adsabs/AstroCLIMB huggingface dataset:
Paper: Approaches for Retrieving Sulfur Species Abundances from Dual X–Ka-band Radio Occultations of Venus with EnVision and VERITAS
Authors: Alex B. Akins, Tatiana M. Bocanegra-Bahamón, Kuo-Nung Wang, Panagiotis Vergados, Chi O. Ao, Sami W. Asmar, Robert A. Preston
Figure caption: Results of cloud aerosol mass simulations for the set (5) model atmosphere. The ensemble of simulations is used to derive a mean profile and associated uncertainties, as shown compared to the true profile.
Paper: Approaches for Retrieving Sulfur Species Abundances from Dual X–Ka-band Radio Occultations of Venus with EnVision and VERITAS
Authors: Alex B. Akins, Tatiana M. Bocanegra-Bahamón, Kuo-Nung Wang, Panagiotis Vergados, Chi O. Ao, Sami W. Asmar, Robert A. Preston
Figure caption: Eddy diffusion profiles used in the 1D atmospheric transport model.
Paper: Approaches for Retrieving Sulfur Species Abundances from Dual X–Ka-band Radio Occultations of Venus with EnVision and VERITAS
Authors: Alex B. Akins, Tatiana M. Bocanegra-Bahamón, Kuo-Nung Wang, Panagiotis Vergados, Chi O. Ao, Sami W. Asmar, Robert A. Preston
Figure caption: Probability of SO2 and H2SO4 aerosol abundance combinations consistent with simulated radio link absorption at X and Ka bands at an altitude of 50 km with an H2SO4 volume mole fraction of 10 ppm. The true abundances used for the simulations are shown as a green dot, and a line is shown representing the range of solutions possible for an error-free measurement.
Paper: Approaches for Retrieving Sulfur Species Abundances from Dual X–Ka-band Radio Occultations of Venus with EnVision and VERITAS
Authors: Alex B. Akins, Tatiana M. Bocanegra-Bahamón, Kuo-Nung Wang, Panagiotis Vergados, Chi O. Ao, Sami W. Asmar, Robert A. Preston
Figure caption: Comparison of retrieved and true column abundances of H2SO4 and SO2. A linear model (black line) is fit to the data assuming a zero intercept and compared to a one-to-one relationship (dashed black line). Regions of 10% (shaded orange) and 25% (shaded blue) are also shown.
Paper: Approaches for Retrieving Sulfur Species Abundances from Dual X–Ka-band Radio Occultations of Venus with EnVision and VERITAS
Authors: Alex B. Akins, Tatiana M. Bocanegra-Bahamón, Kuo-Nung Wang, Panagiotis Vergados, Chi O. Ao, Sami W. Asmar, Robert A. Preston
Figure caption: Draws from the posterior distribution and the median results for H2SO4 aerosol and SO2 profiles for the set (2) model atmosphere.
Paper: Constraints on Europa’s Water Group Torus from HST/COS Observations
Authors: Lorenz Roth, H. Todd Smith, Kazuo Yoshioka, Tracy M. Becker, Aljona Blöcker, Nathaniel J. Cunningham, Nickolay Ivchenko, Kurt D. Retherford, Joachim Saur, Michael Velez, Fuminori Tsuchiya
Figure caption: Observing geometry showing the size and scanning positions of the round 2.″5-wide COS aperture as well as the Galilean moons at their orbital position at the start of the first exposure from 2020 (le2o01010, Table 1). Callisto is beyond the field. The gray dashed lines indicate the moon orbits for Io and Europa, which are both past western elongation approaching eclipse (i.e., moving leftward). (Adapted from https://pds-rings.seti.org.)
Paper: Constraints on Europa’s Water Group Torus from HST/COS Observations
Authors: Lorenz Roth, H. Todd Smith, Kazuo Yoshioka, Tracy M. Becker, Aljona Blöcker, Nathaniel J. Cunningham, Nickolay Ivchenko, Kurt D. Retherford, Joachim Saur, Michael Velez, Fuminori Tsuchiya
Figure caption: Column density maps for H2 (top left), H (top right), and O (bottom) from the torus model (Smith et al. 2019, 2022) in a plane through Jupiter and corresponding to the viewing geometry of the first torus-centered exposure le2oa1010 (Table 1) from 2020. For O, the tori of Europa-genic (left) and Io-genic (right) material are shown separately. Jupiter (large black circle) is centered and Io (white, behind Jupiter) and Europa (black) are shown by the smaller disks to the right (west of Jupiter). The densities are higher closer to the moons (here, west of Jupiter) and the HST/COS observations scanned over the densest regions of the Europa-genic neutrals from 8.0 RJ to 12.5 RJ. (Note that the viewing geometry in Figure 1 corresponds to an 1.5 hr earlier exposure).
