adsabs/AstroCLIMB huggingface dataset:
Paper: Morphological and Spectral Characterization of Lunar Regolith Breakdown due to Water Ice
Authors: A. Shackelford, K. L. Donaldson Hanna, M. Horton, D. Noce
Figure caption: Clump analysis on a Ca/Al image of LHS-1 that was frozen for 6 months with 30 wt% of water ice. Purple boxes: uncountable areas. Green lines: maximum Feret diameters. Orange boxes: primary clump area-defining polygons. Pink markers: primary clump counts. Yellow markers: secondary clump counts. The inset illustrates the difference between primary clumps (conglomerates >2 μm in diameter) and secondary clumps (conglomerates <2 μm in diameter). A “fine,” or single particle <2 μm in diameter, is shown circled in red.
Paper: Morphological and Spectral Characterization of Lunar Regolith Breakdown due to Water Ice
Authors: A. Shackelford, K. L. Donaldson Hanna, M. Horton, D. Noce
Figure caption: Energy Dispersive X-ray Spectroscopy (EDS) elemental map (at left) with magnesium (green), calcium (blue), and aluminum (red) counts overlaid onto an SEM image (at right) of LMS-1, frozen for 1 month with 1 wt% of water taken at 40×  magnification. Green regions are indicative of pyroxene/olivine content, while pink regions are indicative of plagioclase. The Ca/Al or plagioclase particle we imaged to obtain our “clumps” and “fines” images for this sample is circled in red. The scale bar in the image at the right applies to both images.
Paper: Morphological and Spectral Characterization of Lunar Regolith Breakdown due to Water Ice
Authors: A. Shackelford, K. L. Donaldson Hanna, M. Horton, D. Noce
Figure caption: Primary clump count for Mg clump (top) and Ca/Al clump (bottom) images of all samples.
Paper: Morphological and Spectral Characterization of Lunar Regolith Breakdown due to Water Ice
Authors: A. Shackelford, K. L. Donaldson Hanna, M. Horton, D. Noce
Figure caption: Median values for particle sphericity (top), elongation (middle), and ECD (bottom) of the <63 μm particle size fraction of LHS-1. Water ice content increases from unaltered to 30 wt% from left to right. The different symbols show the amount of time that the sample was frozen.
Paper: Morphological and Spectral Characterization of Lunar Regolith Breakdown due to Water Ice
Authors: A. Shackelford, K. L. Donaldson Hanna, M. Horton, D. Noce
Figure caption: Median values for particle sphericity (top), elongation (middle), and ECD (bottom) for the <63 μm particle size fraction of LMS-1. Water ice content increases from unaltered to 30 wt% from left to right. The different symbols show the amount of time that the sample was frozen.
Paper: Morphological and Spectral Characterization of Lunar Regolith Breakdown due to Water Ice
Authors: A. Shackelford, K. L. Donaldson Hanna, M. Horton, D. Noce
Figure caption: ECD, sphericity, and elongation, respectively, as defined by the ExpertShape software, as well as multiple examples of “thresholded” particles.
Paper: Morphological and Spectral Characterization of Lunar Regolith Breakdown due to Water Ice
Authors: A. Shackelford, K. L. Donaldson Hanna, M. Horton, D. Noce
Figure caption: Secondary clump count for Mg clump (top) and Ca/Al clump (bottom) images of all samples.
Paper: Morphological and Spectral Characterization of Lunar Regolith Breakdown due to Water Ice
Authors: A. Shackelford, K. L. Donaldson Hanna, M. Horton, D. Noce
Figure caption: Magnesium fines image of LMS-1 that was frozen for 1 month with 1 wt% of water ice. Counts are shown here within an inset, as displaying all counts renders the image unreadable due to the number of markers. For a resolution reference, particle #42 in the inset is only 0.13 μm in diameter.
Paper: Morphological and Spectral Characterization of Lunar Regolith Breakdown due to Water Ice
Authors: A. Shackelford, K. L. Donaldson Hanna, M. Horton, D. Noce
Figure caption: Primary clump mean maximum Feret diameter in microns.
