina, (136514) 2005 QT36, and (87473) 2000 QK137. Each period search was conducted four times in total, using weights of 0.3, 0.5, 0.7, and 1 for the WISE lightcurves we supplemented to the DAMIT data set. The original DAMIT period is denoted by the vertical dashed line. The shaded region covers ±0.1% of the original DAMIT period. The period associated with the smallest ﹩{\chi }_{\mathrm{LC}}^{2}﹩ in the search range is marked in red. The difference between it and the DAMIT period is labeled P diff in each legend. The period search for (271) Antonia shows the ideal periodogram: a strong, tight V-shape with a clear single ﹩{\chi }_{\mathrm{LC}}^{2}﹩ minimum. Its unique period was automatically identified as there were no other solutions with a ﹩{\chi }_{\mathrm{LC}}^{2}﹩ under the threshold of 1.05 ﹩{\chi }_{\mathrm{LC},\min }^{2}﹩. (64) Angelina is an example of a case where we manually find the unique period. Like for (272) Antonia, the period search shows a clear V-shape and ﹩{\chi }_{\mathrm{LC}}^{2}﹩ minimum. However, there were a few other solutions under the ﹩{\chi }_{\mathrm{LC}}^{2}﹩ threshold with periods differing by a total range of 0.004 hour. (136514) 2005 QT36 is an example of where a unique period was automatically identified, but we rejected the period for its large offset relative to the original DAMIT period—in this case by over 0.3%. Finally, (87473) 2000 QK137 is an example of a periodogram that is mostly flat and shows large scatter, and thus no unique period could be recovered.
Paper: Thermal Properties of 1847 WISE-observed Asteroids
Authors: Denise Hung, Josef Hanuš, Joseph R. Masiero, David J. Tholen
Figure caption: The differences in pole orientation in ecliptic coordinates and period between the original DAMIT shape models and revised shape models for each asteroid. The periods are reported as a percentage difference from the original DAMIT period. The diamond points and colored histograms represent revised shape models where the χ 2 of the associated TPM fits fell into acceptable bounds by our criteria, while the circular points and grayscale histograms represent rejected TPM fits. We obtained a total of 1282 models for 696 asteroids. Of these, 63 asteroids had 1 DAMIT shape model and 1 revised shape model, 148 asteroids had 1 DAMIT shape model and 2 revised shape models, 43 asteroids had 2 DAMIT shape models and 1 revised shape model, and 440 asteroids had 2 DAMIT shape models and 2 revised shape models. In the cases where we had multiple DAMIT shape models, we only report the difference in the revised shape model with the closer DAMIT pole. The majority of revised shape models have poles which fall very closely to the DAMIT solutions with period differences of less than 0.01%. Due to the ambiguities in the pole orientation, we also see the mirror solutions that show up in the local maxima in λ at around ±180°.
Paper: Thermal Properties of 1847 WISE-observed Asteroids
Authors: Denise Hung, Josef Hanuš, Joseph R. Masiero, David J. Tholen
Figure caption: TPM example outputs for (321) Florentina, (725) Amanda, and (44612) 1999 RP27 and their respective best-fit thermal inertia, diameters, and Bond albedos found in Table 3. Each curve represents a different roughness profile as a pair of the crater opening angle γ  c  and crater density ρ  c  as denoted in Table 2. The dashed horizontal line is drawn at ﹩{\chi }_{\min }^{2}﹩ (1 + σ), where σ is related to the degrees of freedom ν by σ = ﹩\sqrt{2\nu }/\nu ﹩, and its intersection with the χ 2 curves approximates the TPM fit’s 1σ uncertainty bounds of the best-fit thermal parameters found. The shaded region shows the contiguous regions around the χ 2 minimum we use to identify the uncertainty ranges for each parameter.
