adsabs/AstroCLIMB huggingface dataset:
Paper: On Ganymede’s Magnetic Quadrupolar Strength
Authors: A. M. Plattner, C. L. Johnson, M. J. Styczinski, S. D. Vance, A. C. Mills
Figure caption: Quadrupole-to-dipole ratio (Q/D) at 0.25r  G  for linear combinations of models L2A– and L2B–, with weights summing to unity.
Paper: On Ganymede’s Magnetic Quadrupolar Strength
Authors: A. M. Plattner, C. L. Johnson, M. J. Styczinski, S. D. Vance, A. C. Mills
Figure caption: Absolute difference of the radial components between (a) models L2A– and L2B–, and (c) models L2B– and L2C–. Flyby ground tracks, denoted by gray lines, are mostly clustered in specific northern regions. The projection is the same as in Figure 1.
Paper: On Ganymede’s Magnetic Quadrupolar Strength
Authors: A. M. Plattner, C. L. Johnson, M. J. Styczinski, S. D. Vance, A. C. Mills
Figure caption: Differences between the spacecraft data and the modeled data in Figure 5 for (a) L2A– and (b) L2B–, shown for flybys G1, G2, G28, and J34.
Paper: Photometric Survey of Neptune's Trojan Asteroids. I. The Color Distribution
Authors: Larissa Markwardt, Hsing Wen Lin, 省文 林, David Gerdes, Fred C. Adams
Figure caption: NT colors as a function of absolute magnitude. Gray points are taken from the literature (Sheppard & Trujillo 2006; Sheppard 2012; Parker et al. 2013; Jewitt 2018; Lin et al. 2019; Schwamb et al. 2019). Colored squares were measured in this paper. Duplicate observations of the same object are connected by dashed lines. The inset plots contain histograms of the cluster indices and Pearson correlation coefficients of a random distribution of colors and absolute magnitude (see Section 4.1). Each gray dashed line in the inset plots shows the corresponding value calculated for the observed distribution.
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 prefit (a) and postfit (b) observed landmark residuals in the NavCam pixel and line directions. The 1σ and 3σ weightings, computed by Equation (1), provide reference for the objective statistical performance.
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 residual standard deviation contour map (a), in units of pixels, and landmark position estimate contour map (b), in units of meters. The colorized contours represent the estimated magnitude of the three-component correction, as well as arrows showing tangential corrections.
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: Navigation campaign timeline denoting key events and science imaging. Credit: University of Arizona, adapted by the authors.
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: F5 SPC end-to-end test trajectory result compared to truth. The red lines represent the position errors in the radial-transverse-normal frame, and the blue lines represent the 1σ reconstructed uncertainties leading up to the data cutoff (DCO).
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 example simulated image from Orbital A, displaying (a) rendered landmark DTMs in even rows compared against ortho-rectified image data in odd rows, and (b) the observed landmark locations in the image marked in yellow, landmark names in red, and direction of the residual in purple.
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: Magnitude of OD position errors during OPIE-2 iterations, compared to NTE-2 center-finding OD errors.
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: Data flow, SPC subroutines, and ancillary tools. Data files are shaded red and software tools are shaded yellow.
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-3A operational test flow.
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 operational test flow.
Paper: Effects of the Librationally Induced Flow in Mercury’s Fluid Core with an Outer Stably Stratified Layer
Authors: Fleur Seuren, Santiago A. Triana, Jérémy Rekier, Ankit Barik, Tim Van Hoolst
Figure caption: Same as Figure 15 but for comparison case 2 with a stably stratified layer.
Paper: Fitting Thermal Evolution Models to the Chronological Record of Erg Chech 002 and Modeling the Ejection Conditions of the Meteorite
Authors: Wladimir Neumann, Robert Luther, Mario Trieloff, Philip M. Reger, Audrey Bouvier
Figure caption: Left column: both the color bar and isolines show fit quality as a function of planetesimal radius R and accretion time t 0 for EC 002 resulting from a fit of thermochronological data without Ar–Ar, Mn–Cr, and Al–Mg ages (top row) or without Mn–Cr and Al–Mg ages but including Ar–Ar age (bottom row). Right column: thermal evolution at the fit depth of EC 002 for best-fit parent bodies indicated by red circles in the left column. Best-fit accretion times correspond to <0.2 Ma (top) and <0.3 Ma (bottom). The best-fit radius range is constrained quite well (20–30 km) for the top row and less well (>150 km) for the bottom row. The exemplary parent bodies from the respective minimum fit quality regions with R = 20 km and t 0 = 0.1 Ma as well as R = 200 km and t 0 = 0.1 Ma are indicated with red circles. Both Al–Mg ages (not used for the fit) are placed directly on the temperature curves. Suggested closure temperatures are ≈1160–1180 K for t  c  = 1.83 Ma and ≈1030–1080 K for t  c  = 2.29 Ma. Mn–Cr ages (not used for the fit) are fixed at a closure temperature of 950 K; see Table 1.
