adsabs/AstroCLIMB huggingface dataset:
Paper: Identifying Interstellar Object Impact Craters
Authors: Samuel H. C. Cabot, Gregory Laughlin
Figure caption: Crater scaling relation for basalt-on-basalt impacts, which serves as verification of our simulation setup. Left: determination of transient crater diameter for the simulation involving a 1000 m diameter projectile. A fifth-degree polynomial is fit to the crater dimensions near maximum volume. The diameter that maximizes the polynomial is taken as D tr. Right: best-fit power law plotted against dimensionless π-scaling quantities for the four simulations considered.
Paper: Identifying Interstellar Object Impact Craters
Authors: Samuel H. C. Cabot, Gregory Laughlin
Figure caption: Analytic estimates of impact speed as a function of the melt volume and diameter of the transient crater for case S3 (see Table 3). The relationship between the three variables follows from scaling relations. Scaling parameters were fit using the simulated transient diameters and melt volumes. For reference, isovelocity contours are plotted for 16 (at which point the scaling relation becomes valid and is also characteristic of asteroid impacts), 30, and 100 km s−1, and the simulation results for 30 and 100 km s−1 impacts are marked.
Paper: Ring Seismology of the Ice Giants Uranus and Neptune
Authors: Joseph A. A'Hearn, Matthew M. Hedman, Christopher R. Mankovich, Hima Aramona, Mark S. Marley
Figure caption: Top: radial displacement eigenfunctions for ℓ = 2, 6, 10, and 14, normalized to ξ  r  = 1 at r = R, from the medium Uranus model. The Brunt–Väisälä frequency N, normalized to peak at 1, is shown with dotted lines. Middle: Eulerian density perturbation ﹩\rho ^{\prime} \left(r\right)﹩ for the same four modes. Bottom: integrand of Equations (11) and (12), ﹩\rho ^{\prime} {r}^{{\ell }+2}﹩, relevant for gravitational potential perturbations, for the same modes. The modes of lower oscillation degree ℓ are more sensitive to inner layers of the planet, while the modes of higher oscillation degree ℓ are more sensitive to outer layers of the planet.
Paper: Ring Seismology of the Ice Giants Uranus and Neptune
Authors: Joseph A. A'Hearn, Matthew M. Hedman, Christopher R. Mankovich, Hima Aramona, Mark S. Marley
Figure caption: Density (solid lines) and Brunt–Väisälä frequency (dotted) for models of Uranus (top) and Neptune (bottom) as functions of the fractional radius r/R. The scales of the y-axes are set equal for both the top and bottom panels for easier comparison between Uranus and Neptune models. The interior models used for this figure and as inputs to the GYRE software are available as data-behind-the-figure.(The data used to create this figure are available.)
Paper: Ring Seismology of the Ice Giants Uranus and Neptune
Authors: Joseph A. A'Hearn, Matthew M. Hedman, Christopher R. Mankovich, Hima Aramona, Mark S. Marley
Figure caption: Normal-mode OLR location predictions from all five Uranus models. The azimuthal order m (equivalent to the number of spiral arms) is the vertical axis, and distance from the center of Uranus is the horizontal axis, shown in Uranus radii on the bottom and in km on the top. OLRs can excite inward-propagating spiral density waves. The typical uncertainty of these resonance locations is shown by one bar on the left.
Paper: Ring Seismology of the Ice Giants Uranus and Neptune
Authors: Joseph A. A'Hearn, Matthew M. Hedman, Christopher R. Mankovich, Hima Aramona, Mark S. Marley
Figure caption: Normal-mode OVR location predictions from all five Uranus models. The azimuthal order m (equivalent to the number of spiral arms) is the vertical axis, and distance from the center of Uranus is the horizontal axis, shown in Uranus radii on the bottom and in km on the top. OVRs can excite outward-propagating bending waves. The typical uncertainty of these resonance locations is shown by one bar on the left.
