adsabs/AstroCLIMB huggingface dataset:
Paper: Estimate of Water and Hydroxyl Abundance on Asteroid (16) Psyche from JWST Data
Authors: Stephanie G. Jarmak, Tracy M. Becker, Charles E. Woodward, Casey I. Honniball, Andrew S. Rivkin, Margaret M. McAdam, Zoe A. Landsman, Saverio Cambioni, Thomas G. Müller, Driss Takir, Kurt D. Retherford, Anicia Arredondo, Linda T. Elkins-Tanton
Figure caption: Relative normalized reflectance spectrum of Psyche near 3 μm. Top: observation 1. Bottom: observation 2.
Paper: Estimate of Water and Hydroxyl Abundance on Asteroid (16) Psyche from JWST Data
Authors: Stephanie G. Jarmak, Tracy M. Becker, Charles E. Woodward, Casey I. Honniball, Andrew S. Rivkin, Margaret M. McAdam, Zoe A. Landsman, Saverio Cambioni, Thomas G. Müller, Driss Takir, Kurt D. Retherford, Anicia Arredondo, Linda T. Elkins-Tanton
Figure caption: Relative normalized reflectance spectrum of Psyche near 3 μm for NIRSpec observation 1 (black) observation 2 (red) and IRTF from Takir et al. (2017) (blue).
Paper: Estimate of Water and Hydroxyl Abundance on Asteroid (16) Psyche from JWST Data
Authors: Stephanie G. Jarmak, Tracy M. Becker, Charles E. Woodward, Casey I. Honniball, Andrew S. Rivkin, Margaret M. McAdam, Zoe A. Landsman, Saverio Cambioni, Thomas G. Müller, Driss Takir, Kurt D. Retherford, Anicia Arredondo, Linda T. Elkins-Tanton
Figure caption: Relative normalized reflectance spectrum of Psyche near 1.28 μm. Binned spectra are binned to 1 nm.
Paper: Mid-infrared Measurements of Ion-irradiated Carbonaceous Meteorites: How to Better Detect Space Weathering Effects
Authors: C. Lantz, T. Nakamura, D. Baklouti, R. Brunetto, E. Henault, S. Kobayashi, O. Mivumbi, Z. Djouadi, E. Quirico, M. Zolensky, T. Hiroi
Figure caption: MIR confocal reflectance spectra of the meteorites. Spectra were acquired at SOLEIL (France) with the Agilent/FPA instrument (imaging) and averaged on a large area of the samples. In the left column (no or less hydrous compounds), from top to bottom: CM Murchison, CM QUE97990, CR EET92159, a ureilite piece of Almahata Sitta, and CK NWA5515-1498. In the right column (more hydrated minerals), from top to bottom: CM MET00639, CM MET01072, CM MET01070, and two different samples of CY Y980115. Sample names are indexed with c for chip and p for pellet. Nonirradiated area spectra are in black, while irradiated ones are in color: 4 keV in gray, 15 keV in brown, 20 keV in yellow, and 40 keV in red. Spectra are scaled to unity at the strongest peak to facilitate the comparison and are shifted along the y-axis for clarity. The marks on the CK, CR, and CM MET01070 spectra are discussed in Section 3.2.
Paper: Mid-infrared Measurements of Ion-irradiated Carbonaceous Meteorites: How to Better Detect Space Weathering Effects
Authors: C. Lantz, T. Nakamura, D. Baklouti, R. Brunetto, E. Henault, S. Kobayashi, O. Mivumbi, Z. Djouadi, E. Quirico, M. Zolensky, T. Hiroi
Figure caption: Evolution of the main band position vs. the width at 75% band maximum upon irradiation for all the studied chondrites. Filled symbols are before irradiation, and open ones are after, with color code as follows: 40 keV (red), 20 keV (yellow), 15 keV (brown), and 4 keV (gray). The inset plot is at the same scale as the main plot. We removed the CY sample, as its width is biased by the presence of two distinct bands, and the ureilite, as we do not have access to the value of the width at 75% height, preventing a straightforward comparison with the other samples. The dashed arrow defines a vector of aqueous alteration scheme among CMs (the three groups are circled), explained in Section 4.2.
