adsabs/AstroCLIMB huggingface dataset:
Paper: The Peregrine Ion Trap Mass Spectrometer (PITMS) Investigation Development and Preflight Planning
Authors: Barbara A. Cohen, Simeon J. Barber, Phillip A. Driggers, David Heather, Christopher Howe, Peter Landsberg, Thomas Morse, Roland Trautner, Feargus Abernethy, Emma-May Butroid, Natalie M. Curran, Christophe Delepaut, Ellis Elliott, Javier Fernandez Salgado, Joseph A. Generie, Philipp Hager, Sophie Hall, Fiona Hillier, Max Hodgkins, Sara Iacobellis, Alicja Kasjanowicz, Ewout Koekkoek, Mark Leese, Karin Lundmark, Jeremy Mayers, Andrew Morse, James Mortimer, Hume L. Peabody, Patrick Reast, Simon Sheridan, Richard Stamper, Peter J. Steigner, Harald Stier, Lauren Summers, Orenthal J. Tucker, Martin Whalley, Simon Woodward
Figure caption: Illustration (nonquantitative) of (a) representative voltage profiles and (b) representative detector counts for the different phases of PITMS operation. The filament and detector bias are kept at constant values throughout the measurement. During the ionization phase, the source gate is open, creating ions that are trapped in the ring electrode field. The settle and post-settle phases allow the source gate to close and the detector gate to open. During the measurement phase, the amplitude of the ring electrode field is increased, sequentially ejecting ions of increasing m/z value. (c) The detector counts would be calibrated to produce instrument-independent mass spectra in units of partial pressure as a function of m/z.
Paper: The Peregrine Ion Trap Mass Spectrometer (PITMS) Investigation Development and Preflight Planning
Authors: Barbara A. Cohen, Simeon J. Barber, Phillip A. Driggers, David Heather, Christopher Howe, Peter Landsberg, Thomas Morse, Roland Trautner, Feargus Abernethy, Emma-May Butroid, Natalie M. Curran, Christophe Delepaut, Ellis Elliott, Javier Fernandez Salgado, Joseph A. Generie, Philipp Hager, Sophie Hall, Fiona Hillier, Max Hodgkins, Sara Iacobellis, Alicja Kasjanowicz, Ewout Koekkoek, Mark Leese, Karin Lundmark, Jeremy Mayers, Andrew Morse, James Mortimer, Hume L. Peabody, Patrick Reast, Simon Sheridan, Richard Stamper, Peter J. Steigner, Harald Stier, Lauren Summers, Orenthal J. Tucker, Martin Whalley, Simon Woodward
Figure caption: The Gruithuisen domes and Sinus Viscositatis as identified in the IAU Nomenclature Gazetteer (https://planetarynames.wr.usgs.gov/Feature/16118). The planned Peregrine Mission-1 landing region is shown in orange (centered at 35.°07 north, 41.°76 west); the actual landing site within this region would have been chosen during the mission.
Paper: The Peregrine Ion Trap Mass Spectrometer (PITMS) Investigation Development and Preflight Planning
Authors: Barbara A. Cohen, Simeon J. Barber, Phillip A. Driggers, David Heather, Christopher Howe, Peter Landsberg, Thomas Morse, Roland Trautner, Feargus Abernethy, Emma-May Butroid, Natalie M. Curran, Christophe Delepaut, Ellis Elliott, Javier Fernandez Salgado, Joseph A. Generie, Philipp Hager, Sophie Hall, Fiona Hillier, Max Hodgkins, Sara Iacobellis, Alicja Kasjanowicz, Ewout Koekkoek, Mark Leese, Karin Lundmark, Jeremy Mayers, Andrew Morse, James Mortimer, Hume L. Peabody, Patrick Reast, Simon Sheridan, Richard Stamper, Peter J. Steigner, Harald Stier, Lauren Summers, Orenthal J. Tucker, Martin Whalley, Simon Woodward
Figure caption: Left: a solid model of the EMS proto-flight model; right: the as-built EMS proto-flight model. The ITMS is in a clean cavity that is isolated from the printed circuit boards (PCBs) stacked below it, with separate outgassing paths.