Paper: Double Asteroid Redirection Test (DART): Structural and Dynamic Interactions between Asteroidal Elements of Binary Asteroid (65803) Didymos
Authors: Masatoshi Hirabayashi, Fabio Ferrari, Martin Jutzi, Ryota Nakano, Sabina D. Raducan, Paul Sánchez, Stefania Soldini, Yun Zhang, Olivier S. Barnouin, Derek C. Richardson, Patrick Michel, Elisabetta Dotto, Alessandro Rossi, Andrew R. Rivkin
Figure caption: Spatial distributions of critical cohesive strength, C crit, with different bulk densities (the contours show its magnitude). If C crit is positive, an element within the body should have cohesive strength; otherwise, that region should mechanically fail. The angle of internal friction, θ, is 35°. (a) ρ  B  = 1820 kg m−3. (b) ρ  B  = 2170 kg m−3. (c) ρ  B  = 2520 kg m−3. For all cases, the shape considered has dimensions of 837 m × 832 m × 786 m. The used dimensions lead to an ∼10% variation in volume, although this discrepancy does not affect the final results. Similar to Figure 2, the three bulk density cases are tested here based on the recent radar-based measurements, 2170 ± 350 kg m−3 (Naidu et al. 2020).
Paper: Radar and Lightcurve Observations and a Physical Model of Potentially Hazardous Asteroid 1981 Midas
Authors: Riley A. McGlasson, Sean E. Marshall, Flaviane C. F. Venditti, Shantanu P. Naidu, Lance A. M. Benner, Marina Brozović, Jon D. Giorgini, Patrick A. Taylor, Betzaida Aponte, Anne K. Virkki, Alan W. Harris, James W. Young, Marek Husárik, Guy Wells, Daniel Bamberger, Jeff Tobak
Figure caption: An early grid search (left, southern/retrograde; right, northern/prograde) to determine the pole direction of the model using lightcurve data. Ecliptic longitude and latitude are plotted on the x- and y-axes, respectively. Each point is color-coded with the reduced chi-square value of the model compared to lightcurve data only, with purple indicating a lower reduced chi-square value and yellow indicating a higher reduced chi-square value. On the left, squares are good models, diamonds are marginal models, and circles indicate models that are outside the 1σ threshold. On the right, the square indicates the best of the prograde models, diamonds are some of the next-best models, and circles are worse models. Looking at these figures, it becomes clear that the models having a northern pole direction (the “best” such model having a reduced chi-square value of about 17) are much worse fits for the lightcurve data.
Paper: Double Asteroid Redirection Test (DART): Structural and Dynamic Interactions between Asteroidal Elements of Binary Asteroid (65803) Didymos
Authors: Masatoshi Hirabayashi, Fabio Ferrari, Martin Jutzi, Ryota Nakano, Sabina D. Raducan, Paul Sánchez, Stefania Soldini, Yun Zhang, Olivier S. Barnouin, Derek C. Richardson, Patrick Michel, Elisabetta Dotto, Alessandro Rossi, Andrew R. Rivkin
Figure caption: Zero-velocity curves on the equatorial plane with three bulk densities. (a) ρ  B  = 1820 kg m−3. (b) ρ  B  = 2170 kg m−3. (c) ρ  B  = 2520 kg m−3. The red points indicate the equilibrium points, where net acceleration in the rotating frame becomes zero, and the contours show the zero-velocity curves. Each equilibrium point is labeled as EQ. The three bulk density cases are tested based on the recent radar-based measurements, 2170 ± 350 kg m−3 (Naidu et al. 2020).
Paper: Double Asteroid Redirection Test (DART): Structural and Dynamic Interactions between Asteroidal Elements of Binary Asteroid (65803) Didymos
Authors: Masatoshi Hirabayashi, Fabio Ferrari, Martin Jutzi, Ryota Nakano, Sabina D. Raducan, Paul Sánchez, Stefania Soldini, Yun Zhang, Olivier S. Barnouin, Derek C. Richardson, Patrick Michel, Elisabetta Dotto, Alessandro Rossi, Andrew R. Rivkin
Figure caption: Initial (left) and final (right) asteroid morphology derived from an SPH simulation of a vertical DART-like impact on a spherical, 150 m diameter body with C 0 = 0 Pa and θ = 31°. The orange regions indicate materials transported from their original locations to new places due to the DART impact. The bulk density, ρ  B , is 1600 kg m−3.