Paper: Mid-infrared Measurements of Ion-irradiated Carbonaceous Meteorites: How to Better Detect Space Weathering Effects
Authors: C. Lantz, T. Nakamura, D. Baklouti, R. Brunetto, E. Henault, S. Kobayashi, O. Mivumbi, Z. Djouadi, E. Quirico, M. Zolensky, T. Hiroi
Figure caption: Shift values measured on all meteorites irradiated by our team using He+ ions to simulate the SpWe solar wind component at different energies. The shift is determined by subtracting the position of the main band (maximum on the spectra; top panel) or Christiansen feature (bottom panel) before and after irradiation. Errors are within the symbol size. We grouped meteorites according to their classes: green triangles for anhydrous CCs, sand squares for pyroxene-rich samples, purple diamonds for the most hydrated meteorites, and blue hexagons for all CMs. We only considered the first peak for the Y980115 samples (both chip and pellet). The meteorites Allende, Lancé, and Frontier Mountain 95002 are abbreviated as “A, L, FM.”
Paper: Mid-infrared Measurements of Ion-irradiated Carbonaceous Meteorites: How to Better Detect Space Weathering Effects
Authors: C. Lantz, T. Nakamura, D. Baklouti, R. Brunetto, E. Henault, S. Kobayashi, O. Mivumbi, Z. Djouadi, E. Quirico, M. Zolensky, T. Hiroi
Figure caption: Comparison of shift values (determined on the main band in the MIR range) between data acquired at SOLEIL (microscope; plus signs) and at Tohoku University (bidirectional; crosses) on the same samples: CMs Murchison (irradiated at 4 keV; gray line) and MET01072 (20 keV; yellow), and CY Y980115 as a chip (20 keV; purple). Corresponding spectra are shown in Figure 1 (SOLEIL) and Figure A1 (Tohoku Univ.). The values presented here for the chip of Y980115 were obtained on the first peak around 980 cm−1.
Paper: Mid-infrared Measurements of Ion-irradiated Carbonaceous Meteorites: How to Better Detect Space Weathering Effects
Authors: C. Lantz, T. Nakamura, D. Baklouti, R. Brunetto, E. Henault, S. Kobayashi, O. Mivumbi, Z. Djouadi, E. Quirico, M. Zolensky, T. Hiroi
Figure caption: Evolution of the main band position vs. the difference between the Christiansen feature and main band position in the MIR upon irradiation. Filled symbols are before irradiation, and open ones are after, with the same color code as in Figure 4 (40 keV, red; 20 keV, yellow; 15 keV, brown; 4 keV, gray). The inset plot is at the same scale as the main plot. The meteorites Allende, Lancé, and Frontier Mountain 95002 are abbreviated as “A, L, FM.” We added points for Ryugu (black diamond) and Bennu (star). Dashed arrows define the vectors of aqueous alteration (blue, as in Figure 4) and SpWe (red).
Paper: Mid-infrared Measurements of Ion-irradiated Carbonaceous Meteorites: How to Better Detect Space Weathering Effects
Authors: C. Lantz, T. Nakamura, D. Baklouti, R. Brunetto, E. Henault, S. Kobayashi, O. Mivumbi, Z. Djouadi, E. Quirico, M. Zolensky, T. Hiroi
Figure caption: MIR bidirectional reflectance spectra of the meteorites CM Murchison (top), CM MET01072 (middle), and CY Y950115 as a chip (bottom) before (black) and after (colored lines) ion irradiation. Spectra are acquired at Tohoku University (Japan) with the Bruker Vertex instrument (solid lines) and at SOLEIL (France) with the Agilent/FPA instrument (dashed lines). Spectra are scaled to unity at the strongest peak to facilitate the comparison and are shifted along the y-axis for clarity.
