adsabs/AstroCLIMB huggingface dataset:
Paper: Low-speed Impacts into Ice–Dust Granular Mixtures
Authors: Julie Brisset, Christopher Cox, Jessica Metzger, Thomas Miletich, Nadia Mohammed, Allison Rascon, Laura Forczyk, Adrienne Dove, Joshua Colwell
Figure caption: Average normalized cumulative ejecta mass M(>v)/m as a function of launch speed v  e  for the four types of targets investigated: dry regolith at room temperature (the red plus signs; μ = 1.6); frosted cryogenic regolith (the black plus signs; μ = 0.8); frosted regolith–ice mixtures (the blue triangles; μ = 0.8); and dry cryogenic regolith (the black diamonds; μ = 1.6). We only show drops with a glass projectile. The respective dashed lines show the power-law fits for each target type. The corresponding μ coefficients are calculated following the Housen & Holsapple (2011) scaling law.
Paper: Low-speed Impacts into Ice–Dust Granular Mixtures
Authors: Julie Brisset, Christopher Cox, Jessica Metzger, Thomas Miletich, Nadia Mohammed, Allison Rascon, Laura Forczyk, Adrienne Dove, Joshua Colwell
Figure caption: Crater volume estimated assuming a conical crater shape for our low-energy impacts. The colors and symbols follow the same pattern as in previous figures, with red showing room-temperature regolith samples, black showing frosted regolith samples, and blue showing water ice mixtures. The large symbols show the average for each target type and energy level with the associated error bar.
Paper: Low-speed Impacts into Ice–Dust Granular Mixtures
Authors: Julie Brisset, Christopher Cox, Jessica Metzger, Thomas Miletich, Nadia Mohammed, Allison Rascon, Laura Forczyk, Adrienne Dove, Joshua Colwell
Figure caption: Total ejecta masses measured on the collection plate for various impact energies and volumetric water ice content. Left: the red plus signs show impacts into dry regolith at room temperature, the black plus signs show impacts into frosted regolith without additional water ice, and the blue symbols show impacts into regolith–ice mixtures. The mixtures contain water ice in volumetric proportions of 33% (crosses; dashed line), 50% (triangles; solid line), and 75% (squares; dashed–dotted line). We do not show collected masses for impacts with energies larger than 106 ergs, as these resulted in significant ejecta landing beyond the collection plate. Right: the total ejecta masses for impacts between 6 and 7 × 105 ergs with varying volumetric water ice content of the target.
Paper: Lightcurves and Rotations of Trans-Neptunian Objects in the 2:1 Mean Motion Resonance with Neptune
Authors: Audrey Thirouin, Scott S. Sheppard
Figure caption: The 2:1 resonant TNOs are classified into four groups: (1) objects with a lightcurve from the literature (blue squares; see Section 4.1 for more details), (2) objects with a flat-to-moderate lightcurve amplitude from our survey (green triangles), (3) objects with a large amplitude from this survey (red diamonds), and (4) objects never observed for lightcurve study (black circles). Our survey is combined with published lightcurves of 2:1 TNOs to cover a range of inclination, eccentricity, and absolute magnitude. Note that the nine likely 2:1 TNOs mentioned in the Introduction are plotted. Orbital elements and absolute and visual magnitudes are from the Minor Planet Center (2022 February).
Paper: Low-speed Impacts into Ice–Dust Granular Mixtures
Authors: Julie Brisset, Christopher Cox, Jessica Metzger, Thomas Miletich, Nadia Mohammed, Allison Rascon, Laura Forczyk, Adrienne Dove, Joshua Colwell
Figure caption: Scaled crater radii in the strength regime. The data point colors correspond to the sample types: dry (red), frosted (black), and ice mixtures (blue, crosses for 33%, triangles for 50%, and squares for 75% volume ice content). For each target type, the three large data points correspond to various impact energies averaged over individual projectiles (as in Figure 8). Associated error bars are shown. The dashed line corresponds to the linear fit ﹩R{\left(\displaystyle \frac{\rho }{m}\right)}^{\tfrac{1}{3}}=4.34{\left(\displaystyle \frac{\rho }{\delta }\right)}^{0.1}{\left[\tfrac{Y}{\rho {U}^{2}}\right]}^{-0.25}﹩.
Paper: Low-speed Impacts into Ice–Dust Granular Mixtures
Authors: Julie Brisset, Christopher Cox, Jessica Metzger, Thomas Miletich, Nadia Mohammed, Allison Rascon, Laura Forczyk, Adrienne Dove, Joshua Colwell
Figure caption: The crater sizes measured for the impacts into dry room-temperature regolith (the red plus signs), frosted regolith (the black plus signs), and water ice mixtures (blue, crosses for 33%, triangles for 50%, and squares for 75% volume ice content). The large symbols show the averages for each type of projectile (Teflon, ρ ∼ 1.5 g/cm3; glass, ρ ∼ 3 g/cm3; and brass, ρ ∼ 9 g/cm3).
