adsabs/AstroCLIMB huggingface dataset:
Paper: Maps of Solar Wind Plasma Precipitation onto Mercury’s Surface: A Geographical Perspective
Authors: Federico Lavorenti, Elizabeth A. Jensen, Sae Aizawa, Francesco Califano, Mario D'Amore, Deborah Domingue, Pierre Henri, Simon Lindsay, Jim M. Raines, Daniel Wolf Savin
Figure caption: Magnetic field lines in the meridian plane (the X–Z plane in the Mercury-centered solar orbital coordinate system) for our two simulations. The left (right) panel corresponds to a simulation with a northward (southward) IMF. Blue lines correspond to magnetic field lines not connected to the planet (i.e., solar wind field lines). Red lines correspond to magnetic field lines with one end connected to the planet (i.e., magnetospheric open field lines). Green lines correspond to magnetic field lines with both ends connected to the planet (i.e., magnetospheric closed field lines). The horizontal gray lines indicate the geographic equator of the planet.
Paper: Maps of Solar Wind Plasma Precipitation onto Mercury’s Surface: A Geographical Perspective
Authors: Federico Lavorenti, Elizabeth A. Jensen, Sae Aizawa, Francesco Califano, Mario D'Amore, Deborah Domingue, Pierre Henri, Simon Lindsay, Jim M. Raines, Daniel Wolf Savin
Figure caption: Same as Figure 3, but for electron precipitation.
Paper: Maps of Solar Wind Plasma Precipitation onto Mercury’s Surface: A Geographical Perspective
Authors: Federico Lavorenti, Elizabeth A. Jensen, Sae Aizawa, Francesco Califano, Mario D'Amore, Deborah Domingue, Pierre Henri, Simon Lindsay, Jim M. Raines, Daniel Wolf Savin
Figure caption: Sketch of plasma precipitation onto Mercury’s surface over orbital time. The 3:2 spin–orbit resonance is responsible for increasing the cusp precipitation at the hot poles (red dashed lines) compared to the warm poles (blue dashed lines). The yellow sectors in the right panel approximately indicate the accumulation of plasma at the cusp over time.
Paper: Two Seismic Events from InSight Confirmed as New Impacts on Mars
Authors: Ingrid J. Daubar, Benjamin A. Fernando, Raphaël F. Garcia, Peter M. Grindrod, Géraldine Zenhäusern, Natalia Wójcicka, Nicholas A. Teanby, Simon C. Stähler, Liliya Posiolova, Anna C. Horleston, Gareth S. Collins, Constantinos Charalambous, John Clinton, Maria E. Banks, Marouchka Froment, Philippe Lognonné, Mark Panning, W. Bruce Banerdt
Figure caption: Constraining and confirmation images for InSight seismic events (A) S1034a and (B) S1160. (A) Cutouts of CTX images (top left) N22_071075_1861_XN_06N225W (2021 September 24) and (top right) U03_072288_1821_XI_02N224W (2021 December 28) constraining the formation of a new darkened area. (bottom) Cutout of HiRISE enhanced color RDR image ESP_075901_1840 of new impact crater corresponding to InSight seismic event S1034a. (B) Cutouts of CTX images (top left) U05_073066_1852_XI_05N225W (2022 February 26) and (top right) U12_075756_1829_XN_02N225W (2022 September 24) constraining the formation of a new darkened area. (bottom) Cutout of HiRISE enhanced color RDR image ESP_076877_1850 of new impact crater cluster corresponding to InSight seismic event S1160a. Images: NASA/JPL/MSSS/University of Arizona.
Paper: Two Seismic Events from InSight Confirmed as New Impacts on Mars
Authors: Ingrid J. Daubar, Benjamin A. Fernando, Raphaël F. Garcia, Peter M. Grindrod, Géraldine Zenhäusern, Natalia Wójcicka, Nicholas A. Teanby, Simon C. Stähler, Liliya Posiolova, Anna C. Horleston, Gareth S. Collins, Constantinos Charalambous, John Clinton, Maria E. Banks, Marouchka Froment, Philippe Lognonné, Mark Panning, W. Bruce Banerdt
Figure caption: Magnitude–distance distribution of InSight very high frequency (VF) seismic events on Mars. Orange and blue triangles mark VF events with and without “chirps” in their signal, respectively. Confirmed impact events are marked with a red circle. Event distances are taken from the InSight Mars Quake Service (MQS) catalog (InSight Marsquake Service 2023) for nonimpacts, while impact events are set to their known respective crater distances from InSight in degrees. Event magnitudes are also from the MQS catalog, but are recalculated for impact events using the correct distances.