Paper: Constraints on Europa’s Water Group Torus from HST/COS Observations
Authors: Lorenz Roth, H. Todd Smith, Kazuo Yoshioka, Tracy M. Becker, Aljona Blöcker, Nathaniel J. Cunningham, Nickolay Ivchenko, Kurt D. Retherford, Joachim Saur, Michael Velez, Fuminori Tsuchiya
Figure caption: Spectra of TORUS-A position (8.0 RJ, le2o55010) from 2021 corrected with the TORUS-E spectra showing detector segment A (top) and segment B (bottom) as in Figure 3. Emission lines with significant brightnesses are detected near 1415 Å (top), 1198 Å, and 1255 Å (bottom) and identified as sulfur ion emission from Io’s torus (e.g., Steffl et al. 2004). The red shaded areas show the integration region for the ion multiplets, covering the brightest lines, and the total brightnesses with errors are stated in red. Our best-fit modeled sulfur ion emissions are shown in red. The brightness around the H Lyα line is off the scale and not shown (gray box).
Paper: Constraints on Europa’s Water Group Torus from HST/COS Observations
Authors: Lorenz Roth, H. Todd Smith, Kazuo Yoshioka, Tracy M. Becker, Aljona Blöcker, Nathaniel J. Cunningham, Nickolay Ivchenko, Kurt D. Retherford, Joachim Saur, Michael Velez, Fuminori Tsuchiya
Figure caption: Spectra of TORUS-C position (9.3 R J) from 2020 (top; le2oa1010) and from 2021 (bottom; le2o54010) corrected with TORUS-E spectra taken directly before and after, respectively (Table 1). The signal is shown in black, the propagated error in gray. The shaded regions show the integration boundaries for the emission brightnesses at the oxygen O I 1304 Å and O I 1356 Å lines. The modeled sulfur ion emissions at 9.3 R J shown by the red peaks around 1410 Å would not be detectable. The integrated brightnesses are stated in blue with propagated uncertainties, revealing no emissions above statistical fluctuations.
Paper: Constraints on Europa’s Water Group Torus from HST/COS Observations
Authors: Lorenz Roth, H. Todd Smith, Kazuo Yoshioka, Tracy M. Becker, Aljona Blöcker, Nathaniel J. Cunningham, Nickolay Ivchenko, Kurt D. Retherford, Joachim Saur, Michael Velez, Fuminori Tsuchiya
Figure caption: Count rates over the exposures in 20 s bins show the variation of geocorona emissions at O I 1304 Å, H I 1216 Å (Lyα), and NI 1200 Å. The red shaded area shows the intervals used for the H I Lyα analysis; the blue shaded areas are the intervals used for the neutral oxygen and sulfur ion analysis.
Paper: Constraints on Europa’s Water Group Torus from HST/COS Observations
Authors: Lorenz Roth, H. Todd Smith, Kazuo Yoshioka, Tracy M. Becker, Aljona Blöcker, Nathaniel J. Cunningham, Nickolay Ivchenko, Kurt D. Retherford, Joachim Saur, Michael Velez, Fuminori Tsuchiya
Figure caption: (Top) Integrated H Lyα brightnesses from the six HST/COS exposures from 2020 shown at the observing time in UTC. The vertical extent of the boxes indicates the statistical uncertainties (σ ∼ 8 R), the width of the box illustrates the length of the exposures (750 s each). (Bottom) Normalized Lyα flux measured by TIMED/SEE. The vertical scales cover similar ranges of ±8% around the mean brightness, which illustrates that the variance in HST/COS data is similar to the variance in the solar flux (as measured by TIMED/SEE), thus not requiring nor indicating emissions from the torus or other sources.