Paper: Low-speed Impacts into Ice–Dust Granular Mixtures
Authors: Julie Brisset, Christopher Cox, Jessica Metzger, Thomas Miletich, Nadia Mohammed, Allison Rascon, Laura Forczyk, Adrienne Dove, Joshua Colwell
Figure caption: Measured porosities of the target samples for room-temperature impacts (red), cold targets without ice (black), and targets with water ice grains (blue). The latter are divided into samples with 33% (crosses), 50% (triangles), and 75% (squares) water ice by volume. The average porosity values are indicated for each target type.
Paper: Lightcurves and Rotations of Trans-Neptunian Objects in the 2:1 Mean Motion Resonance with Neptune
Authors: Audrey Thirouin, Scott S. Sheppard
Figure caption: The Lomb periodogram (upper plot) favors a rotational frequency at 4.87 cycles day−1. Due to the large amplitude and asymmetric lightcurve, the double-peaked rotational lightcurve with a periodicity of 9.85 hr is favored (lower plot). A second-order Fourier fit is overplotted (black line).
Paper: Lightcurves and Rotations of Trans-Neptunian Objects in the 2:1 Mean Motion Resonance with Neptune
Authors: Audrey Thirouin, Scott S. Sheppard
Figure caption: We summarize the number of partial, flat, and full in the 2:1 resonance (left plot). On the right, the bubble size varies with the object’s absolute magnitude. There is no obvious trend between lightcurve variability and absolute magnitude. Binaries display a larger amplitude than single objects. The two large amplitude TNOs found by our survey are indicated.
Paper: Lightcurves and Rotations of Trans-Neptunian Objects in the 2:1 Mean Motion Resonance with Neptune
Authors: Audrey Thirouin, Scott S. Sheppard
Figure caption: The main peak favored by the Lomb periodogram is at 2.31 cycles day−1 (10.40 hr). Due to the large amplitude and assymetric lightcurve, we choose the double-peaked period of 2 × 10.40 hr = 20.80 hr.
Paper: Lightcurves and Rotations of Trans-Neptunian Objects in the 2:1 Mean Motion Resonance with Neptune
Authors: Audrey Thirouin, Scott S. Sheppard
Figure caption: Objects in the 2:1 mean-motion resonance with Neptune.
Paper: The Dynamical Viability of an Extended Jupiter Ring System
Authors: Stephen R. Kane, Zhexing Li
Figure caption: The regular moons and rings of the Jupiter and Saturn systems, where 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 are the fluid satellite Roche limit for each planet.
Paper: The Dynamical Viability of an Extended Jupiter Ring System
Authors: Stephen R. Kane, Zhexing Li
Figure caption: Results of particle injection and survival for the 106 yr (top panel) and 107 yr (middle panel) dynamical simulations. The horizontal axis is the separation from Jupiter in planetary radii, and the vertical axis shows the percentage of the total dynamical simulation that particles survived at that location, represented by the green line. The vertical dotted lines represent the semimajor axes of the Galilean moons, and the vertical dashed lines represent the locations of the rigid and fluid Roche limits. The bottom panel shows the change in eccentricity that occurs for each particle as a function of their initial semimajor axis during the course of the 107 yr simulations.
Paper: The Dynamical Viability of an Extended Jupiter Ring System
Authors: Stephen R. Kane, Zhexing Li
Figure caption: Planet masses (Jupiter masses) and Hill radii (planetary radii) for the known exoplanets with measured masses and radii. The locations of Earth, Jupiter, and Saturn are marked by E, J, and S, respectively. The gray region indicates where formation of massive moons may be limited by disk migration, while a larger Hill radius maximizes primordial and new material to contribute to ring formation.
Paper: The Dynamical Viability of an Extended Jupiter Ring System
Authors: Stephen R. Kane, Zhexing Li
Figure caption: Eccentricity as a function of time for the Galilean satellites: Io, Europa, Ganymede, and Callisto. The eccentricity variations were recorded every 100 yr during a 106 yr simulation, as described in Section 3.
Paper: The Dynamical Viability of an Extended Jupiter Ring System
Authors: Stephen R. Kane, Zhexing Li
Figure caption: The loss rate for all particles within the investigated semimajor axis region around Jupiter, shown as a function of time (fractions of 107 yr) and the percentage of particles that survive to that time.
Paper: Physical Characterization of Near-Earth Asteroid (52768) 1998 OR2: Evidence of Shock Darkening/Impact Melt
Authors: Adam Battle, Vishnu Reddy, Juan A. Sanchez, Benjamin Sharkey, Neil Pearson, Bryn Bowen
Figure caption: Phase-folded lightcurves of NEA (52768) 1998 OR2 from the LEO 0.5 m telescope in four Sloan filters. Error bars are equivalent to or smaller than the points used to display the data. The lightcurve and rotation period are consistent with those published by Koehn et al. (2014) and Warner & Stephens (2020).