Paper: The Peregrine Ion Trap Mass Spectrometer (PITMS) Investigation Development and Preflight Planning
Authors: Barbara A. Cohen, Simeon J. Barber, Phillip A. Driggers, David Heather, Christopher Howe, Peter Landsberg, Thomas Morse, Roland Trautner, Feargus Abernethy, Emma-May Butroid, Natalie M. Curran, Christophe Delepaut, Ellis Elliott, Javier Fernandez Salgado, Joseph A. Generie, Philipp Hager, Sophie Hall, Fiona Hillier, Max Hodgkins, Sara Iacobellis, Alicja Kasjanowicz, Ewout Koekkoek, Mark Leese, Karin Lundmark, Jeremy Mayers, Andrew Morse, James Mortimer, Hume L. Peabody, Patrick Reast, Simon Sheridan, Richard Stamper, Peter J. Steigner, Harald Stier, Lauren Summers, Orenthal J. Tucker, Martin Whalley, Simon Woodward
Figure caption: Left: a prototype of the PITMS ion trap hardware; right: schematic showing the parts of the sensor.
Paper: The Peregrine Ion Trap Mass Spectrometer (PITMS) Investigation Development and Preflight Planning
Authors: Barbara A. Cohen, Simeon J. Barber, Phillip A. Driggers, David Heather, Christopher Howe, Peter Landsberg, Thomas Morse, Roland Trautner, Feargus Abernethy, Emma-May Butroid, Natalie M. Curran, Christophe Delepaut, Ellis Elliott, Javier Fernandez Salgado, Joseph A. Generie, Philipp Hager, Sophie Hall, Fiona Hillier, Max Hodgkins, Sara Iacobellis, Alicja Kasjanowicz, Ewout Koekkoek, Mark Leese, Karin Lundmark, Jeremy Mayers, Andrew Morse, James Mortimer, Hume L. Peabody, Patrick Reast, Simon Sheridan, Richard Stamper, Peter J. Steigner, Harald Stier, Lauren Summers, Orenthal J. Tucker, Martin Whalley, Simon Woodward
Figure caption: Views of the PITMS instrument mounted to the Peregrine deck. The EMS is shrouded in multilayer insulation inside the white-painted Wrapper.
Paper: Europa’s H2O2: Temperature Insensitivity and a Correlation with CO2 
Authors: Peiyu Wu, Samantha K. Trumbo, Michael E. Brown, Katherine de Kleer
Figure caption: Additional representative paired slits to illustrate the lack of a strong diurnal trend. We examine a total of five Keck slit pairs observed on adjacent nights in 2016 and 2018, one of which is shown in Figure 2, and two slit pairs observed across different years. Time spans for each paired comparison are labeled on top. (a) Paired slits from consecutive nights obtained on 2016 February 24 (top) and 2016 February 25 (bottom), when overlapped regions (∼18°–36° west) are in the morning and afternoon, respectively. (b) Paired slits slightly south of A with a slightly shorter time span, obtained on 2016 February 24 (top) and 2016 February 25 (bottom), when overlapped regions (∼20°–45° west) are in the morning and afternoon, respectively. (c) Paired slits obtained from consecutive nights on 2018 June 06 (top) and 2018 June 07 (bottom), when overlapped regions (∼155°–179° west) are in the morning and afternoon, respectively. (d) Paired slits from consecutive nights obtained on 2018 June 06 (top) and 2018 June 07 (bottom), when overlapped regions (∼157°–180° west) are in the morning and afternoon, respectively. (e) Paired slits obtained across years on 2013 December 29 (top) and 2018 June 07 (bottom), when overlapped regions (∼155°–182° west) are in the morning and afternoon, respectively. (f) Paired slits obtained across years on 2018 June 06 (top) and 2013 December 29 (bottom), when overlapped regions (∼155°–181° west) are in the morning and afternoon, respectively. For all pairs and overlapping regions examined, the measured band area changes from morning to afternoon are within −32%–44% (factor of 0.68–1.44). These results suggest the absence of a strong diurnal trend and a lack of sensitivity in H2O2 to temperature variations over the assessed timescales. The slits also present a clear difference between low-latitude chaos and low-latitude plains terrain in east/west slits crossing the leading chaos regions (panels (a)–(d)) and a depletion of H2O2 west of the anti-Jovian point around 210° west, corresponding to a gap between the large-scale chaos regions of the leading and trailing hemispheres (panels (c)–(f)). Leading and trailing chaos regions are outlined in black (E. J. Leonard et al. 2024). Background basemap credit: USGS (2002).