Paper: Erratum: “Reduced Atmospheres of Post-impact Worlds: The Early Earth” (2022, PSJ, 3, 115) 
Authors: Jonathan P. Itcovitz, Auriol S. P. Rae, Robert I. Citron, Sarah T. Stewart, Catriona A. Sinclair, Paul B. Rimmer, Oliver Shorttle
Figure caption:                         H2 abundances, atmospheric fO2, and melt phase fO2 as a function of impactor mass. Results for both the peridotitic (P) and basaltic (B) melt phases are shown. The results for the Fiducial Model (1A) are shown in all panels for comparison (dotted). Comparable results from Zahnle et al. (2020) are also shown in all panels (squares). For each of the other models shown in Figure 6 and detailed in Section 5.2, the post-impact (dashed) and post-equilibration (solid) results are also shown. The standard values of Table 1 are used for all parameters except for the impactor mass in all cases. The standard impactor mass is indicated by the vertical line for each model.
Paper: Erratum: “Reduced Atmospheres of Post-impact Worlds: The Early Earth” (2022, PSJ, 3, 115) 
Authors: Jonathan P. Itcovitz, Auriol S. P. Rae, Robert I. Citron, Sarah T. Stewart, Catriona A. Sinclair, Paul B. Rimmer, Oliver Shorttle
Figure caption: The state of the system at the post-impact stage as a function of impactor mass in Model 3A. All model parameters except for the varying impactor mass are the standard values detailed in Table 1. (a) Composition of the atmosphere with (circles) and without (crosses) the final processing step of local thermochemical equilibrium (LTE). (b) Partial pressures of the three main species in the atmosphere, and total atmospheric pressure. (c) Oxygen fugacities of the atmosphere, basaltic melt, and peridotitic melt. The FMQ and iron wüstite (IW) buffers are shown for reference (dotted lines). (d) Metallic iron remaining in the melt pool after metal saturation has been reached for each melt phase composition. Appendix C contains a similar figure for Model 3B.
Paper: Erratum: “Reduced Atmospheres of Post-impact Worlds: The Early Earth” (2022, PSJ, 3, 115) 
Authors: Jonathan P. Itcovitz, Auriol S. P. Rae, Robert I. Citron, Sarah T. Stewart, Catriona A. Sinclair, Paul B. Rimmer, Oliver Shorttle
Figure caption: Ferric-to-iron ratio (Fe3 + /∑Fe) as a function of impactor mass for the impact-generated melt phase at melt-atmosphere equilibrium (dashed), the remainder of the target mantle that is unmelted (dotted), and the combined bulk mantle (solid). The corresponding fO2 of the melt phase is also shown relative to the FMQ buffer (red). Results are shown for both Models 3A and 3B.
Paper: Stereophotoclinometry on the OSIRIS-REx Mission: Mathematics and Methods
Authors: R. W. Gaskell, O. S. Barnouin, M. G. Daly, E. E. Palmer, J. R. Weirich, C. M. Ernst, R. T. Daly, D. S. Lauretta
Figure caption: Definition of spacecraft–object ( V  0), maplet ( V ), and camera orientation ( C    x  ,  C    y  , and  C    z  ) vectors. Here  W  is the spacecraft–surface vector, and O is the origin of the body-fixed reference frame.
Paper: Stereophotoclinometry on the OSIRIS-REx Mission: Mathematics and Methods
Authors: R. W. Gaskell, O. S. Barnouin, M. G. Daly, E. E. Palmer, J. R. Weirich, C. M. Ernst, R. T. Daly, D. S. Lauretta
Figure caption: Bennu’s south pole modeled using SPC only (a) and with the combined SPCOLA technique using mapolas for constraining heights (b). The smooth areas seen in the SPC model show more relief when the OLA data are included, primarily because images of Bennu’s south pole are poorly illuminated, as illustrated in panel (c), where the model in panel (b) is viewed using current lighting conditions on Bennu. On average, differences between the two products are fairly small (<0.2 m). The addition of OLA removes smooth aprons around rocks and models the tops of rocks better, as seen in the difference map (panel (d)). Bennu products using SPC or OLA only are compared in detail in Al Asad et al. (2021) and not shown here. But differences between OLA and SPC are usually smaller than those seen between panels (a) and (b), shown here, mostly because the lighting conditions are better elsewhere on the asteroid.
Paper: Stereophotoclinometry on the OSIRIS-REx Mission: Mathematics and Methods
Authors: R. W. Gaskell, O. S. Barnouin, M. G. Daly, E. E. Palmer, J. R. Weirich, C. M. Ernst, R. T. Daly, D. S. Lauretta
Figure caption: The SPC and OLA bigmaps used to improve navigation and global size. From left to right: bigmap from SPC, OLA point cloud coverage, and bigmap from OLA vectors. The OLA point cloud is viewed looking vertically down onto the surface shown on the right and left.