Paper: Two Seismic Events from InSight Confirmed as New Impacts on Mars
Authors: Ingrid J. Daubar, Benjamin A. Fernando, Raphaël F. Garcia, Peter M. Grindrod, Géraldine Zenhäusern, Natalia Wójcicka, Nicholas A. Teanby, Simon C. Stähler, Liliya Posiolova, Anna C. Horleston, Gareth S. Collins, Constantinos Charalambous, John Clinton, Maria E. Banks, Marouchka Froment, Philippe Lognonné, Mark Panning, W. Bruce Banerdt
Figure caption: Vertical/north velocity component coherograms (upper panels) and vertical component velocity spectrograms (lower panels) of InSight events S1034a (top) and S1160a (bottom), showing the acoustic chirp signals (dashed black ovals) following the first P-wave arrivals (red lines).
Paper: Temporal Evolution of Titan’s Stratospheric Temperatures and Trace Gases from a Two-dimensional Retrieval of Cassini Composite Infrared Spectrometer Data
Authors: Richard K. Achterberg
Figure caption: As Figure 8, for the C2H2 volume mixing ratio.
Paper: Temporal Evolution of Titan’s Stratospheric Temperatures and Trace Gases from a Two-dimensional Retrieval of Cassini Composite Infrared Spectrometer Data
Authors: Richard K. Achterberg
Figure caption: Cross sections of zonal mean winds, calculated from the temperature data of Figure 8 using the gradient wind approximation, assuming a lower boundary condition assuming winds at 100 km in solid body rotation at 4 times Titan’s rotation rate.
Paper: Temporal Evolution of Titan’s Stratospheric Temperatures and Trace Gases from a Two-dimensional Retrieval of Cassini Composite Infrared Spectrometer Data
Authors: Richard K. Achterberg
Figure caption: As Figure 8, for the haze volume extinction (cm−1 at 100 cm−1) retrieved from FP4 data. There are three contours per decade.
Paper: Temporal Evolution of Titan’s Stratospheric Temperatures and Trace Gases from a Two-dimensional Retrieval of Cassini Composite Infrared Spectrometer Data
Authors: Richard K. Achterberg
Figure caption: As Figure 8, for the C2H6 volume mixing ratio.
Paper: Temporal Evolution of Titan’s Stratospheric Temperatures and Trace Gases from a Two-dimensional Retrieval of Cassini Composite Infrared Spectrometer Data
Authors: Richard K. Achterberg
Figure caption: As Figure 8, for the C3H8 volume mixing ratio.
Paper: Temporal Evolution of Titan’s Stratospheric Temperatures and Trace Gases from a Two-dimensional Retrieval of Cassini Composite Infrared Spectrometer Data
Authors: Richard K. Achterberg
Figure caption: As Figure 8, for the CH3C2H volume mixing ratio.
Paper: Temporal Evolution of Titan’s Stratospheric Temperatures and Trace Gases from a Two-dimensional Retrieval of Cassini Composite Infrared Spectrometer Data
Authors: Richard K. Achterberg
Figure caption: As Figure 8, for the C4H2 volume mixing ratio.
Paper: Temporal Evolution of Titan’s Stratospheric Temperatures and Trace Gases from a Two-dimensional Retrieval of Cassini Composite Infrared Spectrometer Data
Authors: Richard K. Achterberg
Figure caption: As Figure 8, for the HCN volume mixing ratio.
Paper: Roughness and Angularity of Fragments from Meteorite Disruption Experiments
Authors: Gabriel Gowman, Desireé Cotto-Figueroa, Andrew Ryan, Laurence A. J. Garvie, Christian G. Hoover, Erik Asphaug
Figure caption: Plots showing the dependence of AI g  on spherical harmonic degree ℓ and output resolution as measured by the geodesic frequency v. The degree dependence is tested with v = 64; the frequency dependence is tested with ℓ = 25. Samples from Allende are shown with upward-pointing triangles, while samples from Tamdakht are shown with filled circles. Additionally, “shard” samples (with flat surfaces present) have dotted lines, while “random fragment” samples have dashed lines. (a) As the spherical harmonic degree increases, the values of AI g  generally increase, but they do not all show the monotonically increasing behavior of the resolution dependence. They also do not show asymptotic behavior, making it difficult to define a cutoff. We use degree 25 for the calculations in this paper, following the method of Su et al. (2020). (b) As the number of faces increases, the values of AI g  appear to smoothly approach asymptotes. We use v = 64 for the calculations in this paper.