Paper: Thermal Properties of 1847 WISE-observed Asteroids
Authors: Denise Hung, Josef Hanuš, Joseph R. Masiero, David J. Tholen
Figure caption: Our TPM fits’ minimum reduced χ 2 values, using both the nominal DAMIT shape models, ﹩{\chi }_{\mathrm{original}}^{2}﹩, and our new revised shape models, ﹩{\chi }_{\mathrm{new}}^{2}﹩. The points in green show asteroids that were initially removed with the χ 2 cuts in Section 3.1. The dashed line denotes where the two axes are equal. The shaded region shows where the values of the two axes are within 30% of each other. Of the 694 asteroids with revised shape models, we saw improvements in the χ 2 of their TPM fits for 540 asteroids compared to the fits using their DAMIT shape models. For the majority of asteroids, we either saw little change or slightly larger χ 2 when switching to the revised shape models, but we also had several instances of dramatically improved TPM fits with the revised shape models.
Paper: Large Impacts onto the Early Earth: Planetary Sterilization and Iron Delivery
Authors: Robert I. Citron, Sarah T. Stewart
Figure caption: Distribution of iron over the surface of the Earth 24 hr post impact. Surface iron is liquid or solid and is plotted as an equivalent layer thickness. The surface layer is defined as the particles with P < 10 GPa and ρ > 1000 kg m−3 within two smoothing lengths of the planetary radius.
Paper: Thermal Properties of 1847 WISE-observed Asteroids
Authors: Denise Hung, Josef Hanuš, Joseph R. Masiero, David J. Tholen
Figure caption: An example of what we consider a poorly constrained TPM fit for (6087) Lupo. Though the minimum reduced χ 2 is not very large at 2.3, the overall flatness of the χ 2 curve leaves the thermal inertia completely unconstrained.
Paper: Thermal Properties of 1847 WISE-observed Asteroids
Authors: Denise Hung, Josef Hanuš, Joseph R. Masiero, David J. Tholen
Figure caption: Example TPM fits to WISE thermal data for eight asteroids, folded on the rotation phase. The vast majority of asteroids in our sample were only observed by WISE over one to two days. Due to the cadence and the small number of WISE observations, the rotation phase is usually only sparsely sampled with large gaps in coverage (Wright et al. 2010).
Paper: Large Impacts onto the Early Earth: Planetary Sterilization and Iron Delivery
Authors: Robert I. Citron, Sarah T. Stewart
Figure caption: Melt volumes vs. impact energy for 45° impacts from our GADGET simulation results, compared with an analytic melt scaling from de Vries et al. (2016). The melt scaling from de Vries et al. (2016) is based on Abramov et al. (2012). The ×’s plotted in black use the parameter values from de Vries et al. (2016), while the adjusted points (red +’s) use slightly different values for several constants that are more consistent with our simulation model setup (see text). The gray circles and fit are for the complete melt volume (material with 100% degree of melting) from our numerical simulations. The black circles and fit are for the total melt volume (complete + incipient melt) from our numerical simulations.
Paper: Large Impacts onto the Early Earth: Planetary Sterilization and Iron Delivery
Authors: Robert I. Citron, Sarah T. Stewart
Figure caption: (a) Energy increase in silicate atmospheric particles for θ = 45° simulations. (b) Energy increase in silicate surface particles for θ = 45° simulations. The energy increase for only the supercritical fluid (SCF) component of the atmosphere and surface is shown in gray. The values for the best fit to a power law (Ae  b ) are listed. See Table C1.
Paper: Large Impacts onto the Early Earth: Planetary Sterilization and Iron Delivery
Authors: Robert I. Citron, Sarah T. Stewart
Figure caption: Bar charts showing the distribution of projectile iron 24 hr post impact. Projectile iron is divided into escaping material, atmospheric material, surface material (P > 10 GPa and ρ < 1000 kg m−3) and interior material (anything below the surface material). Charts are distributed in columns and rows according to the projectile velocity and mass. The x-axis in each bar chart shows runs of different impact angles (0° = head-on collision). See Table C3.
Paper: Large Impacts onto the Early Earth: Planetary Sterilization and Iron Delivery
Authors: Robert I. Citron, Sarah T. Stewart
Figure caption: Distribution of melt thickness 24 hr post impact for several example simulations. In the plotted coordinates the impact direction is east along the equator. The longitude of the impact point 24 hr post impact varies based on the planetary rotation induced by the impact.