Paper: Europa’s H2O2: Temperature Insensitivity and a Correlation with CO2 
Authors: Peiyu Wu, Samantha K. Trumbo, Michael E. Brown, Katherine de Kleer
Figure caption: (a) Example Keck NIRSPEC slit obtained on 2016 February 24, when 18.°6 west (labeled with the black circle) is in the morning (∼13 hr prior to local noon in Europa’s ∼85 hr day, estimated ∼103 K). (b) Example Keck NIRSPEC slit obtained on 2016 February 25, when the same region (18.°5 west; labeled with the red circle) is in the afternoon (∼16 hr after local noon in Europa’s ∼85 hr day, estimated ∼115 K). (c) Corresponding reflectance spectra for this location in the morning (in black) and in the afternoon (in red). Dashed gray lines outline the H2O2 band. Second-order polynomial continua are indicated by the dashed curves of the same color as the spectrum. Continuum-removed absorptions are included and show nearly overlapping absorptions. A ∼12 K temperature increase over 24 hr is estimated from the thermal model of S. K. Trumbo et al. (2017a). This temperature change results in a negligible −3.1% change in the integrated band areas. Leading chaos regions are outlined in black (E. J. Leonard et al. 2024). Background basemap credit: USGS (2002).
Paper: Europa’s H2O2: Temperature Insensitivity and a Correlation with CO2 
Authors: Peiyu Wu, Samantha K. Trumbo, Michael E. Brown, Katherine de Kleer
Figure caption: (a) Map of the H2O2 integrated band area from the JWST Cycle 1 observations. Gray dashed lines indicate the meridians and the 60° south, 30° south, 0° north, 30° north, and 60° north parallels. The strongest absorption occurs in Tara Regio (∼85° west) to the right of the 90° west meridian and in parts of the chaos region Powys Regio (∼125° west) on the left portion of the disk. (b) Map of the entire ν 3 CO2 integrated band area (μm; S. K. Trumbo & M. E. Brown 2023). Concentrated CO2 occurs in the same regions as concentrated H2O2—the leading chaos terrains. The disk of Europa is indicated by a black circle centered at 2.7° north, 93° west. (c) Linear fit illustrating the relationship between the distributions of the two features. A Pearson correlation coefficient of 0.94 (P < 0.001) signifies a strong positive correlation between the distributions of H2O2 and CO2 on the leading hemisphere. Consistent with S. K. Trumbo & M. E. Brown (2023), limb pixels affected by the instrument’s inherent undersampling of the point-spread function are excluded. Oscillations affected the measurement of the 3.5 μm H2O2 feature in more pixels than that of the CO2 feature. Therefore, a few more pixels are excluded than in S. K. Trumbo & M. E. Brown (2023). Leading chaos regions are outlined in black (E. J. Leonard et al. 2024).
Paper: Europa’s H2O2: Temperature Insensitivity and a Correlation with CO2 
Authors: Peiyu Wu, Samantha K. Trumbo, Michael E. Brown, Katherine de Kleer
Figure caption: Mapped Keck NIRSPEC slits from our 2013, 2016, 2018, and 2021 observations on the (a) leading and (b) trailing hemispheres, which show the spatial distribution of Europa’s 3.5 μm H2O2 band. Consistent with full-disk spectra (K. P. Hand & M. E. Brown 2013) and previous spatially resolved spectra (S. K. Trumbo et al. 2019a), the geologically young chaos regions on the leading hemisphere (outlined in black; E. J. Leonard et al. 2024) exhibit the largest H2O2 features. In contrast, the trailing hemisphere demonstrates generally much weaker absorptions compared to the leading hemisphere and a depletion of H2O2 west of the anti-Jovian point around 210° west, corresponding to a gap between the large-scale chaos regions of the leading and trailing hemispheres. We note that observations from various years are mapped together to illustrate the updated coverage of Europa’s H2O2, despite some apparently stochastic fluctuations in H2O2 between 2016 and later years. Background basemap credit: USGS (2002).
Paper: Europa’s H2O2: Temperature Insensitivity and a Correlation with CO2 
Authors: Peiyu Wu, Samantha K. Trumbo, Michael E. Brown, Katherine de Kleer
Figure caption: Averaged spectra for each ∼1 hr time window of (a) 2 hr pre-eclipse, (b) 1 hr pre-eclipse, (c) 1 hr post-eclipse, (d) 2 hr post-eclipse, (e) 3 hr post-eclipse, (f) 4 hr post-eclipse, (g) 5 hr post-eclipse, and (h) 6 hr post-eclipse. All spectra are normalized to their individual peaks in the 3.6–3.7 μm region. Dashed gray lines outline the H2O2 band. Second-order polynomial continua are indicated by the black dashed curves. Continuum-removed absorptions are included. We note that the 3 hr post-eclipse spectrum is noisier owing to a shorter observation time (necessitated by weather conditions), as indicated in Table 1. A factor of change <2 is shown in the H2O2 band throughout the 8 hr time period surrounding eclipse. The slight changes to the background water-ice absorption bands suggest likely rotational effects as Europa rotates from a more trailing/sub-Jovian geometry toward a more sub-Jovian/leading geometry. More discussion is included in Section 3.