Paper: Roughness and Angularity of Fragments from Meteorite Disruption Experiments
Authors: Gabriel Gowman, Desireé Cotto-Figueroa, Andrew Ryan, Laurence A. J. Garvie, Christian G. Hoover, Erik Asphaug
Figure caption: Plot of whole-sample values of AI g  vs. θ rms. Allende samples are plotted with triangles and dashed lines, Aba Panu samples with squares and a dashed–dotted line, and Tamdakht samples with filled circles and dotted lines for each sample source. Best-fit lines are plotted for each collection with three or more members, and correlation coefficients r are provided for each; however, correlations appear subtle and inconsistent at best.
Paper: Roughness and Angularity of Fragments from Meteorite Disruption Experiments
Authors: Gabriel Gowman, Desireé Cotto-Figueroa, Andrew Ryan, Laurence A. J. Garvie, Christian G. Hoover, Erik Asphaug
Figure caption: Plots illustrating the dependence of θ rms on strength properties. The rms slope and strength show little correlation. However, average roughness is lower for the higher-m Allende samples. (a) Plot of rms slope vs. compressive strength σ for all shard samples. (b) Plot of rms slope vs. Weibull parameter m for Allende and Tamdakht samples.
Paper: Roughness and Angularity of Fragments from Meteorite Disruption Experiments
Authors: Gabriel Gowman, Desireé Cotto-Figueroa, Andrew Ryan, Laurence A. J. Garvie, Christian G. Hoover, Erik Asphaug
Figure caption: 3D plot of local rms slope θ rms,i  distributed over the simplified model’s faces. Each of these plots compares a 50 μm scale model to a 500 μm scale model. Local rms slope values on the color bar are measured in degrees.
Paper: Roughness and Angularity of Fragments from Meteorite Disruption Experiments
Authors: Gabriel Gowman, Desireé Cotto-Figueroa, Andrew Ryan, Laurence A. J. Garvie, Christian G. Hoover, Erik Asphaug
Figure caption: 3D plots of AI g,i  over the surfaces of the scanned samples. Color (and the values of AI g,i  in the color bars) for these figures is on a log10 scale, restricted to the range from 10−0.25 to 101.8 deg.
Paper: Roughness and Angularity of Fragments from Meteorite Disruption Experiments
Authors: Gabriel Gowman, Desireé Cotto-Figueroa, Andrew Ryan, Laurence A. J. Garvie, Christian G. Hoover, Erik Asphaug
Figure caption: 3D models of selected samples from Allende (A-RF-1) and Tamdakht (T-S-t3a-2).
Paper: Roughness and Angularity of Fragments from Meteorite Disruption Experiments
Authors: Gabriel Gowman, Desireé Cotto-Figueroa, Andrew Ryan, Laurence A. J. Garvie, Christian G. Hoover, Erik Asphaug
Figure caption: Evaluation of a geodesic grid on a sphere and the degree-25 spherical harmonic model of sample A-S-AllB-1 with geodesic frequency v = 1, 4, 16, 64. Higher-resolution models re-create the shape of the sample better but are limited by the accuracy of the finite-degree spherical harmonic model.
Paper: Roughness and Angularity of Fragments from Meteorite Disruption Experiments
Authors: Gabriel Gowman, Desireé Cotto-Figueroa, Andrew Ryan, Laurence A. J. Garvie, Christian G. Hoover, Erik Asphaug
Figure caption: Histogram of θ rms,i  values for the nine samples shown in Figure 1. Histograms are drawn with solid lines. The best-fit lognormal distribution is drawn with a dashed line for each sample. These histograms use 250 bins linearly spaced from 0.°1 to 50°. The distribution is similar for coarser or finer binning.