Paper: Large Impacts onto the Early Earth: Planetary Sterilization and Iron Delivery
Authors: Robert I. Citron, Sarah T. Stewart
Figure caption: Energy conservation plots for an example simulation with M  i  = 0.006M Earth, v imp = 1.5v esc, and θ = 45°. (a) Relative energies are shown, displaying the exchange between kinetic energy (KE), the change in internal energy (ΔIE = IE – IE 0), and the change in the gravitational potential energy (ΔGPE = GPE – GPE0), all normalized to the initial kinetic energy (KE0). (b) Energy sums are shown, relative to the initial total participating energy (TPE = PGPE + IE + KE). The participating gravitational potential energy is given by PGPE = GPE – min(GPE).
Paper: Large Impacts onto the Early Earth: Planetary Sterilization and Iron Delivery
Authors: Robert I. Citron, Sarah T. Stewart
Figure caption: Bar charts showing the fraction of surface covered by >100, 10, or 1 km of melt after 24 hr of simulation time. Charts are distributed in columns and rows according to the projectile velocity and mass. The x-axis in each bar chart shows runs of different impact angles (0° = head-on collision).
Paper: Large Impacts onto the Early Earth: Planetary Sterilization and Iron Delivery
Authors: Robert I. Citron, Sarah T. Stewart
Figure caption: Bar charts showing the number of oceans that could be reduced by the iron in the atmosphere and deposited in the surface layer. We assume 1022 kg of iron can reduce 2.3 oceans of water. Charts are distributed in columns and rows according to the projectile velocity and mass. The x-axis in each bar chart shows runs of different impact angles (0° = head-on collision). Note that the y-axis scale changes depending on the projectile mass.
Paper: Large Impacts onto the Early Earth: Planetary Sterilization and Iron Delivery
Authors: Robert I. Citron, Sarah T. Stewart
Figure caption: Bar charts showing the fraction of surface with >100, 10, or 1 km of melt after 24 hr of simulation time. Charts are distributed in columns and rows according to the projectile velocity and mass. The x-axis in each bar chart shows runs of different impact angles (0° = head-on collision). As Figure 6 but includes thickness of condensed forsterite atmosphere.
Paper: Large Impacts onto the Early Earth: Planetary Sterilization and Iron Delivery
Authors: Robert I. Citron, Sarah T. Stewart
Figure caption: (a) Mass of forsterite melt (including supercritical fluid) in the surface and interior. (b) Mass of the forsterite atmosphere (all phases). Results are for after 24 hr of simulation time. See Table C2.
Paper: Thermal Properties of 1847 WISE-observed Asteroids
Authors: Denise Hung, Josef Hanuš, Joseph R. Masiero, David J. Tholen
Figure caption: The top panel plots the estimated nongravitational transverse acceleration parameter A 2 for every asteroid in our sample against the χ 2 of their best TPM fit, while the bottom panel shows the histogram of the same data. We estimated an A 2 value for each asteroid following the procedure outlined in Section 4.4. The data points are distinguished between asteroids which, for the purposes of deriving their shape models, had at least one dense optical lightcurve in their data set and those that did not. In our sample, we have 57 asteroids with an A 2 larger in magnitude than the smallest published A2  value on the JPL Small-Body Database (A2  = 1.9×10-15 au day-2), with 10 also having at least 1 dense optical lightcurve. These asteroids are the most promising for direct observational follow-up to confirm their Yarkovsky drift rates. However, because the lower bound on thermal inertia is unconstrained for 11 of these 57 best Yarkovsky candidates, the lower bound on A 2 here is also unconstrained, and as such the drift rates of these asteroids may be undetectably small.
Paper: The Sparse Atmospheric Model Sampling Analysis (SAMOSA) Intercomparison: Motivations and Protocol Version 1.0: A CUISINES Model Intercomparison Project
Authors: Jacob Haqq-Misra, Eric T. Wolf, Thomas J. Fauchez, Aomawa L. Shields, Ravi K. Kopparapu
Figure caption: Quasi–Monte Carlo selection of 16 points from the ExoPlaSim parameter space, with Sequence 1 (left) consisting of eight points that span the full parameter space and Sequence 2 (right) consisting of eight points within a region where full GCMs are expected to be numerically stable. Points marked with X symbols indicate numerically unstable atmospheres when calculated with ExoCAM. Numbered labels correspond to the sample number in Table 1.