Paper: Stereophotoclinometry on the OSIRIS-REx Mission: Mathematics and Methods
Authors: R. W. Gaskell, O. S. Barnouin, M. G. Daly, E. E. Palmer, J. R. Weirich, C. M. Ernst, R. T. Daly, D. S. Lauretta
Figure caption: Anaglyph of SPC-determined trajectory for the OSIRIS-REx sample collection operations.
Paper: Stereophotoclinometry on the OSIRIS-REx Mission: Mathematics and Methods
Authors: R. W. Gaskell, O. S. Barnouin, M. G. Daly, E. E. Palmer, J. R. Weirich, C. M. Ernst, R. T. Daly, D. S. Lauretta
Figure caption: The ICQ labels (q = 4) and a similarly connected shape model.
Paper: Stereophotoclinometry on the OSIRIS-REx Mission: Mathematics and Methods
Authors: R. W. Gaskell, O. S. Barnouin, M. G. Daly, E. E. Palmer, J. R. Weirich, C. M. Ernst, R. T. Daly, D. S. Lauretta
Figure caption: Local DTM or maplet defining various SPC parameters.
Paper: Stereophotoclinometry on the OSIRIS-REx Mission: Mathematics and Methods
Authors: R. W. Gaskell, O. S. Barnouin, M. G. Daly, E. E. Palmer, J. R. Weirich, C. M. Ernst, R. T. Daly, D. S. Lauretta
Figure caption: Initial Bennu shape model constructed from approach limb data.
Paper: Stereophotoclinometry on the OSIRIS-REx Mission: Mathematics and Methods
Authors: R. W. Gaskell, O. S. Barnouin, M. G. Daly, E. E. Palmer, J. R. Weirich, C. M. Ernst, R. T. Daly, D. S. Lauretta
Figure caption: Summary of the projection of a reference maplet onto a new maplet.
Paper: OSSOS. XXVII. Population Estimates for Theoretically Stable Centaurs between Uranus and Neptune
Authors: Rosemary C. Dorsey, Michele T. Bannister, Samantha M. Lawler, Alex H. Parker
Figure caption: Excitation parameter values (Equation (3)) for the initial states of the Zhang & Gladman (2022) stable Centaur particles (gray) and the combined particle outputs from three planetary migration simulations (green; Nesvorný et al. simulations).
Paper: Stereophotoclinometry for OSIRIS-REx Spacecraft Navigation
Authors: Coralie D. Adam, Leilah K. McCarthy, Jason M. Leonard, Robert Gaskell, Peter G. Antreasian, Andrew J. Liounis, Kenneth Getzandanner, Michael C. Moreau, Eric E. Palmer, John Weirich, Olivier S. Barnouin, Jeroen L. Geeraert, Eric M. Sahr, Benjamin Ashman, Derek S. Nelson, John Y. Pelgrift, Erik J. Lessac-Chenen, Daniel Wibben, Bobby G. Williams, Michael G. Daly, Dante S. Lauretta
Figure caption: Orbital A pass-through (px,ln) landmark residuals for SPC v14, in units of pixels. The pixel and line mean residuals are 0.37 px and 0.27 px, with standard deviations of 1.37 px and 1.26 px, respectively. The purple and green dashed lines, respectively, represent the required 1σ (standard deviation) and 3σ uncertainties to meet the navigation performance requirements.
Paper: Stereophotoclinometry for OSIRIS-REx Spacecraft Navigation
Authors: Coralie D. Adam, Leilah K. McCarthy, Jason M. Leonard, Robert Gaskell, Peter G. Antreasian, Andrew J. Liounis, Kenneth Getzandanner, Michael C. Moreau, Eric E. Palmer, John Weirich, Olivier S. Barnouin, Jeroen L. Geeraert, Eric M. Sahr, Benjamin Ashman, Derek S. Nelson, John Y. Pelgrift, Erik J. Lessac-Chenen, Daniel Wibben, Bobby G. Williams, Michael G. Daly, Dante S. Lauretta
Figure caption: Estimated global altitude corrections in the landmark vectors associated with (a) the AltWG SPC v18 model, and (b) the JPL jpl_181231 model.