Paper: Radar and Lightcurve Observations and a Physical Model of Potentially Hazardous Asteroid 1981 Midas
Authors: Riley A. McGlasson, Sean E. Marshall, Flaviane C. F. Venditti, Shantanu P. Naidu, Lance A. M. Benner, Marina Brozović, Jon D. Giorgini, Patrick A. Taylor, Betzaida Aponte, Anne K. Virkki, Alan W. Harris, James W. Young, Marek Husárik, Guy Wells, Daniel Bamberger, Jeff Tobak
Figure caption: Plot of pole-direction chi-square values. The ecliptic longitude is plotted on the horizontal axis, and the ecliptic latitude on the vertical axis; it is colored by the reduced chi-square value of the model compared to the entire data set (delay-Doppler images, CW spectra, and lightcurves), with purple indicating a lower reduced chi-square value and yellow indicating a higher reduced chi-square value. Squares are good models, diamonds are marginal models, and circles indicate models that are outside the 1σ threshold.
Paper: Science Drivers for the Future Exploration of Ceres: From Solar System Evolution to Ocean World Science
Authors: Julie Castillo-Rogez, Marc Neveu, Vassilissa Vinogradoff, Kelly E. Miller, Michael M. Sori, Federico Tosi, Britney Schmidt, Jennifer E. C. Scully, Mohit Melwani Daswani, Kynan Hughson, Harry McSween, Cristina De Sanctis, Lynnae Quick, Anton Ermakov, Guneshwar Thangjam, Katharina Otto, Katrin Krohn, Paul Schenk, Andreas Nathues, Carol Raymond
Figure caption: Examples of landforms found at Ceres that make it a natural laboratory to study geological processes in an ice-rich crust. (a) Recent evaporite exposure in Occator crater; (b) brine exposure via fractures in Vinalia Faculae, in the eastern part of Occator crater; (c) Ahuna Mons, a cryovolcano built with rock and brine (Ruesch et al. 2016, 2019a), as indicated by the high content of sodium carbonate (bright bluish material) on its flanks (Zambon et al. 2017); (d) glacier-like features in Juling crater (Raponi et al. 2018); (e) landslide whose morphology indicates a high ice content (Schmidt et al. 2017); (f) flat floor resulting from impact-generated heat and melting in Ikapati crater; (g) (forefront) mounds and hills formed from postimpact cryohydrologic processes (Schmidt et al. 2020); (h) fresh salt-rich ejecta (dark blue material) and central crest in Haulani crater (Tosi et al. 2018); (i) normal faulting in an ice-rich crust at Nar Sulcus in Yalode crater (Hughson et al. 2018). Credit: NASA/JPL-Caltech/UCLA/MPS/DLR/IDA/USRA/LPL, based on PIA22090, which contains detailed information on the origin of these pictures.
Paper: Science Drivers for the Future Exploration of Ceres: From Solar System Evolution to Ocean World Science
Authors: Julie Castillo-Rogez, Marc Neveu, Vassilissa Vinogradoff, Kelly E. Miller, Michael M. Sori, Federico Tosi, Britney Schmidt, Jennifer E. C. Scully, Mohit Melwani Daswani, Kynan Hughson, Harry McSween, Cristina De Sanctis, Lynnae Quick, Anton Ermakov, Guneshwar Thangjam, Katharina Otto, Katrin Krohn, Paul Schenk, Andreas Nathues, Carol Raymond
Figure caption: Possible explanations that have been suggested for explaining late activity in Ceres. All three scenarios assume a similar early evolution involving global melting from short-lived radioisotope decay heat. The “ice shell” pathway is based on pre-Dawn models that assume an ice-dominated crust that might be convecting. In those models, thermal metamorphism was expected to happen but not fully modeled. The “clathrate” pathway assumes a crust rich in clathrate hydrates or ice–rock mixtures such that the onset of convection is unlikely. That path enables the preservation of brines, with the potential addition of volatiles produced from thermal metamorphism. The “mudball” pathway assumes that Ceres’ heat transfer was driven by slow hydrothermal circulation in a thick ocean that remains at present. In that case, the mantle temperatures remain too low (<100°C) for thermal metamorphism to develop. It is also likely that Ceres was subject to intensive impacting in its early history, which could have locally warmed its crust and created pathways for the extrusion of deep material.
