adsabs/AstroCLIMB huggingface dataset:
Paper: OSIRIS-APEX: An OSIRIS-REx Extended Mission to Asteroid Apophis
Authors: Daniella N. DellaGiustina, Michael C. Nolan, Anjani T. Polit, Michael C. Moreau, Dathon R. Golish, Amy A. Simon, Coralie D. Adam, Peter G. Antreasian, Ronald-Louis Ballouz, Olivier S. Barnouin, Kris J. Becker, Carina A. Bennett, Richard P. Binzel, Brent J. Bos, Richard Burns, Nayessda Castro, Steven R. Chesley, Philip R. Christensen, M. Katherine Crombie, Michael G. Daly, R. Terik Daly, Heather L. Enos, Davide Farnocchia, Sandra Freund Kasper, Rose Garcia, Kenneth M. Getzandanner, Scott D. Guzewich, Christopher W. Haberle, Timothy Haltigin, Victoria E. Hamilton, Karl Harshman, Noble Hatten, Kyle M. Hughes, Erica R. Jawin, Hannah H. Kaplan, Dante S. Lauretta, Jason M. Leonard, Andrew H. Levine, Andrew J. Liounis, Christian W. May, Laura C. Mayorga, Lillian Nguyen, Lynnae C. Quick, Dennis C. Reuter, Edgard Rivera-Valentín, Bashar Rizk, Heather L. Roper, Andrew J. Ryan, Brian Sutter, Mathilde M. Westermann, Daniel R. Wibben, Bobby G. Williams, Kenneth Williams, C. W. V. Wolner
Figure caption: The capabilities of the APEX spacecraft and cameras offer an unprecedented combination of global coverage and subcentimeter resolution. For each mission, the points mark the approximate fraction of the surface covered at high resolution and the ground sample distance at which that area was covered. Note that NEA missions have surveyed portions of their targets at higher resolution. At Apophis we anticipate that resolution and coverage will be slightly lower than at Bennu because (a) OLA's highest-resolution laser (LELT) is no longer functioning and (b) Apophis’s slow rotation and higher albedo require different observing modes than OREx used at Bennu.
Paper: OSIRIS-APEX: An OSIRIS-REx Extended Mission to Asteroid Apophis
Authors: Daniella N. DellaGiustina, Michael C. Nolan, Anjani T. Polit, Michael C. Moreau, Dathon R. Golish, Amy A. Simon, Coralie D. Adam, Peter G. Antreasian, Ronald-Louis Ballouz, Olivier S. Barnouin, Kris J. Becker, Carina A. Bennett, Richard P. Binzel, Brent J. Bos, Richard Burns, Nayessda Castro, Steven R. Chesley, Philip R. Christensen, M. Katherine Crombie, Michael G. Daly, R. Terik Daly, Heather L. Enos, Davide Farnocchia, Sandra Freund Kasper, Rose Garcia, Kenneth M. Getzandanner, Scott D. Guzewich, Christopher W. Haberle, Timothy Haltigin, Victoria E. Hamilton, Karl Harshman, Noble Hatten, Kyle M. Hughes, Erica R. Jawin, Hannah H. Kaplan, Dante S. Lauretta, Jason M. Leonard, Andrew H. Levine, Andrew J. Liounis, Christian W. May, Laura C. Mayorga, Lillian Nguyen, Lynnae C. Quick, Dennis C. Reuter, Edgard Rivera-Valentín, Bashar Rizk, Heather L. Roper, Andrew J. Ryan, Brian Sutter, Mathilde M. Westermann, Daniel R. Wibben, Bobby G. Williams, Kenneth Williams, C. W. V. Wolner
Figure caption: Top: false-color map of Bennu from MapCam (DellaGiustina et al. 2020). Bottom: spectra of S-complex asteroids (http://smass.mit.edu/catalog.php) and Bennu (DellaGiustina et al. 2020) sampled at the four MapCam visible wavelength bands. The bands can discriminate the differences in asteroid surface mineralogy.