Paper: Effect of Equation of State and Cutoff Density in Smoothed Particle Hydrodynamics Simulations of the Moon-forming Giant Impact
Authors: Scott D. Hull, Miki Nakajima, Natsuki Hosono, Robin M. Canup, Rene Gassmöller
Figure caption: Time evolution of the disk for simulations with impact parameter b = 0.75. Each cutoff density is represented by a distinct line color. The solid lines represent Stewart M-ANEOS simulations, the dashed lines represent N-SPH M-ANEOS simulations, and the dotted lines correspond to our high-resolution run (5b073S-high). (a) Average disk entropy with entropy gain due to orbital circularization assessed at each time step included, (b) average disk temperature, (c) disk VMF calculated with effects of orbital circularization included, (d) disk mass, (e) disk angular momentum, (f) mass fraction of material in the disk originating from Theia. A version of this figure without the effects of orbital circularization of the disk is available in Appendix C, Figure 19.
Paper: Effect of Equation of State and Cutoff Density in Smoothed Particle Hydrodynamics Simulations of the Moon-forming Giant Impact
Authors: Scott D. Hull, Miki Nakajima, Natsuki Hosono, Robin M. Canup, Rene Gassmöller
Figure caption: Time evolution of the disk for simulations with impact parameter b = 0.73. Each cutoff density is represented by a distinct line color. The solid lines represent Stewart M-ANEOS simulations, the dashed lines represent N-SPH M-ANEOS simulations, and the dotted lines correspond to our high-resolution run (5b073S-high). (a) Average disk entropy with entropy gain due to orbital circularization assessed at each time step included, (b) average disk temperature, (c) disk VMF calculated with effects of orbital circularization included, (d) disk mass, (e) disk angular momentum, (f) mass fraction of material in the disk originating from Theia. A version of this figure without the effects of orbital circularization of the disk is available in Appendix C, Figure 18.
Paper: Effect of Equation of State and Cutoff Density in Smoothed Particle Hydrodynamics Simulations of the Moon-forming Giant Impact
Authors: Scott D. Hull, Miki Nakajima, Natsuki Hosono, Robin M. Canup, Rene Gassmöller
Figure caption: The liquid–vapor phase curves for both Stewart (left column) and N-SPH (right column) M-ANEOS forsterite. The top row corresponds to b = 0.73 simulations, and the bottom row corresponds to b = 0.75 simulations. The disk particles for each ρ  c  are plotted with their entropy gains associated with orbital circularization included. Yellow points correspond to simulation 5b073S-high in panel (a) and 2000b075N-low in panel (d). The regions of the plots are color-coded to represent their EoS-specific phase state, with the orange region between the liquid and vapor phase curves representing a mixture of liquid and vapor. The peak of the phase curves represents the critical point, above which we consider the particle to be in a supercritical state. All supercritical particles are treated as 100% vapor in our VMF calculations. The minimum temperatures shown here reflect the initial conditions. A version of this figure without the effects of orbital circularization of the disk is available in Appendix C, Figure 12.
Paper: Effect of Equation of State and Cutoff Density in Smoothed Particle Hydrodynamics Simulations of the Moon-forming Giant Impact
Authors: Scott D. Hull, Miki Nakajima, Natsuki Hosono, Robin M. Canup, Rene Gassmöller
Figure caption: Evolution of the giant impact and the protolunar disk for simulations using Stewart M-ANEOS with an initial impact parameter of b = 0.73. The axes give the x–y spatial coordinates relative to the proto-Earth’s center of mass given in increments of 104 km. Particles are sorted by their z-axis values, and colors indicate whether the particle is part of the proto-Earth (green), part of the disk (yellow), or escaping (purple). Red particles indicate final disk particles that have density values equal to ρ  c  at the given time, and the percentage of final disk particles that are at the value of ρ  c  at each time is noted in the lower right corner of each panel. Each column corresponds to a unique run, and each row is a snapshot of the simulation at (a)–(e) 2.78, (f)–(j) 5.56, (k)–(o) 13.89, and (p)–(t) 50 hr.