Paper: Mid-infrared Measurements of Ion-irradiated Carbonaceous Meteorites: How to Better Detect Space Weathering Effects
Authors: C. Lantz, T. Nakamura, D. Baklouti, R. Brunetto, E. Henault, S. Kobayashi, O. Mivumbi, Z. Djouadi, E. Quirico, M. Zolensky, T. Hiroi
Figure caption: MIR confocal reflectance spectra of the meteorites CK NWA5515-1498 and CM MET01070 acquired on the pellet before ion irradiation exposure. The whole surface has been measured to produce a large area average spectrum (black). Two smaller areas (half pellet; blue and green lines) were also averaged to be compared afterward to the 15 and 40 keV irradiated zones. Spectra are scaled to unity at the strongest peak to facilitate the comparison and are shifted along the y-axis for clarity.
Paper: Mid-infrared Measurements of Ion-irradiated Carbonaceous Meteorites: How to Better Detect Space Weathering Effects
Authors: C. Lantz, T. Nakamura, D. Baklouti, R. Brunetto, E. Henault, S. Kobayashi, O. Mivumbi, Z. Djouadi, E. Quirico, M. Zolensky, T. Hiroi
Figure caption: MIR confocal (dashed lines) and bidirectional (solid lines) reflectance spectra of the meteorite CM Murchison before (black) and after (gray) ion irradiation. Spectra are scaled to unity at the strongest peak to facilitate the comparison and are shifted along the y-axis for clarity.
Paper: LunaIcy: Exploring Europa’s Icy Surface Microstructure through Multiphysics Simulations
Authors: Cyril Mergny, Frédéric Schmidt
Figure caption: (Left) Grain/bond pattern repeated periodically along the ﹩\hat{x}﹩-axis. Each grain is connected to its neighbors by top and bottom bonds. (Right) Schematic representation of the grain/bond geometry. Due to the symmetry along two axes represented here, our model only needs to represent a quarter of the total grain/bond volume. The red line follows the curvature of the vapor/ice interface along the ﹩\hat{x}﹩-axis, while the blue line follows the curvature in the ﹩\hat{y}\hat{z}﹩-plane.
Paper: LunaIcy: Exploring Europa’s Icy Surface Microstructure through Multiphysics Simulations
Authors: Cyril Mergny, Frédéric Schmidt
Figure caption: (Left) Evolution of grain radius (top) and bond radius (bottom) over time at T = 150 K for different bond-per-grain scenarios (1, 2, and 6). (Right) Evolution of gas pressure P gas over time for different bond-per-grain scenarios (1, 2, and 6). The gray dashed line represents the saturated vapor pressure over a flat surface at T = 150 K.
Paper: LunaIcy: Exploring Europa’s Icy Surface Microstructure through Multiphysics Simulations
Authors: Cyril Mergny, Frédéric Schmidt
Figure caption: Evolution of the relative bond radius r b/r g in the P. V. Hobbs & B. J. Mason (1964) experiments (crosses) for different grain sizes at a constant temperature of −3°C. With a single value of the sticking coefficient α = 0.03, the model (lines) can accurately compute the relative bond radius evolution for the three experiments.
Paper: LunaIcy: Exploring Europa’s Icy Surface Microstructure through Multiphysics Simulations
Authors: Cyril Mergny, Frédéric Schmidt
Figure caption: Sintering timescales for different temperatures and initial grain radii, computed based on simulations with two bonds per grain. The timescale is determined when the bond radius reaches half of the grain radius.
Paper: LunaIcy: Exploring Europa’s Icy Surface Microstructure through Multiphysics Simulations
Authors: Cyril Mergny, Frédéric Schmidt
Figure caption: Schematic representation of diffusion by vapor transport. The grain and bond surfaces exchange matter with the surrounding gas in the pore space.