Paper: Grain Size Effects on UV–MIR (0.2–14 μm) Spectra of Carbonaceous Chondrite Groups
Authors: David C. Cantillo, Vishnu Reddy, Adam Battle, Benjamin N. L. Sharkey, Neil C. Pearson, Tanner Campbell, Akash Satpathy, Mario De Florio, Roberto Furfaro, Juan Sanchez
Figure caption: Absolute reflectance of the six grain size bins from our seven studied meteorites across the 0.2–14 μm wavelength range. Each row corresponds to an individual meteorite that is labeled in the leftmost column. Each column corresponds to a set wavelength range, consisting of 0.20–0.60 μm (Column 1), 0.5–2.5 μm (Column 2), 2.0–8.0 μm (Column 3), and 7.5–15.0 μm (Column 4) going from left to right. The range in reflectance for each subpanel varies across meteorite and wavelength range to best display the reflectance features. Different grain sizes across the same meteorite are noted by the line styling in the bottom legend. Color is utilized to indicate the spectrometer used for data collection: blue is Avantes UV, black is ASD Vis–NIR, and red is FTIR NIR–MIR.
Paper: Grain Size Effects on UV–MIR (0.2–14 μm) Spectra of Carbonaceous Chondrite Groups
Authors: David C. Cantillo, Vishnu Reddy, Adam Battle, Benjamin N. L. Sharkey, Neil C. Pearson, Tanner Campbell, Akash Satpathy, Mario De Florio, Roberto Furfaro, Juan Sanchez
Figure caption: Relative reflectance of the six grain size bins from our seven studied meteorites across the 0.2–14 μm wavelength range. The figure layout is identical to that of Figure 1. Column 1 (∼0.20–0.60 μm) is normalized to unity at 0.55 μm, Column 2 (0.6–2.5 μm) is normalized to unity at 1.5 μm, Column 3 (2.5–8 μm) is normalized to unity at 5.0 μm, and Column 4 (∼8–14 μm) is normalized to unity at 13 μm. Normalizing the spectra in our four wavelength bins allows us to better see trends in slope and band depth across varying grain sizes.
Paper: Grain Size Effects on UV–MIR (0.2–14 μm) Spectra of Carbonaceous Chondrite Groups
Authors: David C. Cantillo, Vishnu Reddy, Adam Battle, Benjamin N. L. Sharkey, Neil C. Pearson, Tanner Campbell, Akash Satpathy, Mario De Florio, Roberto Furfaro, Juan Sanchez
Figure caption: The plot of 0.8–1.8 μm spectral slope of our seven studied meteorite samples across our five grain sizes and slab.
Paper: Grain Size Effects on UV–MIR (0.2–14 μm) Spectra of Carbonaceous Chondrite Groups
Authors: David C. Cantillo, Vishnu Reddy, Adam Battle, Benjamin N. L. Sharkey, Neil C. Pearson, Tanner Campbell, Akash Satpathy, Mario De Florio, Roberto Furfaro, Juan Sanchez
Figure caption: The plot of the offset in Christiansen feature band center relative to the 45–90 μm powder for each of our seven studied meteorite samples across our five grain size bins and slab.
Paper: Grain Size Effects on UV–MIR (0.2–14 μm) Spectra of Carbonaceous Chondrite Groups
Authors: David C. Cantillo, Vishnu Reddy, Adam Battle, Benjamin N. L. Sharkey, Neil C. Pearson, Tanner Campbell, Akash Satpathy, Mario De Florio, Roberto Furfaro, Juan Sanchez
Figure caption: The plot of normalized 0.8–1.8 μm spectral slope averaged across our seven studied meteorites for each grain size. The meteorites are offset in the y-direction such that the normalized spectral slope is equal to 1.00 for the smallest grain size bin. The x-axis error bars correspond to this range in grain size between the bin’s boundaries, while the y-axis error bars correspond to the minimum and maximum normalized band depth of individual meteorites in that bin. A negative natural log trend shows the best fit for the data.
Paper: Grain Size Effects on UV–MIR (0.2–14 μm) Spectra of Carbonaceous Chondrite Groups
Authors: David C. Cantillo, Vishnu Reddy, Adam Battle, Benjamin N. L. Sharkey, Neil C. Pearson, Tanner Campbell, Akash Satpathy, Mario De Florio, Roberto Furfaro, Juan Sanchez
Figure caption: The plot of 0.55 μm (photometric V filter) absolute reflectance of our seven studied meteorite samples across our five grain size bins. Slab data are included for thoroughness, though they are not connected due to their unconstrained grain size. Due to material constraints, Tarda lacks a slab measurement.