Paper: Fitting Thermal Evolution Models to the Chronological Record of Erg Chech 002 and Modeling the Ejection Conditions of the Meteorite
Authors: Wladimir Neumann, Robert Luther, Mario Trieloff, Philip M. Reger, Audrey Bouvier
Figure caption: Evolution of the temperature (left panel) and of the silicate volume fraction (right panel) for the preferred best-fit parent body with a radius of 20 km and an accretion time of 0.1 Ma (case (a)). The metal fraction is equal to 1 minus the silicate fraction. The chronological data points (symbols; see Table 1), the onset of melting (1213 K isoline in the right panel), and the core–mantle boundary and the layering depth of EC 002 (dashed lines) are shown for comparison.
Paper: Fitting Thermal Evolution Models to the Chronological Record of Erg Chech 002 and Modeling the Ejection Conditions of the Meteorite
Authors: Wladimir Neumann, Robert Luther, Mario Trieloff, Philip M. Reger, Audrey Bouvier
Figure caption: Left: density vs. relative depth profiles after differentiation and cooling (solid lines) and layering depths fitted (dashed lines). Right: the extension and evolution of the magma ocean (areas bounded by solid lines) as a function of time and relative depth. Layering depths (dashed lines) and upper boundaries of the magma oceans at maximum extension (dotted lines) indicate that melts from a magma ocean likely did not participate in the genesis of the EC 002 material.
Paper: Fitting Thermal Evolution Models to the Chronological Record of Erg Chech 002 and Modeling the Ejection Conditions of the Meteorite
Authors: Wladimir Neumann, Robert Luther, Mario Trieloff, Philip M. Reger, Audrey Bouvier
Figure caption: Times of reaching selected temperatures (blues lines), relative normalized fit qualities (black lines), and maximum temperatures at fit depths (red lines) as functions of the accretion time. Two exemplary bodies from Figure 1 with R = 20 km (upward-pointing triangles) and R = 200 km (downward-pointing triangles) are considered. For these two bodies, the times at which T = 1460 K is reached for the first time and the times at which the maximum temperature is reached at the fit depth are within 50,000 yr from each other (thus, blue lines stand for both radii). The relative normalized fit quality is shown for fixed radii and varying accretion time and calculated from χ  n  (Figure 1) by dividing by the maximum value of 10.5 obtained within 1 Ma after CAIs. It varies between 0 and 1, but the figure does not provide a scaling. The maximum temperatures at fit depth are similar to identical for early accretion but distinct after t 0 = 0.9 Ma.
Paper: Fitting Thermal Evolution Models to the Chronological Record of Erg Chech 002 and Modeling the Ejection Conditions of the Meteorite
Authors: Wladimir Neumann, Robert Luther, Mario Trieloff, Philip M. Reger, Audrey Bouvier
Figure caption: Accretion times of parent bodies of some achondritic and primitive achondritic meteorites (colored patches) derived from model fits to meteorite chronology (data points and text statements). The accretion times and thermochronological data are from this study (EC 002), Kleine et al. (2020) and Neumann et al. (2018b) (magmatic iron meteorites), Neumann et al. (2014b) (HED meteorites/Vesta), Budde et al. (2015) (ureilites), Kleine et al. (2012) and Schiller et al. (2016) (angrites), Neumann et al. (2018a) (acapulcoites–lodranites), Neumann et al. (2023) (NWA 011 and NWA 6704), and Ma et al. (2022) (tafassites). The data points are derived from the following chronometers: Hf–W (left-pointing triangles), Mn–Cr (right-pointing triangles), U–Pb–Pb (squares), Al–Mg (circles), I–Xe (upward-pointing triangles), Ar–Ar (downward-pointing triangles), U–Th–He (star), and Pu fission tracks (diamond). For the data, see Table 1 (EC 002) and papers cited (all other meteorites).