Paper: Effect of Equation of State and Cutoff Density in Smoothed Particle Hydrodynamics Simulations of the Moon-forming Giant Impact
Authors: Scott D. Hull, Miki Nakajima, Natsuki Hosono, Robin M. Canup, Rene Gassmöller
Figure caption: Evolution of the giant impact and the protolunar disk for simulations using N-SPH M-ANEOS with an initial impact parameter of b = 0.73. The axes give the x–y spatial coordinates relative to the proto-Earth’s center of mass given in increments of 104 km. Particles are sorted by their z-axis values, and colors indicate whether the particle is part of the proto-Earth (green), part of the disk (yellow), or escaping (purple). Red particles indicate final disk particles that have density values equal to ρ  c  at the given time, and the percentage of final disk particles that are at the value of ρ  c  at each time is noted in the lower right corner of each subplot. Each column corresponds to a unique run, and each row is a snapshot of the simulation at (a)–(d) 2.78, (e)–(h) 5.56, (i)–(l) 13.89, and (m)–(p) 50 hr.
Paper: Effect of Equation of State and Cutoff Density in Smoothed Particle Hydrodynamics Simulations of the Moon-forming Giant Impact
Authors: Scott D. Hull, Miki Nakajima, Natsuki Hosono, Robin M. Canup, Rene Gassmöller
Figure caption: Disk particles for simulations with impact parameter b = 0.73 relative to the EoS-specific Hugoniot curve (dashed curve) and the calculated Hugoniot curve (solid curve) given by the Rankine–Hugoniot relations. (a) Disk particles from Stewart M-ANEOS runs at the moment of the initial impact between Earth and Theia. (b) Disk particles from N-SPH M-ANEOS runs at the moment of the initial impact between Earth and Theia. (c) Disk particles from Stewart M-ANEOS runs at 50 simulated hr. (d) Disk particles from N-SPH M-ANEOS runs at 50 simulated hr. The disk particles at 50 hr are not well approximated by the Hugoniot and cannot be used to constrain a value of ρ  c  for the disk. The wavelike features in panels (c) and (d) are the result of particles that have reached their respective values of ρ  c .
Paper: Effect of Equation of State and Cutoff Density in Smoothed Particle Hydrodynamics Simulations of the Moon-forming Giant Impact
Authors: Scott D. Hull, Miki Nakajima, Natsuki Hosono, Robin M. Canup, Rene Gassmöller
Figure caption: The supported smoothing length H  i  as a function of particle density, where each line represents a different simulation particle resolution. The functional dependency of h on particle mass m scales as a function of particle count; therefore, particle mass is given as the total mass of the canonical giant impact, M tot = 1.019 M ⊕, divided by the total number of particles in the simulation.
Paper: Effect of Equation of State and Cutoff Density in Smoothed Particle Hydrodynamics Simulations of the Moon-forming Giant Impact
Authors: Scott D. Hull, Miki Nakajima, Natsuki Hosono, Robin M. Canup, Rene Gassmöller
Figure caption: The Wendland C6 SPH kernel as a function of particle distance. The kernel is given for our minimum and maximum values of ρ  c , ρ  c  = 5 kg m−3 (solid lines) and ρ  c  = 2000 kg m−3 (dashed lines). Line colors represent different particle resolutions.
Paper: Effect of Equation of State and Cutoff Density in Smoothed Particle Hydrodynamics Simulations of the Moon-forming Giant Impact
Authors: Scott D. Hull, Miki Nakajima, Natsuki Hosono, Robin M. Canup, Rene Gassmöller
Figure caption: Disk particles from runs with b = 0.73 and using Stewart M-ANEOS colored as a function of specific entropy change (ΔS) between the displayed time in each row and ∼3 hr prior. The axes give the x–y spatial coordinates relative to the proto-Earth’s center of mass given in increments of 104 km. Particles are sorted by their z-axis values. Each column corresponds to a unique run, and each row is a snapshot of the simulation at (a)–(e) 41.67, (f)–(j) 44.45, (k)–(o) 47.22, and (p)–(t) 50 hr.