Paper: Europa’s H2O2: Temperature Insensitivity and a Correlation with CO2 
Authors: Peiyu Wu, Samantha K. Trumbo, Michael E. Brown, Katherine de Kleer
Figure caption: Representative JWST spectra used for Figure 4, showing both the H2O2 and CO2 bands in the Cycle 1 JWST data recently used to map Europa’s leading-hemisphere CO2 (S. K. Trumbo & M. E. Brown 2023; G. L. Villanueva et al. 2023). The black spectrum is extracted from a pixel within Tara Regio (92° west, 17° south), and the gray spectrum is extracted from a pixel north of Tara Regio (57° west, 19° north). A clear enrichment of both H2O2 and CO2 is shown in the Tara Regio spectrum.
Paper: Experimental Examination of Brine and Water Lifetimes after Impact on Airless Worlds
Authors: Michael J. Poston, Samantha R. Baker, Jennifer E. C. Scully, Elizabeth M. Carey, Lauren E. Mc Keown, Julie C. Castillo-Rogez, Carol A. Raymond
Figure caption: Eutectic (23%) brine with JSC-1a and stirring. JSC-1a_dilute_Brined_Stirred_2022-05-12_16-01-41 0:02—valve closed 0:03—during expansion, 0:12—floating crystals beginning to form, 0:25—floating crystals stop flowing, 0:57—beginning to consolidate on walls and rod, some overturn begins, 2:03—lid/overturn consolidates enough to stop rotating (around 6:40 the lid becomes opaque enough to no longer see the spindle blades), 7:54—shortly before spindle stuck.
Paper: Experimental Examination of Brine and Water Lifetimes after Impact on Airless Worlds
Authors: Michael J. Poston, Samantha R. Baker, Jennifer E. C. Scully, Elizabeth M. Carey, Lauren E. Mc Keown, Julie C. Castillo-Rogez, Carol A. Raymond
Figure caption: Eutectic (23%) brine with JSC-1a and stirring. JSC-1a_Brine_Stirred_2022-05-12_14-15-24 (not “dilute”) 0:14—valve closed, 0:20—during expansion, 0:28—lumpy crust formed, but several openings to bright lower layer, 0:37—lumpy crust has mostly closed up, 0:47—overturn starting, 1:47—large chunks have overturned, revealing brighter surfaces, 6:51—after several minutes without stirring, the material has further brightened.
Paper: Experimental Examination of Brine and Water Lifetimes after Impact on Airless Worlds
Authors: Michael J. Poston, Samantha R. Baker, Jennifer E. C. Scully, Elizabeth M. Carey, Lauren E. Mc Keown, Julie C. Castillo-Rogez, Carol A. Raymond
Figure caption: Eutectic (23%) brine with stirring. Brine_Stirred_2022-05-11_17-59-20 0:05—valve closed 0:10—during expansion 0:38—thin layer of unconsolidated solid floating on top 3:05—thicker layer of unconsolidated solid floating on top 4:04—beginning to consolidate on walls and rod 4:58—more consolidated, with piece angled up out of the liquid 5:57—some of the last liquid flows onto surface 6:52—fully consolidated 8:25—spindle stuck.
Paper: Experimental Examination of Brine and Water Lifetimes after Impact on Airless Worlds
Authors: Michael J. Poston, Samantha R. Baker, Jennifer E. C. Scully, Elizabeth M. Carey, Lauren E. Mc Keown, Julie C. Castillo-Rogez, Carol A. Raymond
Figure caption: Eutectic (23%) brine with JSC-1a and stirring. JSC-1a_dilute_Brine_Stirred_2022-05-12_17-18-53 0:06—valve closed, 0:07—during expansion, 0:29—thin layer of unconsolidated solid floating on top stops flowing, 2:09—droplet reveals solid still unconsolidated, though has been starting to stick to walls, 3:09—overturning lid has nearly consolidated “now it's like a hummocky texture,” 10:55—spindle stuck.