Paper: Near-infrared Spectral Homogeneity of the Didymos System Before and After the DART Impact 
Authors: Simone Ieva, E. Mazzotta Epifani, E. Dotto, V. Petropoulou, J. D. P. Deshapriya, P. H. Hasselmann, G. Poggiali, D. Perna, M. Dall'Ora, A. Lucchetti, M. Pajola, S. L. Ivanovski, A. Rossi, J. R. Brucato, P. Palumbo, V. Della Corte, A. Zinzi, C. A. Thomas, J. de León, T. Kareta, N. Moskovitz, N. L. Chabot, A. S. Rivkin, M. Amoroso, I. Bertini, A. Capannolo, S. Caporali, M. Ceresoli, G. Cremonese, I. Gai, L. Gomez-Casajus, E. Gramigna, G. Impresario, R. Lasagni Manghi, M. Lavagna, M. Lombardo, D. Modenini, S. Pirrotta, P. Tortora, F. Tusberti, M. Zannoni, G. Zanotti
Figure caption: Molar content of Fa/Fs for all the average spectra of Didymos observed each night and the ejecta tail (observed on November 3), overimposed on a collection of the same values for H- (x), L- (circles), and LL-ordinary chondrites (triangles), retrieved from T. Nakamura et al. (2011). Didymos data are in agreement with L-ordinary chondrites, although ejecta data show a slightly lower value for Fa/Fs. The average errors for Fs and Fa are originally inferred in T. L. Dunn et al. (2010) and correspond to ±1.3 mol% for Fa, and ±1.4 mol% for Fs.
Paper: Near-infrared Spectral Homogeneity of the Didymos System Before and After the DART Impact 
Authors: Simone Ieva, E. Mazzotta Epifani, E. Dotto, V. Petropoulou, J. D. P. Deshapriya, P. H. Hasselmann, G. Poggiali, D. Perna, M. Dall'Ora, A. Lucchetti, M. Pajola, S. L. Ivanovski, A. Rossi, J. R. Brucato, P. Palumbo, V. Della Corte, A. Zinzi, C. A. Thomas, J. de León, T. Kareta, N. Moskovitz, N. L. Chabot, A. S. Rivkin, M. Amoroso, I. Bertini, A. Capannolo, S. Caporali, M. Ceresoli, G. Cremonese, I. Gai, L. Gomez-Casajus, E. Gramigna, G. Impresario, R. Lasagni Manghi, M. Lavagna, M. Lombardo, D. Modenini, S. Pirrotta, P. Tortora, F. Tusberti, M. Zannoni, G. Zanotti
Figure caption: Averaged spectra taken during November 3 of main body (Didymos + Dimorphos) in red and the ejecta tail in blue.
Paper: Contribution of the Moon-forming Impactor to the Volatile Inventory in the Bulk Silicate Earth
Authors: Damanveer S. Grewal, Yoshinori Miyazaki, Nicole X. Nie
Figure caption: Illustration depicting the delivery of H–C–N–S to the proto-Earth exclusively by the MFI in cases where the impactor (a) retained or (b) lost its MO-degassed atmosphere before the giant impact. Post-impact, the inventory of H–C–N–S in the BSE is controlled by the exchange of these volatiles between the molten fraction of the mantle, the BSI (= mantle ± MO-degassed atmosphere), and the reequilibrating fraction of the impactor’s core (f). Note that the BSp-E is H–C–N–S-free and the BSI and the impactor’s core are H–C–N–S-bearing.
Paper: Contribution of the Moon-forming Impactor to the Volatile Inventory in the Bulk Silicate Earth
Authors: Damanveer S. Grewal, Yoshinori Miyazaki, Nicole X. Nie
Figure caption: H–C–N–S distribution between the core, MO, and MO-degassed atmosphere of the MFI for the f = 0.1 and M MO = 0.5M BSE scenario. The MO-degassed atmosphere is the major N reservoir, but it also contains a substantial amount of C and H, whereas the impactor’s core is the major H, C, and S reservoir. Similar distribution patterns are applicable for the other scenarios explored in this study.