Paper: OSIRIS-APEX: An OSIRIS-REx Extended Mission to Asteroid Apophis
Authors: Daniella N. DellaGiustina, Michael C. Nolan, Anjani T. Polit, Michael C. Moreau, Dathon R. Golish, Amy A. Simon, Coralie D. Adam, Peter G. Antreasian, Ronald-Louis Ballouz, Olivier S. Barnouin, Kris J. Becker, Carina A. Bennett, Richard P. Binzel, Brent J. Bos, Richard Burns, Nayessda Castro, Steven R. Chesley, Philip R. Christensen, M. Katherine Crombie, Michael G. Daly, R. Terik Daly, Heather L. Enos, Davide Farnocchia, Sandra Freund Kasper, Rose Garcia, Kenneth M. Getzandanner, Scott D. Guzewich, Christopher W. Haberle, Timothy Haltigin, Victoria E. Hamilton, Karl Harshman, Noble Hatten, Kyle M. Hughes, Erica R. Jawin, Hannah H. Kaplan, Dante S. Lauretta, Jason M. Leonard, Andrew H. Levine, Andrew J. Liounis, Christian W. May, Laura C. Mayorga, Lillian Nguyen, Lynnae C. Quick, Dennis C. Reuter, Edgard Rivera-Valentín, Bashar Rizk, Heather L. Roper, Andrew J. Ryan, Brian Sutter, Mathilde M. Westermann, Daniel R. Wibben, Bobby G. Williams, Kenneth Williams, C. W. V. Wolner
Figure caption: The spacecraft−Apophis relative range and phase angle through close Earth approach on 2029 April 13 (EGA3) through the end of the APEX Approach mission phase. Note that the phase angle remains fairly high for about a week after Apophis's Earth encounter, enhancing the ability to search for small particles. APEX will fly by Apophis on April 22 and then make a series of AAMs to carefully approach to rendezvous in early 2029 June.
Paper: OSIRIS-APEX: An OSIRIS-REx Extended Mission to Asteroid Apophis
Authors: Daniella N. DellaGiustina, Michael C. Nolan, Anjani T. Polit, Michael C. Moreau, Dathon R. Golish, Amy A. Simon, Coralie D. Adam, Peter G. Antreasian, Ronald-Louis Ballouz, Olivier S. Barnouin, Kris J. Becker, Carina A. Bennett, Richard P. Binzel, Brent J. Bos, Richard Burns, Nayessda Castro, Steven R. Chesley, Philip R. Christensen, M. Katherine Crombie, Michael G. Daly, R. Terik Daly, Heather L. Enos, Davide Farnocchia, Sandra Freund Kasper, Rose Garcia, Kenneth M. Getzandanner, Scott D. Guzewich, Christopher W. Haberle, Timothy Haltigin, Victoria E. Hamilton, Karl Harshman, Noble Hatten, Kyle M. Hughes, Erica R. Jawin, Hannah H. Kaplan, Dante S. Lauretta, Jason M. Leonard, Andrew H. Levine, Andrew J. Liounis, Christian W. May, Laura C. Mayorga, Lillian Nguyen, Lynnae C. Quick, Dennis C. Reuter, Edgard Rivera-Valentín, Bashar Rizk, Heather L. Roper, Andrew J. Ryan, Brian Sutter, Mathilde M. Westermann, Daniel R. Wibben, Bobby G. Williams, Kenneth Williams, C. W. V. Wolner
Figure caption: Apophis’s bilobate shape model (Brozović et al. 2018), interpolated to a 15 m facet size.