Paper: Fitting Thermal Evolution Models to the Chronological Record of Erg Chech 002 and Modeling the Ejection Conditions of the Meteorite
Authors: Wladimir Neumann, Robert Luther, Mario Trieloff, Philip M. Reger, Audrey Bouvier
Figure caption: Initial position of ejected projectile and target material for an impact velocity of 500 m s−1 (left panel) and 5000 m s−1 (right panel). The projectile radius a is specified in the legend for all cases.
Paper: Fitting Thermal Evolution Models to the Chronological Record of Erg Chech 002 and Modeling the Ejection Conditions of the Meteorite
Authors: Wladimir Neumann, Robert Luther, Mario Trieloff, Philip M. Reger, Audrey Bouvier
Figure caption: Ejected material. The launch velocities in radial direction (panels (a) and (c)) and peak pressure (panels (b) and (d)) by which the material was affected are plotted against the depth from where the material originates for the two impact velocities of 500 m s−1 (panels (a) and (b)) and 5000 m s−1 (panels (c) and (d)). Black dashed vertical lines indicate the depth of excavation to reach the formation depth of EC 002. Horizontal dotted lines indicate the escape velocity of the body. Colors correspond to the different projectile radii.
Paper: Fitting Thermal Evolution Models to the Chronological Record of Erg Chech 002 and Modeling the Ejection Conditions of the Meteorite
Authors: Wladimir Neumann, Robert Luther, Mario Trieloff, Philip M. Reger, Audrey Bouvier
Figure caption: Sketches of hypothetical extreme cooling scenarios compared with the best-fit temperature curve. The arrows are colored according to the data points in lime green (quasi-instantaneous cooling), teal (slow cooling, late boundary of the U–Pb–Pb phosphate data range), and yellow (very slow cooling, late boundary of the Ar–Ar data range).
Paper: Titania's Heat Fluxes Revealed by Messina Chasmata
Authors: Chloe B. Beddingfield, Erin J. Leonard, Tom A. Nordheim, Richard J. Cartwright, Julie C. Castillo-Rogez
Figure caption: Annotated and modified version of the geologic map of Titania’s imaged southern hemisphere (Croft & Soderblom 1991). Our study area location is shown by the yellow box. The Plains Materials include the following units: Pb: bright slope material; Ps: smooth plains; Pm: moderately cratered plains; and Ph: heavily cratered plains. The Crater Materials include the following: C3: rayed/bright deposit craters; C2: fresh appearing, no rays; C1: moderately degraded craters; Ce: elongate craters (possibly secondaries); Cr: crater rim massifs; and Cf: crater floor material. Points B–E indicate locations of limb profiles analyzed by Thomas (1988).
Paper: Titania's Heat Fluxes Revealed by Messina Chasmata
Authors: Chloe B. Beddingfield, Erin J. Leonard, Tom A. Nordheim, Richard J. Cartwright, Julie C. Castillo-Rogez
Figure caption: A map-projected portion of Voyager 2 ISS image c2684313, and the associated DEM that we created of our study area (see Appendix A.1 for additional information). South is down, and the white squares are removed reseau points.
Paper: Titania's Heat Fluxes Revealed by Messina Chasmata
Authors: Chloe B. Beddingfield, Erin J. Leonard, Tom A. Nordheim, Richard J. Cartwright, Julie C. Castillo-Rogez
Figure caption: Voyager 2 ISS image c2684313 (2.88 km pixel−1) showing major geologic features on Titania (Titania’s diameter (D): 1578 km). Blue stars indicate the centers of craters mapped in Croft & Soderblom (1991) (Figure 2). Black filled circles are reseau points.
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: This illustration presents a perspective view of the Raditladi impact crater basin. The left half of the image reveals the subsurface temperature distribution right after the impact, as projected by the iSALE2D hydrocode simulation of the crater’s formation. In contrast, the right half reveals the stratigraphic makeup of the impact-excavated upper section, comprising a 2 km thick VRL surmounting a multi-kilometer-thick volcanic crust. Note that the peak ring region (highlighted in red boxes in panels (A) and (B)) emerges as a distinctive area, marked by a synergy of high relief and the outermost confines of the impact-triggered thermal disturbance (as further detailed in simulation close-ups (B) and (C)).