Paper: Effect of Equation of State and Cutoff Density in Smoothed Particle Hydrodynamics Simulations of the Moon-forming Giant Impact
Authors: Scott D. Hull, Miki Nakajima, Natsuki Hosono, Robin M. Canup, Rene Gassmöller
Figure caption: Disk particles from runs with b = 0.75 and using N-SPH M-ANEOS colored as a function of specific entropy change (ΔS) between the displayed time in each row and ∼3 hr prior. The axes give the x–y spatial coordinates relative to the proto-Earth’s center of mass given in increments of 104 km. Particles are sorted by their z-axis values. Each column corresponds to a unique run, and each row is a snapshot of the simulation at (a)–(e) 41.67, (f)–(j) 44.45, (k)–(o) 47.22, and (p)–(t) 50 hr.
Paper: Effect of Equation of State and Cutoff Density in Smoothed Particle Hydrodynamics Simulations of the Moon-forming Giant Impact
Authors: Scott D. Hull, Miki Nakajima, Natsuki Hosono, Robin M. Canup, Rene Gassmöller
Figure caption: Disk particles from runs with b = 0.73 and using N-SPH M-ANEOS colored as a function of specific entropy change (ΔS) between the displayed time in each row and ∼3 hr prior. The axes give the x–y spatial coordinates relative to the proto-Earth’s center of mass given in increments of 104 km. Particles are sorted by their z-axis values. Each column corresponds to a unique run, and each row is a snapshot of the simulation at (a)–(d) 41.67, (e)–(h) 44.45, (i)–(l) 47.22, and (m)–(p) 50 hr.
Paper: Effect of Equation of State and Cutoff Density in Smoothed Particle Hydrodynamics Simulations of the Moon-forming Giant Impact
Authors: Scott D. Hull, Miki Nakajima, Natsuki Hosono, Robin M. Canup, Rene Gassmöller
Figure caption: A sample of disk particles from the 5b073S run showing numerical shocks and instability as a function of simulation time. Left to right: particle density, particle entropy, particle specific internal energy, particle temperature, and number of neighboring particles within the smoothing length H  i . The density y-axis is artificially limited to emphasize density perturbations around ρ  c  late in the simulation.
Paper: Effect of Equation of State and Cutoff Density in Smoothed Particle Hydrodynamics Simulations of the Moon-forming Giant Impact
Authors: Scott D. Hull, Miki Nakajima, Natsuki Hosono, Robin M. Canup, Rene Gassmöller
Figure caption: A sample of disk particles from the 5b073N run showing numerical shocks and instability as a function of simulation time. Left to right: particle density, particle entropy, particle specific internal energy, particle temperature, and number of neighboring particles within the smoothing length H  i . The density y-axis is artificially limited to emphasize density perturbations around ρ  c  late in the simulation.
Paper: Effect of Equation of State and Cutoff Density in Smoothed Particle Hydrodynamics Simulations of the Moon-forming Giant Impact
Authors: Scott D. Hull, Miki Nakajima, Natsuki Hosono, Robin M. Canup, Rene Gassmöller
Figure caption: Disk particles colored as a function of entropy for simulations using N-SPH M-ANEOS with b = 0.75. The axes give the x–y spatial coordinates relative to the proto-Earth’s center of mass given in increments of 104 km. Particles are sorted by their z-axis values. Each column corresponds to a unique run, and each row is a snapshot of the simulation at (a)–(e) 2.78, (f)–(j) 5.56, (k)–(o) 13.89, and (p)–(t) 50 hr.
Paper: Effect of Equation of State and Cutoff Density in Smoothed Particle Hydrodynamics Simulations of the Moon-forming Giant Impact
Authors: Scott D. Hull, Miki Nakajima, Natsuki Hosono, Robin M. Canup, Rene Gassmöller
Figure caption: Disk particles from runs with b = 0.75 and using Stewart SPH M-ANEOS colored as a function of specific entropy change (ΔS) between the displayed time in each row and ∼3 hr prior. The axes give the x–y spatial coordinates relative to the proto-Earth’s center of mass given in increments of 104 km. Particles are sorted by their z-axis values. Each column corresponds to a unique run, and each row is a snapshot of the simulation at (a)–(d) 41.67, (e)–(h) 44.45, (i)–(l) 47.22, and (m)–(p) 50 hr.