Paper: Contribution of the Moon-forming Impactor to the Volatile Inventory in the Bulk Silicate Earth
Authors: Damanveer S. Grewal, Yoshinori Miyazaki, Nicole X. Nie
Figure caption: Comparison between the S content in the impactor’s core, its C content predicted by ﹩{D}_{{\rm{C}}}^{\mathrm{metal}/\mathrm{silicate}}﹩, and its graphite-saturated C solubility limit (Csolubility) as a function of the extent of its reequilibration with the post-impact MO (f). In the case of the impactor retaining its MO-degassed atmosphere prior to the Moon-forming giant impact, C content in the core predicted by ﹩{D}_{{\rm{C}}}^{\mathrm{metal}/\mathrm{silicate}}﹩ is generally lower than Csolubility, except for a narrow range of f . This means that the MFI’s core was almost always C undersaturated for the atmospheric retention case, whereas for the case of atmospheric loss before the impact, the impactor’s core is C saturated for almost all values of f.
Paper: Contribution of the Moon-forming Impactor to the Volatile Inventory in the Bulk Silicate Earth
Authors: Damanveer S. Grewal, Yoshinori Miyazaki, Nicole X. Nie
Figure caption: Required inventory of H–C–N–S in the MFI to establish the abundances of these elements in the BSE in cases where the impactor (a) retained or (b) lost its MO-degassed atmosphere before the giant impact. In panel (a) MFI is required to contain subchondritic content of H, C (except for ECs), N, and S, whereas in panel (b) the required inventories of N and C fall between those of ECs and CIs/CMs and the required inventories of H and S are lower than those of chondrites (except for ECs, which are almost H-free). H–C–N–S inventories in the BSE (Hirschmann 2018; Marty et al. 2020) and in EC, CM, and CI chondrites (Alexander 2022) are also plotted for comparison.
Paper: Contribution of the Moon-forming Impactor to the Volatile Inventory in the Bulk Silicate Earth
Authors: Damanveer S. Grewal, Yoshinori Miyazaki, Nicole X. Nie
Figure caption: The total mass of an element participating in atmosphere–MO–core equilibration in the post–giant impact Earth (﹩{{m}}_{{i}}^{\mathrm{total}}﹩) normalized to the mass of that element in the BSE (﹩{{m}}_{{i}}^{\mathrm{BSE}}﹩). Within the realistic range of f values explored in this study (f = 0.05–0.2), ﹩{{m}}_{{i}}^{\mathrm{total}}﹩ values lie in a narrow range, whereas for f = 0.5, ﹩{{m}}_{{i}}^{\mathrm{total}}﹩ values for H and C are substantially higher.
Paper: Estimate of Water and Hydroxyl Abundance on Asteroid (16) Psyche from JWST Data
Authors: Stephanie G. Jarmak, Tracy M. Becker, Charles E. Woodward, Casey I. Honniball, Andrew S. Rivkin, Margaret M. McAdam, Zoe A. Landsman, Saverio Cambioni, Thomas G. Müller, Driss Takir, Kurt D. Retherford, Anicia Arredondo, Linda T. Elkins-Tanton
Figure caption: Spectral energy distribution of Psyche obtained from NIRSpec and MIRI instruments prior to removal of the solar spectrum and thermal emission to create a reflectance spectrum. Average resolution is ∼0.001 μm for the NIRSpec observations and ∼0.002 μm for the MIRI observations, corresponding to a factor of ∼25x (AKARI) and ∼60x (Spitzer) increased resolution compared to previous space telescope infrared observations of Psyche. For each instrument, observation 1 is in black and observation 2 is in red.