Paper: Grain Size Effects on UV–MIR (0.2–14 μm) Spectra of Carbonaceous Chondrite Groups
Authors: David C. Cantillo, Vishnu Reddy, Adam Battle, Benjamin N. L. Sharkey, Neil C. Pearson, Tanner Campbell, Akash Satpathy, Mario De Florio, Roberto Furfaro, Juan Sanchez
Figure caption: The plot of ∼1 μm band depth of our seven studied meteorite samples across our five grain size bins and slab.
Paper: Grain Size Effects on UV–MIR (0.2–14 μm) Spectra of Carbonaceous Chondrite Groups
Authors: David C. Cantillo, Vishnu Reddy, Adam Battle, Benjamin N. L. Sharkey, Neil C. Pearson, Tanner Campbell, Akash Satpathy, Mario De Florio, Roberto Furfaro, Juan Sanchez
Figure caption: The plot of 0.35–2.5 μm (Vis–NIR) spectra of CM2 Aguas Zarcas powders. Aguas Zarcas has a positive (red) spectral slope at smaller grain sizes and shifts to a negative (blue) spectral slope with increasing particle size. The data is normalized to unity at 1.5 μm.
Paper: Temporal Evolution of Titan’s Stratospheric Temperatures and Trace Gases from a Two-dimensional Retrieval of Cassini Composite Infrared Spectrometer Data
Authors: Richard K. Achterberg
Figure caption: Top: modeled Titan spectra between 600 and 850 cm−1 for a limb-viewing geometry with a tangent point at 80°N latitude, 150 km altitude, at spectral resolutions of 0.5 cm−1 (left) and 15.5 cm−1 (right), using a full 2D radiative model with latitude variations of all atmospheric parameters (black lines), a 1D radiative model with atmospheric parameters for 80°N (red lines), and a hybrid model with only temperature and haze extinction variable with latitude (blue lines). Second row: difference between the 2D forward model and the 1D model (red lines) and hybrid model (blue lines) at 0.5 cm−1 (left) and 15.5 cm−1 (right). The black dashed line is the estimated noise equivalent radiance for an average of 25 CIRS spectra. Third row: as top row, for 400 km altitude. Bottom: as second row, for 400 km altitude.
Paper: Temporal Evolution of Titan’s Stratospheric Temperatures and Trace Gases from a Two-dimensional Retrieval of Cassini Composite Infrared Spectrometer Data
Authors: Richard K. Achterberg
Figure caption: Top: modeled Titan spectra between 1100 and 1400 cm−1 for a limb-viewing geometry with a tangent point at 80°N latitude, 150 km altitude, at spectral resolutions of 0.5 cm−1 (left) and 15.5 cm−1 (right), using a full 2D radiative model with latitude variations of all atmospheric parameters (black lines), and a 1D radiative model with atmospheric parameters for 80°N (red lines). Second row: difference between the 2D forward model and the 1D model (red lines) at 0.5 cm−1 (left) and 15.5 cm−1 (right). The black dashed line is the estimated noise equivalent radiance for an average of 25 CIRS spectra. Third row: as top row, for 400 km altitude. Bottom: as second row, for 400 km altitude.
Paper: Temporal Evolution of Titan’s Stratospheric Temperatures and Trace Gases from a Two-dimensional Retrieval of Cassini Composite Infrared Spectrometer Data
Authors: Richard K. Achterberg
Figure caption: Temperatures retrieved using a 2D model from pairs of observations on 2005 August and October (T4, T6; top left), 2007 November and December (T37, T39; top right), 2010 June (T69, T70; second row, left), 2011 May and June (T76, T77; second row, right), 2012 January and February (T80, T82; third row, left), 2015 March and May (T110, T111; third row, right), 2015 September and November (T113, T114; bottom left), and 2015 February (T116, T117; bottom right). Contour intervals are 10 K.