Paper: Science Drivers for the Future Exploration of Ceres: From Solar System Evolution to Ocean World Science
Authors: Julie Castillo-Rogez, Marc Neveu, Vassilissa Vinogradoff, Kelly E. Miller, Michael M. Sori, Federico Tosi, Britney Schmidt, Jennifer E. C. Scully, Mohit Melwani Daswani, Kynan Hughson, Harry McSween, Cristina De Sanctis, Lynnae Quick, Anton Ermakov, Guneshwar Thangjam, Katharina Otto, Katrin Krohn, Paul Schenk, Andreas Nathues, Carol Raymond
Figure caption: Two architectures proposed for addressing key open questions about Ceres’ endogenic activity, habitability potential, and origin. The in situ architecture is a hopper that explores two sites at Occator crater, the first one at the northeastern ejecta blanket called Homowo Regio and the second one in the Vinalia Faculae. The second concept would return a sample from the Vinalia Faculae. Both concepts would include an orbital phase during which high-resolution imaging and gravity data are acquired at key landforms of potential cryovolcanic origin. Also, in both concepts, the in situ phase includes an electromagnetic investigation that would map the distribution of brines below Occator crater down to 50 km depth (J. C. Castillo-Rogez et al. 2022, in press). Credit: Raoul Ranoa.
Paper: Science Drivers for the Future Exploration of Ceres: From Solar System Evolution to Ocean World Science
Authors: Julie Castillo-Rogez, Marc Neveu, Vassilissa Vinogradoff, Kelly E. Miller, Michael M. Sori, Federico Tosi, Britney Schmidt, Jennifer E. C. Scully, Mohit Melwani Daswani, Kynan Hughson, Harry McSween, Cristina De Sanctis, Lynnae Quick, Anton Ermakov, Guneshwar Thangjam, Katharina Otto, Katrin Krohn, Paul Schenk, Andreas Nathues, Carol Raymond
Figure caption: Summary of the science themes addressed by the exploration of Ceres. The themes are presented along with the science priorities in NASA’s Planetary Science Decadal Survey (National Research Council 2011). Synergies between science themes refer to high-priority questions, such as the origin of volatiles and organics in the inner solar system and the habitability of large icy bodies through time. A future mission to Ceres should aim to address questions that pertain both to the origin of the current architecture of our solar system and to the habitability of icy bodies through time. These themes are also relevant to the search for habitable worlds in exoplanetary systems.
Paper: Science Drivers for the Future Exploration of Ceres: From Solar System Evolution to Ocean World Science
Authors: Julie Castillo-Rogez, Marc Neveu, Vassilissa Vinogradoff, Kelly E. Miller, Michael M. Sori, Federico Tosi, Britney Schmidt, Jennifer E. C. Scully, Mohit Melwani Daswani, Kynan Hughson, Harry McSween, Cristina De Sanctis, Lynnae Quick, Anton Ermakov, Guneshwar Thangjam, Katharina Otto, Katrin Krohn, Paul Schenk, Andreas Nathues, Carol Raymond
Figure caption: Summary of processes that may alter the chemical properties of a deep ocean over time: loss of volatiles from the mantle upon thermal metamorphism and radiolysis. The Occator impact itself could introduce exogenic material in the crust. Based on Altair et al. (2018); background rendering from Raoul Ranoa.