Paper: Experimental Examination of Brine and Water Lifetimes after Impact on Airless Worlds
Authors: Michael J. Poston, Samantha R. Baker, Jennifer E. C. Scully, Elizabeth M. Carey, Lauren E. Mc Keown, Julie C. Castillo-Rogez, Carol A. Raymond
Figure caption: Eutectic (23%) brine with stirring. Brine_Stirred400_2022-05-11_17-12-28 0:37—valve closed 0:38—during expansion 0:56—thin layer of unconsolidated solid floating on top 2:49—layer is thick enough to block sight through liquid in cup 3:55—beginning to consolidate on walls and rod 4:42—overturn has begun 5:37—spindle stuck, last visible bit of liquid turns solid.
Paper: Experimental Examination of Brine and Water Lifetimes after Impact on Airless Worlds
Authors: Michael J. Poston, Samantha R. Baker, Jennifer E. C. Scully, Elizabeth M. Carey, Lauren E. Mc Keown, Julie C. Castillo-Rogez, Carol A. Raymond
Figure caption: Eutectic (23%) brine with stirring. Brine_Stirred3200_quickDegas_2022-05-11_11-17-45 0:05—valve closed 0:06—during expansion 0:24—thin layer of unconsolidated solid floating on top (might have been sooner, but droplet on window blocking most of view) 1:28—overturn underway 1:53—shiny material revealed by overturn, but several seconds later spindle gets stuck.
Paper: Experimental Examination of Brine and Water Lifetimes after Impact on Airless Worlds
Authors: Michael J. Poston, Samantha R. Baker, Jennifer E. C. Scully, Elizabeth M. Carey, Lauren E. Mc Keown, Julie C. Castillo-Rogez, Carol A. Raymond
Figure caption: Eutectic (23%) brine with stirring. Brine_Stirred80_2022-05-11_16-22-03 0:06—valve closed 0:08—during expansion 0:23—thin layer of unconsolidated solid floating on top 3:38—beginning to consolidate on walls and rod 4:14—overturn has begun but sporadic 6:26—shiny material revealed by overturn, but several seconds later spindle gets stuck.
Paper: Experimental Examination of Brine and Water Lifetimes after Impact on Airless Worlds
Authors: Michael J. Poston, Samantha R. Baker, Jennifer E. C. Scully, Elizabeth M. Carey, Lauren E. Mc Keown, Julie C. Castillo-Rogez, Carol A. Raymond
Figure caption: Eutectic (23%) brine with stirring. Brine_Stirred3200_goodDegas_2022-05-11_10-12-01 0:06—valve closed 0:07—during expansion 0:12—thin layer of unconsolidated solid floating on top 0:34—beginning to consolidate on walls and rod 0:39—overturn underway 1:05—shiny material revealed by overturn, but several seconds later spindle gets stuck.
Paper: Experimental Examination of Brine and Water Lifetimes after Impact on Airless Worlds
Authors: Michael J. Poston, Samantha R. Baker, Jennifer E. C. Scully, Elizabeth M. Carey, Lauren E. Mc Keown, Julie C. Castillo-Rogez, Carol A. Raymond
Figure caption: Eutectic (23%) brine with stirring. Brine_Stirred1600_2022-05-11_15-20-49 0:03—valve closed 0:04—during expansion 0:11—thin layer of unconsolidated solid floating on top 3:34—beginning to consolidate on walls and rod 3:47—overturn underway 4:19—shiny material revealed by overturn, but several seconds later spindle gets stuck.
Paper: Multiple Overspill Flood Channels from Young Craters Require Surface Melting and Hundreds of Meters of Midlatitude Ice Late in Mars’s History
Authors: Alexandra O. Warren, Sharon A. Wilson, Alan Howard, Axel Noblet, Edwin S. Kite
Figure caption: (a–d) DEMs and (e–h) topographic rim profiles of multiple-breach tadpole craters. (a) Arabia Terra 1, (b) Arabia Terra 2, (c) Hellas, (d) Noachis (Tadpole crater nicknames, latitude/longitude, and image numbers given in Table 1). B1–B5 mark breaches incised into the rim. Solid black lines show measured rim topography from A to A′, and dotted red lines show interpolated pre-incision topography between fresh-appearing (i.e., unincised) rim sections on either side of each breach.