Paper: Temporal Evolution of Titan’s Stratospheric Temperatures and Trace Gases from a Two-dimensional Retrieval of Cassini Composite Infrared Spectrometer Data
Authors: Richard K. Achterberg
Figure caption: Fits to FP3 (left) and FP4 (right) spectra at a sample of the tangent heights at 85°N for 1D (blue lines) and 2D (red lines) retrievals from the T4 MIRLBMAP observation on 2005 April 1. The data are shown as black squares with error bars. Spectra at successive tangent heights are offset by ﹩{10}^{-7}\,{\rm{W}}\,{\mathrm{cm}}^{-2}\,{\mathrm{str}}^{-1}\,/\,{\mathrm{cm}}^{-1}﹩ for FP3 and ﹩2\times {10}^{-8}\,{\rm{W}}\,{\mathrm{cm}}^{-2}\,{\mathrm{str}}^{-1}\,/\,{\mathrm{cm}}^{-1}﹩ for FP4.
Paper: Temporal Evolution of Titan’s Stratospheric Temperatures and Trace Gases from a Two-dimensional Retrieval of Cassini Composite Infrared Spectrometer Data
Authors: Richard K. Achterberg
Figure caption: Time and latitude coverage of the limb-mapping observations (MIRLMBMAPs) taken by Cassini CIRS. Observations discussed in this paper are indicated by red “×”s, other observations by gray “+”s.
Paper: Temporal Evolution of Titan’s Stratospheric Temperatures and Trace Gases from a Two-dimensional Retrieval of Cassini Composite Infrared Spectrometer Data
Authors: Richard K. Achterberg
Figure caption: Retrievals of temperature (top row), haze volume extinction at 100 cm−1 (second row), C2H6 volume mixing ratio (third row), and C2H2 volume mixing ratio (bottom row) from the T4 MIRLMBMAP observation on 2005 April 1. The left column is retrievals using a 2D retrieval model, the right column is from a 1D retrieval model.
Paper: Temporal Evolution of Titan’s Stratospheric Temperatures and Trace Gases from a Two-dimensional Retrieval of Cassini Composite Infrared Spectrometer Data
Authors: Richard K. Achterberg
Figure caption: Retrievals of HCN (top row), C4H2 volume mixing ratio (second row), CH3C2H volume mixing ratio (third row), and C3H8 volume mixing ratio (bottom row) from the T4 MIRLMBMAP observation on 2005 April 1. The left column is retrievals using a 2D retrieval model, the right column is from a 1D retrieval model.
Paper: Temporal Evolution of Titan’s Stratospheric Temperatures and Trace Gases from a Two-dimensional Retrieval of Cassini Composite Infrared Spectrometer Data
Authors: Richard K. Achterberg
Figure caption: Raypaths for the MIRLMBMAP observation during the T4 flyby on 2005 April 1 (solid black lines), plotted over the temperatures retrieved by Achterberg et al. (2008) from a combination of limb and nadir data from the first 2 yr of the Cassini mission. Contour interval for the temperatures is 10 K.
Paper: Impact Crater Morphometry on Pluto: Implications for Surface Composition and Evolution
Authors: Joshua E. Hedgepeth, Catherine D. Neish, Veronica J. Bray
Figure caption: This illustration visualizes potential crater morphologies in Pluto’s layered ice, contingent on various thicknesses of the volatile-ice layer. The figure compares the immediate postimpact morphologies to the preimpact surface, as well as to the stages following short- and long-term alterations due to possible escape erosion and relaxation. Note that this figure is a conceptual model designed to underscore how we expect crater depth to change, rather than a true-to-life model of crater morphology. Furthermore, “short” and “long” are relative terms, with duration dependent on the type of volatile ice. Craters formed in a volatile-ice layer that is thick enough (i.e., h > d, where h is the volatile-ice thickness, and d is the crater depth) are presumed to generate a traditional, albeit shallower, crater shape that relaxes over time. If craters form in less thick volatile-ice layers, we assume that they behave like craters formed in layered terrains similar to those found on Mars, where water ice overlays stronger basalt bedrock (see text for details). Escape erosion and deposition could alter any crater, with the craters formed in thicker volatile-ice layers (h > 0.5 ∗ d) affected most, as thinner layers (h < 0.5 ∗ d) would form stronger water-ice rims when the stratigraphy is inverted during impact. In scenarios of moderate volatile thickness (d > h > 0.5 ∗ d), the volatile ice is anticipated to behave fluidly, with the thicker layer capable of concealing the sturdier water-ice basin. Depending on the strength of the volatile ice, a shallow crater basin might form, but it would rapidly undergo viscous relaxation. Ultimately, escape erosion may reveal a shallower water-ice crater. For extremely thick volatile layers (h > d), escape erosion will work alongside relaxation to degrade the crater.