Paper: Stereophotoclinometry for OSIRIS-REx Spacecraft Navigation
Authors: Coralie D. Adam, Leilah K. McCarthy, Jason M. Leonard, Robert Gaskell, Peter G. Antreasian, Andrew J. Liounis, Kenneth Getzandanner, Michael C. Moreau, Eric E. Palmer, John Weirich, Olivier S. Barnouin, Jeroen L. Geeraert, Eric M. Sahr, Benjamin Ashman, Derek S. Nelson, John Y. Pelgrift, Erik J. Lessac-Chenen, Daniel Wibben, Bobby G. Williams, Michael G. Daly, Dante S. Lauretta
Figure caption: Orbital A pass-through (px,ln) landmark residuals for SPC v18, in units of pixels. The sample/line mean residuals are 0.37 px and 0.077 px, with standard deviations of 0.73 px and 0.54 px, respectively. The purple and green dashed lines, respectively, represent the required 1σ (standard deviation) and 3σ uncertainties to meet the navigation performance requirements.
Paper: Stereophotoclinometry for OSIRIS-REx Spacecraft Navigation
Authors: Coralie D. Adam, Leilah K. McCarthy, Jason M. Leonard, Robert Gaskell, Peter G. Antreasian, Andrew J. Liounis, Kenneth Getzandanner, Michael C. Moreau, Eric E. Palmer, John Weirich, Olivier S. Barnouin, Jeroen L. Geeraert, Eric M. Sahr, Benjamin Ashman, Derek S. Nelson, John Y. Pelgrift, Erik J. Lessac-Chenen, Daniel Wibben, Bobby G. Williams, Michael G. Daly, Dante S. Lauretta
Figure caption: Observed landmark line-coordinate residual trends compared to potential correlated sources. The black curves represent the running mean of the data, and the cyan curves represent 1, 2, and 3σ standard deviations of the data using a rolling standard deviation algorithm. Histograms showing the distribution of data points are included above and next to the figures (Leonard et al. 2020a).
Paper: Stereophotoclinometry for OSIRIS-REx Spacecraft Navigation
Authors: Coralie D. Adam, Leilah K. McCarthy, Jason M. Leonard, Robert Gaskell, Peter G. Antreasian, Andrew J. Liounis, Kenneth Getzandanner, Michael C. Moreau, Eric E. Palmer, John Weirich, Olivier S. Barnouin, Jeroen L. Geeraert, Eric M. Sahr, Benjamin Ashman, Derek S. Nelson, John Y. Pelgrift, Erik J. Lessac-Chenen, Daniel Wibben, Bobby G. Williams, Michael G. Daly, Dante S. Lauretta
Figure caption: Orbital A pass-through (px,ln) landmark residuals for SPC v20, in units of pixels. The sample/line mean residuals are both −0.01 px, with standard deviations of 0.61 px and 0.41 px, respectively. The purple and green dashed lines, respectively, represent the required 1σ (standard deviation) and 3σ uncertainties to meet the navigation performance requirements.
Paper: Stereophotoclinometry for OSIRIS-REx Spacecraft Navigation
Authors: Coralie D. Adam, Leilah K. McCarthy, Jason M. Leonard, Robert Gaskell, Peter G. Antreasian, Andrew J. Liounis, Kenneth Getzandanner, Michael C. Moreau, Eric E. Palmer, John Weirich, Olivier S. Barnouin, Jeroen L. Geeraert, Eric M. Sahr, Benjamin Ashman, Derek S. Nelson, John Y. Pelgrift, Erik J. Lessac-Chenen, Daniel Wibben, Bobby G. Williams, Michael G. Daly, Dante S. Lauretta
Figure caption: Landmark residual errors plotted as a function of a priori spacecraft position error magnitude. The sample and line mean residuals are zero-mean, with standard deviations of 0.018 px and 0.015896 px, respectively (McCarthy et al. 2022a).
Paper: Stereophotoclinometry for OSIRIS-REx Spacecraft Navigation
Authors: Coralie D. Adam, Leilah K. McCarthy, Jason M. Leonard, Robert Gaskell, Peter G. Antreasian, Andrew J. Liounis, Kenneth Getzandanner, Michael C. Moreau, Eric E. Palmer, John Weirich, Olivier S. Barnouin, Jeroen L. Geeraert, Eric M. Sahr, Benjamin Ashman, Derek S. Nelson, John Y. Pelgrift, Erik J. Lessac-Chenen, Daniel Wibben, Bobby G. Williams, Michael G. Daly, Dante S. Lauretta
Figure caption: SPC v42 landmark residuals in (a) pixel, and (b) line directions, plotted over emission, illumination, and solar phase angle.