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: (A) View portraying the BC landscape, characterized by its segmentation of heavily cratered terrains. Notice the similarly degraded craters of varying diameters (10–160 km) exhibiting rim discontinuities (arrows 1–3). The dashed curve traces the location of the profile Z–Z′. (B) A close-up of BC’s floor reveals a crater-saturated surface, including notably degraded craters morphing into irregular depressions (feature 1). Larger irregular depressions (feature 2) and even more extensive plains with enclosed mesas consisting of heavily cratered plateau residues (feature 3) can also be seen. A regionally consistent topographic base around −4000 m indicates the interface between a regional VRL and the gravity-detected cratered, lava-covered paleosurface (refer to Figure 7). Data source: both panels consist of a MESSENGER Mercury global DEM (∼665 m px−1) draped over a MESSENGER MDIS global base map (∼166 m px−1; courtesy of NASA/JPL/GSFC).
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: Illustrative diagrams depicting key geological scenarios: (A) Gravity data (Qingyun et al. 2018) reveals the presence of an ancient cratered terrain, which we propose to have been overlain by a global VRL. This panel shows a cross-sectional view of this stratigraphy along a longitudinal reconstruction spanning from the equator to the north pole. (B) Extensive areas of the VRL are concealed beneath basalts, while the VRL remains exposed in the north polar region. (C) Impact events on the basaltic surface result in crater formation and the exhumation of buried VRL materials. Craters are also observed in the north polar area. (D) The exhumed VRL material flows and gives rise to glacier-like lobate features. The north polar region undergoes collapse, leading to the degradation or elimination of most craters.
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 depicted above, taken by NASA’s orbital MESSENGER spacecraft, underscores the faint blue shade (here in exaggerated color contrast) of unique geological formations termed “hollows” on Mercury. Mercury’s landscape is punctuated by impact craters consisting of bowl-shaped depressions, each typically accentuated by raised rims and accompanying ejecta blankets. In stark contrast, hollows emerge as irregular, pit-like structures, their steep walls descending into flat or gently sloping floors. An unmistakable feature of these hollows is the surrounding bright halos, a characteristic that sets them distinctly apart from craters, as they notably lack the common traits of raised rims and ejecta blankets. The showcased image offers a detailed view of a 40 km segment of the Raditladi impact basin’s base, featuring its striking central peak mountains. Image Credit: NASA/JHU APL/CIW.
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: Comparative Perspectives of Different Glacier Types—Raditlati’s lobe presumed to be a halite glacier (A), a debris-covered Martian ice glacier (B) at coordinates 102°58′E, 40°36′S, and a salt glacier in Iran’s Zagros Mountains (C) at coordinates 54°54′E, 27°59′N. The white and red arrows distinctly point toward the originating mountains and their respective lobate glacier fronts.
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: iSALE2D hydrocode model incorporating a dunite crust—A potential superior match to basalt, assuming that Mercury’s crust shares closer thermal and physical characteristics with komatiites. Observe that the peak ring area, approximately 60 km from the center, continues to harbor VRL materials. (a) Snapshot at 30 s post-impact, illustrating the maximum depth achieved. (b) Frame at 170 s, depicting the ejecta curtain encapsulating the overturned stratigraphy. (c) Image at 300 s showcasing the formation of a transient central peak and ejecta blanket. (d) Final visualization at 700 s (see also Figure 9(A)).
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: Implementation of iSALE2D hydrocode model with enhanced initial VRL—This model features a considerably thickened VRLr, extending to a depth of 11 km. Note the preservation of VRL constituents within the peak ring, located approximately 60 km from the central point. (a) Snapshot at 30 s post-impact, illustrating the maximum depth achieved. (b) Frame at 170 s, depicting the ejecta curtain encapsulating the overturned stratigraphy. (c) Image at 300 s showcasing the formation of a transient central peak and ejecta blanket. (d) Final visualization at 700 s (see also Figure 9(A)).
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: Sequential representation of iSALE2D hydrocode model results. (a) Snapshot at 30 s post-impact, illustrating the maximum depth achieved. (b) Frame at 170 s, depicting the ejecta curtain encapsulating the overturned stratigraphy. (c) Image at 300 s showcasing the formation of a transient central peak and ejecta blanket. (d) Final visualization at 700 s (see also Figure 9(A)).