Paper: Longitudinal Variation of H2O Ice Absorption on Miranda
Authors: Riley A. DeColibus, Nancy J. Chanover, Richard J. Cartwright
Figure caption: Left panel: examples of four nightly average spectra acquired with TripleSpec. The wavelengths between 1.35–1.42 μm and 1.81–1.93 μm are strongly affected by telluric noise and have been omitted for clarity. The short-wavelength “bump” between 0.95 and 1.15 μm in the TripleSpec data is an artifact of merging spectral orders. A spectrum of Uranus is also plotted to show which wavelength ranges have the strongest contamination, visible as increased error estimates in certain regions of the spectrum, primarily on the anti-Uranus and sub-Uranus spectra. See Table 2 for observation details. Right panel: the “grand-average” TripleSpec spectra, constructed from multiple nights of data. Spectra in both panels are normalized to unity at 1.72 μm and offset in increments of 0.5.
Paper: Longitudinal Variation of H2O Ice Absorption on Miranda
Authors: Riley A. DeColibus, Nancy J. Chanover, Richard J. Cartwright
Figure caption: Subobserver latitudes and longitude ranges of the Miranda spectra presented in this work. The width of the horizontal bars attached to each data point represents the subobserver longitudes at the beginning and end of the set of spectral frames that contributed to a particular final spectrum. Spectra acquired with SpeX are marked with colored crosses and dotted error bars, TripleSpec with colored squares and solid error bars, and GNIRS with black diamonds and dashed error bars. The SpeX spectrum from UT000907, our only spectrum of the southern hemisphere, has been omitted in order to better visualize the latitudinal spread of the northern hemisphere spectra. Spectra acquired at latitudes >35°N are new in this work. Gray shaded regions on either side of the plot show overlap from spectra crossing 0° longitude, and spectra in this region are plotted on both the left and right sides of the diagram. In this plot and spectral plots, we maintain a color scheme of blue tones for the leading quadrant, green tones for the anti-Uranus quadrant, orange tones for the trailing quadrant, and purple tones for the sub-Uranus quadrant.
Paper: Longitudinal Variation of H2O Ice Absorption on Miranda
Authors: Riley A. DeColibus, Nancy J. Chanover, Richard J. Cartwright
Figure caption: Left panel: hemisphere and quadrant ratios for all three H2O ice bands on Miranda, designated on the X-axis. These ratios are calculated using the mean band measurements with all spectra included. The yellow squares represent the 1.5 μm band, the purple circles are the 1.65 μm band, and the red triangles are the 2.0 μm band. Right panel: leading/trailing hemisphere ratios of H2O ice band areas for the Uranian satellites vs. planetocentric distance, based on Figure 9 in Cartwright et al. (2018). Plotted error bars represent 2σ uncertainties. The mean radius of Uranus is included for illustrative purposes.
Paper: Longitudinal Variation of H2O Ice Absorption on Miranda
Authors: Riley A. DeColibus, Nancy J. Chanover, Richard J. Cartwright
Figure caption: Left panel: GNIRS spectra of Miranda. Right panel: the three previously unpublished SpeX spectra that we included in our analysis. Spectra in both panels are normalized to unity at 1.72 μm and offset in increments of 0.5. See Table 2 for observation details.
Paper: Longitudinal Variation of H2O Ice Absorption on Miranda
Authors: Riley A. DeColibus, Nancy J. Chanover, Richard J. Cartwright
Figure caption: A plot of the integrated band areas (left panel) and fractional band depths (right panel) vs. longitude on Miranda. Blue squares are TripleSpec spectra, green circles are SpeX spectra, and red triangles are GNIRS spectra. Vertical error bars represent 1σ errors in both panels. The lowest, lightest-colored set of measurements represents the 1.65 μm band, the middle set of measurements represents the 1.5 μm band, and the darker-colored upper set is for the 2.0 μm band. The golden horizontal lines represent the weighted mean band areas (and depths), and the gray dashed lines represent our best-fit sinusoidal models. Other features are the same as in Figure 3.
Paper: Longitudinal Variation of H2O Ice Absorption on Miranda
Authors: Riley A. DeColibus, Nancy J. Chanover, Richard J. Cartwright
Figure caption: Left panel: a plot of the calculated H2O ice temperatures for each spectrum vs. longitude on Miranda. Blue squares are TripleSpec spectra, green circles are SpeX spectra, and red triangles are GNIRS spectra. Right panel: the temperatures for the grand-average TripleSpec spectra (blue squares), mean temperatures of all spectra for each quadrant (green squares), and temperatures of the GNIRS spectra (red triangles). Vertical error bars represent 1σ errors in both panels. Other features are the same as in Figure 3.