Paper: Large Impacts onto the Early Earth: Planetary Sterilization and Iron Delivery
Authors: Robert I. Citron, Sarah T. Stewart
Figure caption: The habitability of Earth in the aftermath of late-accretion impacts depends strongly on the post-impact melt and iron distribution, and the energy deposited into the post-impact atmosphere. (a) In a nominal oblique impact a portion of the mantle is melted and ejecta heating also occurs downrange of the impact. The post-impact Earth has an ambiguous surface boundary of supercritical fluid, and the atmosphere consists of volatiles and a mix of vaporized silicate and projectile iron. Projectile iron is deposited in the melt/mantle/atmosphere, and some fraction also escapes the system with the impact ejecta. (b) In a head-on impact the projectile iron penetrates deep into the mantle, potentially reaching the core for larger impacts, and little material escapes the system. (c) In hit-and-run impacts, less melt is generated by the impact and a significant fraction of the projectile escapes the system.
Paper: The Sparse Atmospheric Model Sampling Analysis (SAMOSA) Intercomparison: Motivations and Protocol Version 1.0: A CUISINES Model Intercomparison Project
Authors: Jacob Haqq-Misra, Eric T. Wolf, Thomas J. Fauchez, Aomawa L. Shields, Ravi K. Kopparapu
Figure caption: Additional quasi–Monte Carlo selection of points from the ExoPlaSim parameter space. The left panel shows 16 additional points (green dots) that extend the selection shows in Figure 1, with Sequence 1b consisting of eight additional points continuing from Sequence 1 (dark dots), which spans the full parameter space, and Sequence 2b consisting of eight additional points continuing from Sequence 2 (blue dots), which is restricted to a region where full GCMs are expected to be numerically stable. The right panel shows Sequence 3, which is a sample of 32 new points that are selected within the parameter space but do not necessarily fall along the ExoPlaSim grid.
Paper: The Sparse Atmospheric Model Sampling Analysis (SAMOSA) Intercomparison: Motivations and Protocol Version 1.0: A CUISINES Model Intercomparison Project
Authors: Jacob Haqq-Misra, Eric T. Wolf, Thomas J. Fauchez, Aomawa L. Shields, Ravi K. Kopparapu
Figure caption: Global average surface temperature for all 16 cases using ExoCAM (left) and ExoPlaSim (right). Colors correspond to the climate state calculated for each case, with dashed lines showing approximate boundaries between climate states.
Paper: The Sparse Atmospheric Model Sampling Analysis (SAMOSA) Intercomparison: Motivations and Protocol Version 1.0: A CUISINES Model Intercomparison Project
Authors: Jacob Haqq-Misra, Eric T. Wolf, Thomas J. Fauchez, Aomawa L. Shields, Ravi K. Kopparapu
Figure caption: ExoCAM time series simulation output from case 6, showing mean (solid) and maximum (dashed) temperature (top left), stratospheric specific humidity (top right), net energy balance (bottom left), and total pressure (bottom right).
Paper: Large Impacts onto the Early Earth: Planetary Sterilization and Iron Delivery
Authors: Robert I. Citron, Sarah T. Stewart
Figure caption: Stacked bar charts showing how the initial projectile kinetic energy is distributed between the interior, surface, atmosphere, and escaping plus disk material, after 24 hr of simulation time. Charts are distributed in columns and rows according to the projectile velocity and mass. The x-axis in each bar chart shows simulations with different impact angles (0° = head-on collision). See Table C1.
Paper: Large Impacts onto the Early Earth: Planetary Sterilization and Iron Delivery
Authors: Robert I. Citron, Sarah T. Stewart
Figure caption: Snapshots of a simulation of a 0.006 M Earth projectile impacting a Earth target at 1.5 v esc and θ = 45°. Colors track the projectile and target core and mantle materials. Axis units are in present-day Earth radii (6371 km).
Paper: The Sparse Atmospheric Model Sampling Analysis (SAMOSA) Intercomparison: Motivations and Protocol Version 1.0: A CUISINES Model Intercomparison Project
Authors: Jacob Haqq-Misra, Eric T. Wolf, Thomas J. Fauchez, Aomawa L. Shields, Ravi K. Kopparapu
Figure caption: Average surface temperature for the 10 cases from Sequence 1 and Sequence 2 that remain stable with ExoCAM.