Paper: Effect of Equation of State and Cutoff Density in Smoothed Particle Hydrodynamics Simulations of the Moon-forming Giant Impact
Authors: Scott D. Hull, Miki Nakajima, Natsuki Hosono, Robin M. Canup, Rene Gassmöller
Figure caption: Disk particles colored as a function of entropy for simulations using Stewart M-ANEOS with b = 0.75. The axes give the x–y spatial coordinates relative to the proto-Earth’s center of mass given in increments of 104 km. Particles are sorted by their z-axis values. Each column corresponds to a unique run, and each row is a snapshot of the simulation at (a)–(d) 2.78, (e)–(h) 5.56, (i)–(l) 13.89, and (m)–(p) 50 hr.
Paper: The Relative Effects of Surface and Subsurface Morphology on the Deflection Efficiency of Kinetic Impactors: Implications for the DART Mission
Authors: Mallory E. DeCoster, Robert Luther, Gareth S. Collins, Kaiyi Dai, Thomas Davison, Dawn M. Graninger, Felix Kaufmann, Emma S. G. Rainey, Angela M. Stickle
Figure caption: Comparison of provenance of ejecta as a function of vertical ejection velocity (V  z ) normalized by the impact velocity (U) for (a) a half-buried boulder, (b) a fully submerged boulder, and (c) no boulder. (d) Cumulative ejected momentum as a function of normalized ejection velocity for a boulder with a 3 m diameter at various burial depths. The blue lines indicate where the boulders extended above the surface, and the green lines indicate where the boulders were buried below the surface.
Paper: The Relative Effects of Surface and Subsurface Morphology on the Deflection Efficiency of Kinetic Impactors: Implications for the DART Mission
Authors: Mallory E. DeCoster, Robert Luther, Gareth S. Collins, Kaiyi Dai, Thomas Davison, Dawn M. Graninger, Felix Kaufmann, Emma S. G. Rainey, Angela M. Stickle
Figure caption: Comparison of the 3D spherical rubble-pile and 2D rubble-pile targets. The boulder fill fraction for the 2D and 3D targets was 62% and 59%, respectively. Panel (a) shows the full 3D spherical rubble-pile; (b) shows the 3D xz cut-through with the impact point at x = 0, z = 81.5 m; (c) shows the 2D xy cut-through with the impact point at x = 0, y =  81.5 m; and (d)–(f) show the impact site and projectile geometry for the (d) 3D yz-plane, (e) 3D xz-plane, and (f) 2D simulations.
Paper: The Relative Effects of Surface and Subsurface Morphology on the Deflection Efficiency of Kinetic Impactors: Implications for the DART Mission
Authors: Mallory E. DeCoster, Robert Luther, Gareth S. Collins, Kaiyi Dai, Thomas Davison, Dawn M. Graninger, Felix Kaufmann, Emma S. G. Rainey, Angela M. Stickle
Figure caption: CTH results showing (a) the temporal profile of β−1 and (b) the cumulative ejecta mass (M ejecta) normalized by the impactor mass (m) vs. the ejecta velocity (V ejecta) normalized by the impactor velocity (u) at 130 ms postimpact. The plots show the results for homogeneous targets and four rubble-pile targets where the boulder cohesion (Y  o,b ) was held constant, the cohesion of the regolith material (Y  o,reg) was varied from 1 to 10 Pa, and the boulder size at the surface was varied from d = 1.0 to 6.0 m.
Paper: The Relative Effects of Surface and Subsurface Morphology on the Deflection Efficiency of Kinetic Impactors: Implications for the DART Mission
Authors: Mallory E. DeCoster, Robert Luther, Gareth S. Collins, Kaiyi Dai, Thomas Davison, Dawn M. Graninger, Felix Kaufmann, Emma S. G. Rainey, Angela M. Stickle
Figure caption: Schematic detailing the parameter phase space for modeling a kinetic impact for planetary defense in reference to the DART mission. The known parameters are in pink, and the unknowns are in orange. For DART, observations made before and after impact (light blue) provided constraints on the preimpact unknowns, which allowed for further constraints on impact model parameters (green). Future observations from the ESA's Hera mission (dark blue) will further constrain forthcoming impact models.