Paper: Contribution of the Moon-forming Impactor to the Volatile Inventory in the Bulk Silicate Earth
Authors: Damanveer S. Grewal, Yoshinori Miyazaki, Nicole X. Nie
Figure caption: Comparison of the MFI’s required H–C–N–S inventory to its accretion of 40% CI/CM-chondrite-like materials for the case where it lost its MO-degassed atmosphere before the giant impact. An MFI composed of 40% CI/CM-chondrite-like materials has the potential to deliver the entire required inventory of H and S and up to half of the required C, whereas its potential to deliver N depends on f values, where higher values indicate a greater potential contribution.
Paper: Estimate of Water and Hydroxyl Abundance on Asteroid (16) Psyche from JWST Data
Authors: Stephanie G. Jarmak, Tracy M. Becker, Charles E. Woodward, Casey I. Honniball, Andrew S. Rivkin, Margaret M. McAdam, Zoe A. Landsman, Saverio Cambioni, Thomas G. Müller, Driss Takir, Kurt D. Retherford, Anicia Arredondo, Linda T. Elkins-Tanton
Figure caption: Orientation of Psyche at the time of observations. Top: NIRSpec observations. Bottom: MIRI observations. Each observation is nearly pole-on (aspect angle 24°) viewing the north pole. These figures were produced in Pyvista (Sullivan & Kaszynski 2019) using the shape model from Shepard et al. (2021).
Paper: Detectability Simulations of a Near-infrared Surface Biosignature on Proxima Centauri b with Future Space Observatories
Authors: Connor O. Metz, Nancy Y. Kiang, Geronimo L. Villanueva, M. N. Parenteau, Vincent Kofman
Figure caption: “Hyperrealistic” RGB images of Control at a phase of 40°, generated with PSG GlobES. Top left: true-color image without BVLO. Proxima b appears orange because Proxima Centauri is a cool star that emits mostly red light in the visible. In this image, the darkest regions on the planet are oceans, and the lighter regions are ice or clouds. To identify clouds, compare with top right. Top right: the cloud cover fraction, with high numbers indicating grid cells mostly covered with clouds. Bottom right: false-color image of Control with BVLO. The BVLOs appear purple because the Qy feature strongly absorbs in the green channel at 1 μm. Bottom left: same as top left but with BVLOs added (﹩{A}_{max}=1﹩). The BVLOs fill in the open-water regions. To easily see regions of BVLO coverage, compare with purple regions in bottom right.
Paper: Impacts on Ocean Worlds Are Sufficiently Frequent and Energetic to Be of Astrobiological Importance
Authors: Shannon M. MacKenzie, Alexandra Pontefract, R. Terik Daly, Jacob J. Buffo, Gordon R. Osinski, Christopher J. Cline, Mark J. Cintala, Kathleen L. Craft, Mallory J. Kinczyk, Joshua Hedgepeth, Sarah M. Hörst, Abel Méndez, Ben K. D. Pearce, Angela M. Stickle, Steven D. Vance
Figure caption: Impact velocities and first contact pressures relevant to OW for ice (solid, black) and basalt (dashed, gray) projectiles into ice targets at a representative span of impact angles between 15° and 75°. Shock studies of biota (green) or biologically relevant molecules (black) shown along the y-axes; impactors in the inner solar system shown at the top for context. Vertical orange, teal, and magenta bars indicate the average impact velocity of heliocentric impactors calculated by Zahnle et al. (2008); Nesvorný et al. (2023)a; Martins et al. (2013)b; Goldman et al. (2010)c; Blank et al. (2001)d; Furukawa et al. (2015)e; Horneck et al. (2001); Burchell (2007); Stöffler et al. (2007); Burchell et al. (2014)f; Traspas & Burchell 2021                      g; O’Brien & Sykes (2011)h; Le Feuvre & Wieczorek (2008).
