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: Median values for particle sphericity (top), elongation (middle), and ECD (bottom) for the 63–125 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: LHS-1 (left) and LMS-1 (right) samples after 1, 3, and 6 months of freezing compared to unaltered (dry) simulant. Intermediate-infrared spectra are normalized to 2.55 μm and are offset on the y-axis for clarity.
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: LHS-1 (left) and LMS-1 (right) samples after 1, 3, and 6 months of freezing compared to unaltered (dry) simulant. SWIR spectra are normalized to 2.4 μm and are offset on the y-axis for clarity.
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 >250 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 63–125 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: Median values for particle sphericity (top), elongation (middle), and ECD (bottom) for the 125–250 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 >250 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: Median values for particle sphericity (top), elongation (middle), and ECD (bottom) for the 125–250 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: 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, not including the entropy gain associated with orbital circularization, in contrast with the companion Figure 5. The top row corresponds to b = 0.73 simulations, and the bottom row corresponds to b = 0.75 simulations. 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.
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: Energy conservation for simulations with b = 0.75. FDPS SPH conserves energy within ∼1%, showing that the numerical issues associated with small values of ρ  c  do not violate energy conservation beyond typical numerical noise in SPH. (a) Mass in the disk. (b) Total specific energy in the disk. Some variance is associated with the changing mass of the disk as a function of time. (c) Total specific energy of the entire simulation, including the proto-Earth, disk, and escaping particles.
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: Energy conservation for simulations with b = 0.73. FDPS SPH conserves energy within ∼1%, showing that the numerical issues associated with small values of ρ  c  do not violate energy conservation beyond typical numerical noise in SPH. (a) Mass in the disk. (b) Total specific energy in the disk. Some variance is associated with the changing mass of the disk as a function of time. (c) Total specific energy of the entire simulation, including the proto-Earth, disk, and escaping particles.
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 = 0.75 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 by 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)–(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: Time evolution of the disk for simulations with impact parameter b = 0.73. This figure differs from Figure 3 in that it includes runs with ρ  c  = 100 kg m−3. 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 corresponds 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.
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 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: 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)–(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: Fraction of final disk particles with densities equal to ρ  c  as a function of simulated time. Line colors correspond to the value of ρ  c  set in the simulation, where solid lines are simulations using Stewart M-ANEOS, and dashed lines are simulations using N-SPH M-ANEOS. The dotted lines correspond to simulation 5b073S-high in panel (a) and 2000b075N-low in panel (b). (a) Runs with b = 0.73. (b) Runs with b = 0.75.
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: Density vs. pressure for disk particles at 50 simulated hr. Lower values of ρ  c  tend to be capped at slightly lower pressures than those at high ρ  c . (a) and (b) Simulations with b = 0.73. (c) and (d) Simulations with b = 0.75. The left column corresponds to simulations using Stewart M-ANEOS, and the right column corresponds to simulations using N-SPH M-ANEOS.
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 = 0.73. 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. 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 colored as a function of temperature for simulations using Stewart M-ANEOS with 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. 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 colored as a function of pressure for simulations using Stewart M-ANEOS with 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. 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 colored as a function of pressure 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: Companion figure to Figure 3 for simulations with b = 0.73, but the entropy gain and related increase in VMF associated with orbital circularization of the disk are not included in panels (a) and (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: Companion figure to Figure 4 for simulations with b = 0.75, but the entropy gain and related increase in VMF associated with orbital circularization of the disk are not included in panels (a) and (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: Disk particles colored as a function of pressure 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: 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 = 0.73. 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. 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 colored as a function of pressure for simulations using N-SPH M-ANEOS with 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. 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:  β−1 vs. the normalized regolith layer thickness, where h was the thickness of the regolith layer on top of the core, and a was the radius of the center sphere of the projectile (35.3 cm). CTH results were plotted at 130 ms (filled symbols), and iSALE results were plotted as open symbols 4 s postimpact. Note that the vastly different timescales between CTH (130 ms) and iSALE (4 s) means the CTH simulations had not evolved to a “final” crater; therefore, comparisons between the data should be avoided.
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 (top) β−1 and (bottom) the cumulative normalized ejecta mass vs. the normalized ejecta velocity for the 2DC rubble-pile with small surface boulders to the 3DR rubble-pile where the cohesion strengths of the boulders and regolith were set to Y  o,b  = 1 MPa and Y  o,reg = 1 Pa, respectively.
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: Temporal evolution of β−1 for simulations with varying subsurface morphology performed in CTH (top) and iSALE (bottom). The shallowest iSALE simulation (blue line) had a core layer placed 1 m below the target surface rather than 0.88 m below the surface (which was the shallowest layer modeled in CTH). Note the vastly different timescales between CTH (150 ms) and iSALE (4 s). The difference in timescale means the CTH simulations had not evolved to a “final” crater.
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: The cumulative ejecta mass (M ejecta) normalized by the impactor mass (m) vs. the ejecta velocity (V ejecta) normalized by the impactor velocity (u) separated by the boulder (dashed) and regolith (dotted) contributions to the ejecta at 130 ms.
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: Crater width and depth metrics. CTH data are plotted as filled symbols at 130 ms postimpact, and iSALE data are plotted as open symbols at 4 s postimpact. See Tables B1 and B3 for crater values. Note that the vastly different timescales between CTH (130 ms) and iSALE (4 s) means the CTH simulations had not evolved to a “final” crater; therefore, comparisons between the data should be avoided.
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 right half of the rubble-pile setup in iSALE. The gray scale denotes the materials, with dark gray for the projectile, medium gray for the matrix material, and light gray for the boulders.
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: 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 for CTH (left) and 4 s postimpact for iSALE (right).
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: Plot of the transient crater at 130 ms postimpact for the CTH simulations. Table B2 contains tabulated values, and Figure B2 shows illustrations of the transient craters.
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: The damage profile at 130 ms postimpact for the 2DC (left) and 3DR (middle and right) rubble-pile simulations.
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: (a) Model pond concentrations of adenine from organic haze particle deposition at 4.4 bya for a 0.5% methane atmosphere (this work) compared with meteoritic delivery (Pearce et al. 2017), IDP delivery (Pearce et al. 2017), and in situ production from atmospherically sourced HCN for two different periods during the Hadean (Pearce et al. 2022b). Concentrations are calculated using a comprehensive sources-and-sinks pond model originally developed in Pearce et al. (2017) that has a ∼6-month wet cycle and a ∼6-month dry cycle; the one exception is the “Meteorites—no UV” model, which never dries up and for which UV is never turned on owing to water shielding. (b) Maximum pond concentrations of six other nucleobases from organic haze particle deposition at 4.4 bya (this work). Asterisks indicate that the values are calculated using the high-methane (5%) CH4 experimental haze particle concentration, as xanthine and guanine were not detected in the low-methane (0.5%) organic haze particles (see Table 1).
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: Nucleobase abundances measured in the four organic haze particle samples in this study. Nucleobase order is from lowest to highest molar mass. Units are μg biomolecule/g haze particles, or ppm.