Paper: OSIRIS-APEX: An OSIRIS-REx Extended Mission to Asteroid Apophis
Authors: Daniella N. DellaGiustina, Michael C. Nolan, Anjani T. Polit, Michael C. Moreau, Dathon R. Golish, Amy A. Simon, Coralie D. Adam, Peter G. Antreasian, Ronald-Louis Ballouz, Olivier S. Barnouin, Kris J. Becker, Carina A. Bennett, Richard P. Binzel, Brent J. Bos, Richard Burns, Nayessda Castro, Steven R. Chesley, Philip R. Christensen, M. Katherine Crombie, Michael G. Daly, R. Terik Daly, Heather L. Enos, Davide Farnocchia, Sandra Freund Kasper, Rose Garcia, Kenneth M. Getzandanner, Scott D. Guzewich, Christopher W. Haberle, Timothy Haltigin, Victoria E. Hamilton, Karl Harshman, Noble Hatten, Kyle M. Hughes, Erica R. Jawin, Hannah H. Kaplan, Dante S. Lauretta, Jason M. Leonard, Andrew H. Levine, Andrew J. Liounis, Christian W. May, Laura C. Mayorga, Lillian Nguyen, Lynnae C. Quick, Dennis C. Reuter, Edgard Rivera-Valentín, Bashar Rizk, Heather L. Roper, Andrew J. Ryan, Brian Sutter, Mathilde M. Westermann, Daniel R. Wibben, Bobby G. Williams, Kenneth Williams, C. W. V. Wolner
Figure caption: The size and proximity of Apophis during 2029 stand out as a rare event when looking back at two centuries of known asteroid−Earth approaches within 0.5 lunar distances. Relative object sizes are to scale. Adapted from Binzel (2020).
Paper: OSIRIS-APEX: An OSIRIS-REx Extended Mission to Asteroid Apophis
Authors: Daniella N. DellaGiustina, Michael C. Nolan, Anjani T. Polit, Michael C. Moreau, Dathon R. Golish, Amy A. Simon, Coralie D. Adam, Peter G. Antreasian, Ronald-Louis Ballouz, Olivier S. Barnouin, Kris J. Becker, Carina A. Bennett, Richard P. Binzel, Brent J. Bos, Richard Burns, Nayessda Castro, Steven R. Chesley, Philip R. Christensen, M. Katherine Crombie, Michael G. Daly, R. Terik Daly, Heather L. Enos, Davide Farnocchia, Sandra Freund Kasper, Rose Garcia, Kenneth M. Getzandanner, Scott D. Guzewich, Christopher W. Haberle, Timothy Haltigin, Victoria E. Hamilton, Karl Harshman, Noble Hatten, Kyle M. Hughes, Erica R. Jawin, Hannah H. Kaplan, Dante S. Lauretta, Jason M. Leonard, Andrew H. Levine, Andrew J. Liounis, Christian W. May, Laura C. Mayorga, Lillian Nguyen, Lynnae C. Quick, Dennis C. Reuter, Edgard Rivera-Valentín, Bashar Rizk, Heather L. Roper, Andrew J. Ryan, Brian Sutter, Mathilde M. Westermann, Daniel R. Wibben, Bobby G. Williams, Kenneth Williams, C. W. V. Wolner
Figure caption: APEX will provide information about the near-surface properties of Apophis by using the spacecraft thrusters to excavate the top layer of regolith.
Paper: Validation of the Survey Simulator Tool for the NEO Surveyor Mission Using NEOWISE Data
Authors: Joseph R. Masiero, Dar W. Dahlen, Amy K. Mainzer, William F. Bottke, Jennifer C. Bragg, James. M. Bauer, Tommy Grav
Figure caption: Histogram showing the number of epochs of new detections recovered as a function of time. The bin size used is 28 days, and the vertical dotted lines mark January 1 for each year starting with 2010. The red histogram shows epochs that consist of only a single detection, while the black histogram is all other recovered epochs. The large gap from 2011 to 2014 is the time when the WISE spacecraft was in hibernation. The recovery rate is higher during the cryogenic phase, as the telescope was more sensitive then, and because the astrometry for the objects recovered by Mainzer et al. (2014b) was not submitted to the MPC and so does not appear in the list of already-reported detections. The general trend of increasing epochs with time during the reactivation mission is a result of the increasing number of objects discovered by ground-based surveys.
Paper: Validation of the Survey Simulator Tool for the NEO Surveyor Mission Using NEOWISE Data
Authors: Joseph R. Masiero, Dar W. Dahlen, Amy K. Mainzer, William F. Bottke, Jennifer C. Bragg, James. M. Bauer, Tommy Grav
Figure caption: Length of tracklets found in our search of NEOWISE data for objects that had no previously reported measurements. The majority have less than five detections (left of the dotted line) and could not have been found by the automated processing. The longest tracklet here is 55 detections, for object 2017 SG14.