Paper: Stereophotoclinometry for OSIRIS-REx Spacecraft Navigation
Authors: Coralie D. Adam, Leilah K. McCarthy, Jason M. Leonard, Robert Gaskell, Peter G. Antreasian, Andrew J. Liounis, Kenneth Getzandanner, Michael C. Moreau, Eric E. Palmer, John Weirich, Olivier S. Barnouin, Jeroen L. Geeraert, Eric M. Sahr, Benjamin Ashman, Derek S. Nelson, John Y. Pelgrift, Erik J. Lessac-Chenen, Daniel Wibben, Bobby G. Williams, Michael G. Daly, Dante S. Lauretta
Figure caption: Landmark residuals in (a) pixel, and (b) line directions plotted over SPC correlation score (McCarthy et al. 2022a). The blue histograms represent the relative distribution data points per bin.
Paper: Stereophotoclinometry for OSIRIS-REx Spacecraft Navigation
Authors: Coralie D. Adam, Leilah K. McCarthy, Jason M. Leonard, Robert Gaskell, Peter G. Antreasian, Andrew J. Liounis, Kenneth Getzandanner, Michael C. Moreau, Eric E. Palmer, John Weirich, Olivier S. Barnouin, Jeroen L. Geeraert, Eric M. Sahr, Benjamin Ashman, Derek S. Nelson, John Y. Pelgrift, Erik J. Lessac-Chenen, Daniel Wibben, Bobby G. Williams, Michael G. Daly, Dante S. Lauretta
Figure caption: NTE-3B landmark residuals over emission angle, illumination angle, solar phase angle, latitude, longitude, and distance to surface plotted (a) before and (b) after estimating a body-fixed landmark vector scale error.
Paper: Nuclear and Orbital Characterization of the Transition Object (4015) 107P/Wilson–Harrington
Authors: Theodore Kareta, Vishnu Reddy
Figure caption: The evolution of (4015) 107P/Wilson–Harrington’s nominal orbit from late 2022 backwards 2000 yr in time, as well as the identical propagation of 1000 clones sampled from the covariance matrix of its orbital fit (JPL 282). Despite Wilson–Harrington’s very near-Earth perihelion and low inclination, its orbit is remarkably stable over the time period—including no phases as a near-Sun object like some other dormant comets that might correlate with altered surface reflective properties from intense heating (Kareta et al. 2021a). Integrations further backwards in time continued to chaotically diverge but showed no obvious trends or close encounters.
Paper: Nuclear and Orbital Characterization of the Transition Object (4015) 107P/Wilson–Harrington
Authors: Theodore Kareta, Vishnu Reddy
Figure caption: The combined visible/near-infrared reflectance spectrum of 107P/Wilson–Harrington (black) is compared against the closest spectral matches in the RELAB database (Pieters 1983), the insoluble organic material (IOM) from the CM Chondrite Murchison (orange), a sample of the C I Ivuna after it had been heated to 300° Celsius (gray), and the Ungrouped C3 chondrite MAC 88107 (blue). Murchison’s IOM is the best fit spectrally, while MAC 88107 is the best match in albedo.
Paper: Mercury’s Hidden Past: Revealing a Volatile-dominated Layer through Glacier-like Features and Chaotic Terrains
Authors: J. Alexis P. Rodriguez, Deborah Domingue, Bryan Travis, Jeffrey S. Kargel, Oleg Abramov, Mario Zarroca, Maria E. Banks, John Weirich, Anthony Lopez, Nicholas Castle, Yan Jianguo, Frank Chuang
Figure caption: The image delineates the varied behavior of halite under differing viscosity conditions during simulations. When the viscosity is elevated, the resultant flow exhibits a sharp leading edge, as depicted in the figure. The profiles illustrate the interrelation between flow thickness and runout length at discrete temporal junctures. The corresponding times (t  i ) depend on the initial internal temperature of the flowing layer. Given an initial internal temperature approximating 400 °C, falling within the 300 °C–500 °C range inferred from the iSALE2D simulations, the timescale (t 4) is estimated to be of the order of 150 yr. Alternatively, if the initial internal temperature approximates 200 °C, mirroring the surface temperature at the conclusion of the iSALE2D simulations, the timescale (t 4) is projected to span roughly 5000 yr. Upon the flowing material entirely vacating the peak ring slope, any ensuing creep flow is anticipated to markedly decelerate.