Paper: Longitudinal Variation of H2O Ice Absorption on Miranda
Authors: Riley A. DeColibus, Nancy J. Chanover, Richard J. Cartwright
Figure caption: A visual demonstration of the band area and depth measurement process, using the trailing hemisphere TripleSpec spectrum from UT201013. Error bars on the spectrum have been omitted for clarity. The gap between 1.85 and 1.88 μm is intrinsic to TripleSpec, and those wavelengths are ignored in the continuum-fitting process. The right-side continuum for the 1.5 μm band overlaps with the left-side continuum for the 2.0 μm band.
Paper: Longitudinal Variation of H2O Ice Absorption on Miranda
Authors: Riley A. DeColibus, Nancy J. Chanover, Richard J. Cartwright
Figure caption: Voyager 2/ISS full-disk mosaic of the southern hemisphere of Miranda, including the three large coronae (highlighted in green and outlined with dashes), which were likely formed by tectonism and perhaps cryovolcanic processes as well. Miranda’s south pole is at disk center. All but one of our spectra are located on the northern hemisphere, which was not imaged by Voyager 2, so this figure is included as context for the discussion in Section 5. Image credit: NASA/JPL/Caltech/USGS, PIA18185.
Paper: Longitudinal Variation of H2O Ice Absorption on Miranda
Authors: Riley A. DeColibus, Nancy J. Chanover, Richard J. Cartwright
Figure caption: The same as Figure 7, but only showing the band measurements of our mean and TripleSpec grand-average spectra. Blue squares are the mean band areas/depths for each quadrant, with purple horizontal lines representing weighted means. Orange triangles are the band areas/depths of the grand-average spectra, with yellow horizontal lines representing weighted means. Vertical error bars represent 2σ errors on both plots.
Paper: Longitudinal Variation of H2O Ice Absorption on Miranda
Authors: Riley A. DeColibus, Nancy J. Chanover, Richard J. Cartwright
Figure caption: We use the TripleSpec spectrum of Miranda from UT210105 to demonstrate our ability to correct the scattered light from Uranus and retrieve the shape of the 1.5 μm H2O ice band. From top to bottom, we plot in shades of orange the different spectral orders in the uncorrected and unmerged spectrum, in shades of blue the Uranus-corrected and unmerged spectrum, in green the Uranus-corrected and merged spectrum, and in black the GNIRS sub-Uranus spectrum, which was acquired at similar subobserver longitudes. While the “peaks” of contamination are effectively removed, some spurious spectral slopes remain between different spectral orders (<1.25 μm), which propagate into the final, merged spectrum and create the 0.95–1.15 μm “bump.” All spectra are normalized to unity at 1.72 μm and offset in increments of 0.5.
Paper: Longitudinal Variation of H2O Ice Absorption on Miranda
Authors: Riley A. DeColibus, Nancy J. Chanover, Richard J. Cartwright
Figure caption: We demonstrate the uncertainty in the derived scale factor in order 4 (H band) and its effect on the resulting Uranus-subtracted spectrum. The blue spectrum is the “observed” Miranda spectrum from UT210105, the green spectrum is the Miranda spectrum after subtracting Uranus (best-fit scale factor), and the orange spectra represent the ±1σ uncertainty in the scale factor. We note that we corrected a full-night spectrum in this figure for clarity, but corrections for the data used for analysis in this work were applied to multiple groups of telluric-corrected spectra per night.
Paper: Longitudinal Variation of H2O Ice Absorption on Miranda
Authors: Riley A. DeColibus, Nancy J. Chanover, Richard J. Cartwright
Figure caption: This figure plots TripleSpec spectra of our G-type telluric standard stars, divided by the spectrum of the Sun. All spectra are normalized to unity between 2.21 and 2.225 μm and are offset in increments of 0.1. For the purposes of clarity, the spectra have been substantially smoothed by a 25-pixel boxcar kernel.