Paper: How Does the Thermal Environment Affect the Exosphere/Surface Interface at Mercury?
Authors: F. Leblanc, M. Sarantos, D. Domingue, A. Milillo, D. W. Savin, P. Prem, J. Benkhoff, J. Zender, A. Galli, G. Murakami, S. Sasaki, M. Thompson, J. Raines
Figure caption: The derived spectral parameters. (a) CF position (μm), (b) RB1 position (μm), (c) RB1 emissivity, and (d) RB spectral contrast (μm) for each silicate are plotted against their corresponding sample temperature. From Varatharajan et al. (2020).
Paper: Libration- and Precession-driven Dissipation in the Fluid Cores of the TRAPPIST-1 Planets
Authors: Dhananjhay Bansal, Hannah S. Christie, Mathieu Dumberry
Figure caption: Dissipation induced by precession in the fluid core of each TRAPPIST-1 planet. The dissipation is computed based on a turbulent flow regime model.
Paper: Evidence for Fine-grained Material at Lunar Red Spots: Insights from Thermal Infrared and Radar Data Sets
Authors: Benjamin D Byron, Catherine M. Elder, Timothy D. Glotch, Paul O. Hayne, Lori M. Pigue, Joshua T. S. Cahill
Figure caption: Clementine color-ratio map showing lunar red spots in the vicinity of Mare Imbrium (top) and throughout southern Oceanus Procellarum, Mare Cognitum, and Mare Nubium (bottom). This map was created using three spectral filters (415, 750, and 1000 nm), where red = 750/415, green = 750/1000, and blue = 415/750.
Paper: Evidence for Fine-grained Material at Lunar Red Spots: Insights from Thermal Infrared and Radar Data Sets
Authors: Benjamin D Byron, Catherine M. Elder, Timothy D. Glotch, Paul O. Hayne, Lori M. Pigue, Joshua T. S. Cahill
Figure caption: Lambert Albedo maps created using Diviner Channel 1 solar reflectance data. Red spots (outlined in each image) generally have higher reflectance than surrounding maria. We use these albedo maps as an input to our H-parameter model.
Paper: The Importance of Isentropic Mixing in the Formation of the Martian Polar Layered Deposits
Authors: E. R. Ball, W. J. M. Seviour, D. M. Mitchell
Figure caption: HiRISE image PSP_001398_2615 of layers in the NPLDs. This image is centered at 81.°515N, 47.°300E. Credit: NASA/JPL-Caltech/Univ. of Arizona.
Paper: Dynamical Interactions and Mass Loss within the Uranian System
Authors: Stephen R. Kane, Zhexing Li
Figure caption: The regular moons and rings of the Jupiter (top), Saturn (middle), and Uranus (bottom) systems. The relative sizes of the moons are shown, and their semimajor axes are provided in units of the host planet radii. The extent of the current ring systems, including dense and tenuous rings, are shown as gray regions, and the vertical red dashed lines indicate the location of the fluid satellite Roche limit for each planet.
Paper: The Near-Earth Object Surveyor Mission
Authors: A. K. Mainzer, J. R. Masiero, Paul A. Abell, J. M. Bauer, William Bottke, Bonnie J. Buratti, Sean J. Carey, D. Cotto-Figueroa, R. M. Cutri, D. Dahlen, Peter R. M. Eisenhardt, Y. R. Fernandez, Roberto Furfaro, Tommy Grav, T. L. Hoffman, Michael S. Kelley, Yoonyoung Kim, J. Davy Kirkpatrick, Christopher R. Lawler, Eva Lilly, X. Liu, Federico Marocco, K. A. Marsh, Frank J. Masci, Craig W. McMurtry, Milad Pourrahmani, Lennon Reinhart, Michael E. Ressler, Akash Satpathy, C. A. Schambeau, S. Sonnett, Timothy B. Spahr, Jason A. Surace, Mar Vaquero, E. L. Wright, Gregory R. Zengilowski
Figure caption: The NEO Surveyor mission consists of a single infrared instrument operating at two infrared channels. The instrument is shielded from the Sun by its sunshade, and the black-painted radiator surfaces on the back of the instrument enable the mission to achieve its operating temperatures through passive cooling. The NEO Surveyor mission’s 6.15 m sunshade enables it to look down to solar elongations of 45° in order to detect asteroids more efficiently in the most circular, Earth-like orbits. The instrument is shown on the right with its one-time deployable aperture cover still attached.