Paper: Impacts on Ocean Worlds Are Sufficiently Frequent and Energetic to Be of Astrobiological Importance
Authors: Shannon M. MacKenzie, Alexandra Pontefract, R. Terik Daly, Jacob J. Buffo, Gordon R. Osinski, Christopher J. Cline, Mark J. Cintala, Kathleen L. Craft, Mallory J. Kinczyk, Joshua Hedgepeth, Sarah M. Hörst, Abel Méndez, Ben K. D. Pearce, Angela M. Stickle, Steven D. Vance
Figure caption: (a) Cumulative cratering rates assuming heliocentric, cometary impactors from Zahnle et al. (2003). Observed crater diameter ranges from the distribution of observed craters on Europa, Titan, and Enceladus. (b) Initial depth of melt and freezing timescales calculated as in Kraus et al. (2011) for impactors of differing densities.
Paper: Impacts on Ocean Worlds Are Sufficiently Frequent and Energetic to Be of Astrobiological Importance
Authors: Shannon M. MacKenzie, Alexandra Pontefract, R. Terik Daly, Jacob J. Buffo, Gordon R. Osinski, Christopher J. Cline, Mark J. Cintala, Kathleen L. Craft, Mallory J. Kinczyk, Joshua Hedgepeth, Sarah M. Hörst, Abel Méndez, Ben K. D. Pearce, Angela M. Stickle, Steven D. Vance
Figure caption: Total melt production for observed craters on Enceladus (cyan) and Titan (orange), binned by observed crater diameter. Impactor velocities (v  i ) were assigned to span expected values at each body (i.e., the width of boxes in Figure 1) based on the crater diameter bin; darker colors represent the maximum velocity while lighter colors represent the minimum. (The necessary catalogs of impact craters do not yet exist to conduct this analysis for Europa.).
Paper: Crater Equilibrium State Characterization given Crater Production from a Single Power Law
Authors: Masatoshi Hirabayashi, Caleb I. Fassett, Emily S. Costello, David A. Minton
Figure caption: Comparison with the reported crater distribution in a heavily cratered area (W. K. Hartmann 1984) and the model solutions with α = 1, β = 0, γ 1 = 10,000, and γ 2 = 0, where γ 1 is set to mimic the theoretical condition, γ 1 → ∞. The blue line shows the reported crater distribution (W. K. Hartmann 1984). The yellow line gives a full solution with η = 1.83, while the green line is the analytical solution with the same condition. The black dashed line represents an example of the class I crater equilibrium state with η = 2.45 and β = −0.17 while keeping α = 1, γ 1 = 10,000, and γ 2 = 0.0.
Paper: Crater Equilibrium State Characterization given Crater Production from a Single Power Law
Authors: Masatoshi Hirabayashi, Caleb I. Fassett, Emily S. Costello, David A. Minton
Figure caption: Modeled class IV crater equilibrium CSFDs. The full solution is in blue, while the analytical models are given in orange and green. The orange line is supposed to be the analytical model when craters are large, while the green line is for small craters. Each panel gives different parameter settings. (a) α = 1.0, γ 1 = 0.0, γ 2 = 0.5, η = 2.3, β = 0.0; (b) α = 1.0, γ 1 = 0.0, γ 2 = 2.0, η = 2.3, β = 0.0; (c) α = 1.0, γ 1 = 0.2, γ 2 = 0.5, η = 2.3, β = 0.0; and (d) α = 1.0, γ 1 = 0.0, γ 2 = 0.5, η = 2.3, β = 0.5. The black dashed vertical lines indicate the locations of D tr given by Equation (27).
Paper: Crater Equilibrium State Characterization given Crater Production from a Single Power Law
Authors: Masatoshi Hirabayashi, Caleb I. Fassett, Emily S. Costello, David A. Minton
Figure caption: Variations in k as a function of ﹩\check{D}/D﹩, given in Equation (12). The x-axis gives ﹩\check{D}/D﹩, while the y-axis shows k. The unity value along the x-axis means ﹩\check{D}/D=1﹩.