Paper: The CUISINES Framework for Conducting Exoplanet Model Intercomparison Projects, Version 1.0
Authors: Linda E. Sohl, Thomas J. Fauchez, Shawn Domagal-Goldman, Duncan A. Christie, Russell Deitrick, Jacob Haqq-Misra, C. E. Harman, Nicolas Iro, Nathan J. Mayne, Kostas Tsigaridis, Geronimo L. Villanueva, Amber V. Young, Guillaume Chaverot
Figure caption: Illustration of a “MALBEC.txt” file created by Villanueva et al. (2024) to generate synthetic spectra from model output. The file begins with a description of how the spectra are generated, followed by a list of the input variables and their values for this specific case.
Paper: The CUISINES Framework for Conducting Exoplanet Model Intercomparison Projects, Version 1.0
Authors: Linda E. Sohl, Thomas J. Fauchez, Shawn Domagal-Goldman, Duncan A. Christie, Russell Deitrick, Jacob Haqq-Misra, C. E. Harman, Nicolas Iro, Nathan J. Mayne, Kostas Tsigaridis, Geronimo L. Villanueva, Amber V. Young, Guillaume Chaverot
Figure caption: Illustration of the general experimental design for the CREME exoMIP (K. Tsigaridis et al. 2024, in preparation) as an example of how to structure an exoMIP to allow broad community participation.
Paper: Multiple Overspill Flood Channels from Young Craters Require Surface Melting and Hundreds of Meters of Midlatitude Ice Late in Mars’s History
Authors: Alexandra O. Warren, Sharon A. Wilson, Alan Howard, Axel Noblet, Edwin S. Kite
Figure caption: Meltwater pond overspill modeling results for Arabia Terra 2 B1, B2, B3, B4, and B5 (Figure 1(b)) for measured breach parameters in Table 2 as a function of fractional melt pond area. (a) Downward erosion of breach base per individual overspilling event. Smaller melt pond areas generate less erosion when they overspill the rim. (b) The number of overspill events required to carve each observed breach. The number of breaches required decreases as melt pond area increases. (d) Total water volume required per overspill event in panel (b). (d) Melt days required to generate the water volumes required in panel (c) at a melt rate of 4 m yr−1 m2 (Kite et al. 2013) across the entire crater area.
Paper: Multiple Overspill Flood Channels from Young Craters Require Surface Melting and Hundreds of Meters of Midlatitude Ice Late in Mars’s History
Authors: Alexandra O. Warren, Sharon A. Wilson, Alan Howard, Axel Noblet, Edwin S. Kite
Figure caption: Meltwater pond overspill modeling results for Arabia Terra 1 B1 and B2 (Figure 1(a)) for measured breach parameters in Table 2 as a function of fractional melt pond area. (a) Downward erosion of breach base per individual overspilling event. Smaller melt pond areas generate less erosion when they overspill the rim. (b) The number of overspill events required to carve each observed breach. The number of breaches required decreases as melt pond area increases. (d) Total water volume required per overspill event in panel (b). (d) Melt days required to generate the water volumes required in panel (c) at a melt rate of 4 m yr−1 m2 (Kite et al. 2013) across the entire crater area.
Paper: Multiple Overspill Flood Channels from Young Craters Require Surface Melting and Hundreds of Meters of Midlatitude Ice Late in Mars’s History
Authors: Alexandra O. Warren, Sharon A. Wilson, Alan Howard, Axel Noblet, Edwin S. Kite
Figure caption: Meltwater pond overspill modeling results for Hellas B1 and B2 (Figure 1(c)) for measured breach parameters in Table 2 as a function of fractional melt pond area. (a) Downward erosion of breach base per individual overspilling event. Smaller melt pond areas generate less erosion when they overspill the rim. (b) The number of overspill events required to carve each observed breach. The number of breaches required decreases as melt pond area increases. (d) Total water volume required per overspill event in panel (b). (d) Melt days required to generate the water volumes required in panel (c) at a melt rate of 4 m yr−1 m2 (Kite et al. 2013) across the entire crater area.
Paper: Multiple Overspill Flood Channels from Young Craters Require Surface Melting and Hundreds of Meters of Midlatitude Ice Late in Mars’s History
Authors: Alexandra O. Warren, Sharon A. Wilson, Alan Howard, Axel Noblet, Edwin S. Kite
Figure caption: Schematic illustration of the three remaining multiple-breach tadpole-crater-forming hypotheses (Figure 2) that are consistent with our morphological and modeling constraints on tadpole-breach-forming climate.