Paper: The Near-Earth Object Surveyor Mission
Authors: A. K. Mainzer, J. R. Masiero, Paul A. Abell, J. M. Bauer, William Bottke, Bonnie J. Buratti, Sean J. Carey, D. Cotto-Figueroa, R. M. Cutri, D. Dahlen, Peter R. M. Eisenhardt, Y. R. Fernandez, Roberto Furfaro, Tommy Grav, T. L. Hoffman, Michael S. Kelley, Yoonyoung Kim, J. Davy Kirkpatrick, Christopher R. Lawler, Eva Lilly, X. Liu, Federico Marocco, K. A. Marsh, Frank J. Masci, Craig W. McMurtry, Milad Pourrahmani, Lennon Reinhart, Michael E. Ressler, Akash Satpathy, C. A. Schambeau, S. Sonnett, Timothy B. Spahr, Jason A. Surace, Mar Vaquero, E. L. Wright, Gregory R. Zengilowski
Figure caption: The NEO Surveyor field of regard (gray cones) is shown compared to that of NEOWISE (pink cones) and the orbit of the Earth (dashed line). The simulated population of PHAs larger than 50 m at the time of discovery is shown as blue dots. The NEOWISE field of regard is limited by its relatively short sunshade and low-Earth orbit, which prohibits it from reaching the near-Sun regions on the sky where NEOs are more likely to be found. NEO Surveyor’s sunshade is tall enough to enable it to observe down to 45° from the Sun, subtending a larger portion of the PHAs.
Paper: The Near-Earth Object Surveyor Mission
Authors: A. K. Mainzer, J. R. Masiero, Paul A. Abell, J. M. Bauer, William Bottke, Bonnie J. Buratti, Sean J. Carey, D. Cotto-Figueroa, R. M. Cutri, D. Dahlen, Peter R. M. Eisenhardt, Y. R. Fernandez, Roberto Furfaro, Tommy Grav, T. L. Hoffman, Michael S. Kelley, Yoonyoung Kim, J. Davy Kirkpatrick, Christopher R. Lawler, Eva Lilly, X. Liu, Federico Marocco, K. A. Marsh, Frank J. Masci, Craig W. McMurtry, Milad Pourrahmani, Lennon Reinhart, Michael E. Ressler, Akash Satpathy, C. A. Schambeau, S. Sonnett, Timothy B. Spahr, Jason A. Surace, Mar Vaquero, E. L. Wright, Gregory R. Zengilowski
Figure caption: Overview of the survey pattern. (a) Each NEO Surveyor Visit consists of six Exposures collected in a hexagonal dither pattern. (b) Visits are repeated in a Loop four times to make a Quad. (c) Quads are then tiled into Stacks, then Sides of the Sun (orange line). This figure shows two full Sides during the survey, made up of three Stacks each; darker colors indicate the first Quad in each stack. This pattern is then repeated.
Paper: The Near-Earth Object Surveyor Mission
Authors: A. K. Mainzer, J. R. Masiero, Paul A. Abell, J. M. Bauer, William Bottke, Bonnie J. Buratti, Sean J. Carey, D. Cotto-Figueroa, R. M. Cutri, D. Dahlen, Peter R. M. Eisenhardt, Y. R. Fernandez, Roberto Furfaro, Tommy Grav, T. L. Hoffman, Michael S. Kelley, Yoonyoung Kim, J. Davy Kirkpatrick, Christopher R. Lawler, Eva Lilly, X. Liu, Federico Marocco, K. A. Marsh, Frank J. Masci, Craig W. McMurtry, Milad Pourrahmani, Lennon Reinhart, Michael E. Ressler, Akash Satpathy, C. A. Schambeau, S. Sonnett, Timothy B. Spahr, Jason A. Surace, Mar Vaquero, E. L. Wright, Gregory R. Zengilowski
Figure caption: The spectral energy distribution for two different 140 m NEOs observed at 90° phase angle with visible geometric albedos of 0.03 and 0.17, with the NC1 and NC2 bandpasses overplotted as the cyan and magenta patches, respectively.