Paper: The Relative Effects of Surface and Subsurface Morphology on the Deflection Efficiency of Kinetic Impactors: Implications for the DART Mission
Authors: Mallory E. DeCoster, Robert Luther, Gareth S. Collins, Kaiyi Dai, Thomas Davison, Dawn M. Graninger, Felix Kaufmann, Emma S. G. Rainey, Angela M. Stickle
Figure caption: Initial conditions showing the different target surface and subsurface morphologies considered in the 2D CTH simulations. (a) The full rubble-pile target, (b) zoom-in of the surface from the full rubble pile with large surface boulders (diameter r = 6.0 m), (c) zoom-in of the rubble-pile surface with small surface boulders (diameter r = 1.0 m), (d) small surface boulders with a substrate core ranging from 0.88 to 15 m below the surface, and (e) a homogeneous target.
Paper: The Relative Effects of Surface and Subsurface Morphology on the Deflection Efficiency of Kinetic Impactors: Implications for the DART Mission
Authors: Mallory E. DeCoster, Robert Luther, Gareth S. Collins, Kaiyi Dai, Thomas Davison, Dawn M. Graninger, Felix Kaufmann, Emma S. G. Rainey, Angela M. Stickle
Figure caption: DART DRACO image of Dimorphos 11 s before impact; the yellow dot shows the approximate impact site, and the arrow indicates the direction of the Dimorphos +Z (north) axis. Credit: NASA/Johns Hopkins APL.
Paper: The Relative Effects of Surface and Subsurface Morphology on the Deflection Efficiency of Kinetic Impactors: Implications for the DART Mission
Authors: Mallory E. DeCoster, Robert Luther, Gareth S. Collins, Kaiyi Dai, Thomas Davison, Dawn M. Graninger, Felix Kaufmann, Emma S. G. Rainey, Angela M. Stickle
Figure caption: Relative total momentum of ejecta launched in the first 2 s postimpact as a function of boulder size and normalized position (elevation of the top of the boulder relative to the surface, z, divided by boulder radius, r). The antiarmoring regime is above the black horizontal line indicative of β−1 with no boulder present, and the armoring regime falls below this line.
Paper: The Relative Effects of Surface and Subsurface Morphology on the Deflection Efficiency of Kinetic Impactors: Implications for the DART Mission
Authors: Mallory E. DeCoster, Robert Luther, Gareth S. Collins, Kaiyi Dai, Thomas Davison, Dawn M. Graninger, Felix Kaufmann, Emma S. G. Rainey, Angela M. Stickle
Figure caption: Initial conditions showing the different target surface and subsurface morphologies considered in the iSALE-2D simulations for (a) the full rubble-pile target, (b) the rubble-pile target with a substrate core layer 5 m below the surface, and (c) the rubble-pile target with a substrate core layer 1 m below the surface. The left side of each image plots the damage, and the right side plots the material density.
Paper: Organic Hazes as a Source of Life’s Building Blocks to Warm Little Ponds on the Hadean Earth
Authors: Ben K. D. Pearce, Sarah M. Hörst, Joshua A. Sebree, Chao He
Figure caption: Calibration curves calculated for the seven nucleobases. Equations of the lines of best fit and χ 2 values are added to the legend. Uncertainties are the shaded regions calculated as the variance from a model linearly connecting each data point. Peak areas are added for the (a) 5% CH4 haze particles, (b) 0.5% CH4 haze particles, and (c) heated 5% CH4 haze particles. The uracil data point for the 7-day heated experiment is colored in peach and falls directly on top of the data point for the 1-day heated experiment.
Paper: Organic Hazes as a Source of Life’s Building Blocks to Warm Little Ponds on the Hadean Earth
Authors: Ben K. D. Pearce, Sarah M. Hörst, Joshua A. Sebree, Chao He
Figure caption: GC/MS and GC/MS/MS chromatograms for the nucleobase standard, followed by two GC/MS runs of methanol, followed by a GC/MS/MS run of an MTBSTFA derivatizer. Nucleobase peaks do not show up in the methanol runs that were run after the nucleobase standard, but they do show up when MTBSFTA is run through the inlet, suggesting that underivatized nucleobases stick around in the inlet from the high-concentration standard runs.