Paper: How Does the Thermal Environment Affect the Exosphere/Surface Interface at Mercury?
Authors: F. Leblanc, M. Sarantos, D. Domingue, A. Milillo, D. W. Savin, P. Prem, J. Benkhoff, J. Zender, A. Galli, G. Murakami, S. Sasaki, M. Thompson, J. Raines
Figure caption: Map of the modeled local maximum surface temperatures superposed on MESSENGER MDIS surface albedo map (Bauch et al. 2021). Bauch et al. (2021) excluded the polar regions from their analysis due to a lack of usable albedo data.
Paper: How Does the Thermal Environment Affect the Exosphere/Surface Interface at Mercury?
Authors: F. Leblanc, M. Sarantos, D. Domingue, A. Milillo, D. W. Savin, P. Prem, J. Benkhoff, J. Zender, A. Galli, G. Murakami, S. Sasaki, M. Thompson, J. Raines
Figure caption: (Left) Profile of the range of stresses experienced within a microstructure over one lunar diurnal cycle for a flat equatorial lunar surface. A homogeneous pyroxene microstructure (black line) is compared to a standard structure of 75% pyroxene and 25% plagioclase grains (green envelope). (Right) Profiles of average (dashed lines) and peak (solid lines) stresses over one lunar diurnal cycle for a homogeneous pyroxene microstructure (black), a standard microstructure (green), and a standard microstructure including cracks (magenta). In both panels, the vertical dashed lines represent sunrise, noon, and sunset, from left to right. Tensile stresses are represented as positive values, and compressional stresses are represented as negative values. From Molaro et al. (2015).
Paper: How Does the Thermal Environment Affect the Exosphere/Surface Interface at Mercury?
Authors: F. Leblanc, M. Sarantos, D. Domingue, A. Milillo, D. W. Savin, P. Prem, J. Benkhoff, J. Zender, A. Galli, G. Murakami, S. Sasaki, M. Thompson, J. Raines
Figure caption: The simulated release of adsorbed argon from a computer-generated powder (in black) at two different latitudes is gradual near the sunrise terminator. In contrast, models that do not account for inward diffusion (blue and red) and that treat desorption as an exponential decay of the adsorbate reservoir underestimate the gas residence time. It does not suffice to simply increase the residence time (contrast blue vs. red curves). Rather, the distribution of waiting times is not exponential; either it can be described as a second-order desorption (magenta line) ,or it can be interpreted as a distribution of adsorption energies. From Sarantos & Tsavachidis (2021).
Paper: How Does the Thermal Environment Affect the Exosphere/Surface Interface at Mercury?
Authors: F. Leblanc, M. Sarantos, D. Domingue, A. Milillo, D. W. Savin, P. Prem, J. Benkhoff, J. Zender, A. Galli, G. Murakami, S. Sasaki, M. Thompson, J. Raines
Figure caption: Calculated maximum temperature in the north polar region of Mercury superposed on a shaded relief map of MESSENGER-derived topography (from Paige et al. 2013).
Paper: How Does the Thermal Environment Affect the Exosphere/Surface Interface at Mercury?
Authors: F. Leblanc, M. Sarantos, D. Domingue, A. Milillo, D. W. Savin, P. Prem, J. Benkhoff, J. Zender, A. Galli, G. Murakami, S. Sasaki, M. Thompson, J. Raines
Figure caption: Profiles of the interior (left) and exterior/surface (right) stresses in lunar boulders throughout the lunar day, taken at the location in the boulder where the maximum stress occurs. This is shown for 0.3–1 m (top), 1–6 m (middle), and 10–50 m (bottom) boulders. Dashed lines show sunrise, noon, and sunset from left to right. From Molaro et al. (2017).
Paper: How Does the Thermal Environment Affect the Exosphere/Surface Interface at Mercury?
Authors: F. Leblanc, M. Sarantos, D. Domingue, A. Milillo, D. W. Savin, P. Prem, J. Benkhoff, J. Zender, A. Galli, G. Murakami, S. Sasaki, M. Thompson, J. Raines
Figure caption: Thermal profile with depth as calculated by Hale & Hapke (2002) for a single-layer model and for a thermal inertia of 67 J m−2 s−1/2 K−1 and a conductivity ratio of 50 J m−2 s−1 K−1.
Paper: How Does the Thermal Environment Affect the Exosphere/Surface Interface at Mercury?
Authors: F. Leblanc, M. Sarantos, D. Domingue, A. Milillo, D. W. Savin, P. Prem, J. Benkhoff, J. Zender, A. Galli, G. Murakami, S. Sasaki, M. Thompson, J. Raines
Figure caption: The average (black) and maximum (green) stresses induced during the state of peak tension in a microstructure with a given percentage of pyroxene and plagioclase grains. The values of each point on the plot are given in Table 1. From Molaro et al. (2015).
Paper: How Does the Thermal Environment Affect the Exosphere/Surface Interface at Mercury?
Authors: F. Leblanc, M. Sarantos, D. Domingue, A. Milillo, D. W. Savin, P. Prem, J. Benkhoff, J. Zender, A. Galli, G. Murakami, S. Sasaki, M. Thompson, J. Raines
Figure caption: Observed sodium limb column density (with line-of-sight tangent points below 30° in latitude) projected onto Mercury’s equatorial plane over the course of a Mercury year. The white dashed lines indicate the position of the warm longitudes as Mercury rotates. From Cassidy et al. (2016).
Paper: How Does the Thermal Environment Affect the Exosphere/Surface Interface at Mercury?
Authors: F. Leblanc, M. Sarantos, D. Domingue, A. Milillo, D. W. Savin, P. Prem, J. Benkhoff, J. Zender, A. Galli, G. Murakami, S. Sasaki, M. Thompson, J. Raines
Figure caption: The effects of target temperature on the production rates for impact melt and vapor. The Hermean flux assuming a circular orbit for the planet at 0.387 au is used for illustrative purposes. From Cintala (1992).
Paper: The Case for Future Gravity Science Investigations at Saturn with a Planetary Orbiter
Authors: Marzia Parisi
Figure caption: Evolution of Saturn’s pole position over 3 decades for two models: black curve from the IAU report (Archinal et al. 2018) and red curve from Jacobson (2022).
Paper: Stable Brine Layers beneath Europa’s Chaos
Authors: C. J. Chivers, J. J. Buffo, B. E. Schmidt
Figure caption: The distinct thermal and chemical evolution of NaCl sills is clear in their extended lifetimes (compared to freshwater). In each subplot, the left columns denote the thin-shell scenario (D = 10 km, T bot = 271.1 K; (a)–(c), (g), (i)) and the right columns the thick shell (D = 5 km, T bot = 260 K; (d)–(f), (h), (j)). (a)–(f) Cross-sectional profiles of entrained NaCl through the center of each sill after complete solidification. Depths of emplacement are grouped by row (e.g., (a), (d) are 1 km depth, (c), (f) are 3 km depth) and sill thicknesses are labeled in color and line style as shown in (f). Points on profiles denote where in the sill the top-down and bottom-up freeze fronts meet. (g), (h) Solidification times of all NaCl sills tested with depth from surface labeled in color. (i), (j) Comparison of the thermal and chemical evolution of NaCl sills, expressed in terms of total amount of NaCl precipitated out of solution during a simulation (in % of the initial mass of dissolved salts) vs. the “characteristic saturation time.” Depth of emplacement is labeled in color (shown in (g)) and initial sill thickness is denoted by the size of the circle (shown in (i)).