Paper: Reduced Atmospheres of Post-impact Worlds: The Early Earth
Authors: Jonathan P. Itcovitz, Auriol S. P. Rae, Robert I. Citron, Sarah T. Stewart, Catriona A. Sinclair, Paul B. Rimmer, Oliver Shorttle
Figure caption: Left: simplified box model used in melt–atmosphere calculations (see Section 4). In Model 3A, we assume that the iron accreted by the target interior is well mixed in the impact-generated melt phase and can chemically interact with the melt. In Model 3B, we assume that this iron instead sinks to the bottom of the melt, and is unable to chemically interact with the melt. An approximate pressure–temperature profile is given, showing the 1900 K we use as the temperature at the interface between the atmosphere and melt boxes in our model, and which is based off of Kasting (1988) and Solomatov and Stevenson (1993). Right: vertical slice of the target at the post-impact stage, depicting the settled-out structure of the impact-generated melt phase (i.e., the summation of shock melting, adiabatic melting, and isostatic adjustment), the large steam-dominated atmosphere, and material that is gravitationally unbound from the planet that we classify as unaccreted by the target.
Paper: Reduced Atmospheres of Post-impact Worlds: The Early Earth
Authors: Jonathan P. Itcovitz, Auriol S. P. Rae, Robert I. Citron, Sarah T. Stewart, Catriona A. Sinclair, Paul B. Rimmer, Oliver Shorttle
Figure caption: Left: vertical slice of the target and impactor (impact angle of 45°) before the impact takes place, showing the mantles and cores of both bodies, as well as the target’s surface conditions. Right: decision tree showing the components of the physical model included in each of the five models presented in Section 5.
Paper: Reduced Atmospheres of Post-impact Worlds: The Early Earth
Authors: Jonathan P. Itcovitz, Auriol S. P. Rae, Robert I. Citron, Sarah T. Stewart, Catriona A. Sinclair, Paul B. Rimmer, Oliver Shorttle
Figure caption: Timeline of important events and processes that the target and impactor experience from the moment of impact to long after it. The left-hand segment shows processes that we assume to have finished occurring by the time we begin equilibrium calculations involving melt–atmosphere interactions. The central segment shows the period of melt–atmosphere interactions, where the system is otherwise in a pseudo-steady-state with few other processes occurring that substantially affect the state of the planet. The right-hand segment shows processes that we assume to occur after the melt and atmosphere have reached equilibrium, including solidification of the melt phase (throughout which melt–atmosphere interactions will also occur to maintain equilibrium, but a different equilibrium to that which we find in this study), hydrogen escape from the top of the atmosphere, significant cooling of the system to space, the resulting condensation of the steam atmosphere, and the ensuing photochemistry of Zahnle et al. (2020).
Paper: Reduced Atmospheres of Post-impact Worlds: The Early Earth
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 1 and detailed in Section 5.2, the post-impact (dashed) and post-equilibration (solid) results are shown. The standard values of Table 1 are used for all parameters except impactor mass in all cases. The standard impactor mass is indicated by the vertical line for each model.
Paper: Reduced Atmospheres of Post-impact Worlds: The Early Earth
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 major three species in the atmosphere, and total atmospheric pressure. (c) Oxygen fugacities of the atmosphere, basaltic 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: Reduced Atmospheres of Post-impact Worlds: The Early Earth
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 which 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: Reduced Atmospheres of Post-impact Worlds: The Early Earth
Authors: Jonathan P. Itcovitz, Auriol S. P. Rae, Robert I. Citron, Sarah T. Stewart, Catriona A. Sinclair, Paul B. Rimmer, Oliver Shorttle
Figure caption: GADGET2 impact-generated melt and vapor masses as a function of impactor mass and impact energy. We show impact energy, despite using specific energy within our models, as this better demonstrates the increasing melt and vapor mass as the impacts become more head-on (i.e., lower θ  i ). The vertical dashed line indicates an impact under our standard values (Table 1). The solid black line in the central panel is an example of how use linear fits of the data in log space to interpolate melt and vapor masses from the simulations. The total mass that we classify as our melt phase moving into melt–atmosphere interactions consists of the summed mass of melt and vapours (see text).
Paper: Reduced Atmospheres of Post-impact Worlds: The Early Earth
Authors: Jonathan P. Itcovitz, Auriol S. P. Rae, Robert I. Citron, Sarah T. Stewart, Catriona A. Sinclair, Paul B. Rimmer, Oliver Shorttle
Figure caption: Partial pressures of atmospheric species at each step of impact processing and melt–atmosphere equilibration. Total atmospheric pressure at each stage is also shown. We note that several of the processes occurring during impact will occur over similar timescales (e.g., Figure 3), and our representation of these processes here is simply the ordering we have implemented within our calculations. Species other than H2O and H2 are not involved in melt–atmosphere interactions. Melt–atmosphere interactions dominantly cause changes in the atmosphere during the first step (i.e., Step 1), meaning that the system is almost at equilibrium, and only minor changes occur in subsequent steps.
Paper: Reduced Atmospheres of Post-impact Worlds: The Early Earth
Authors: Jonathan P. Itcovitz, Auriol S. P. Rae, Robert I. Citron, Sarah T. Stewart, Catriona A. Sinclair, Paul B. Rimmer, Oliver Shorttle
Figure caption: Distribution of impactor iron inventory between different target reservoirs as a function of impactor mass for v  i  = 2v esc. The solid lines are quadratic fits in log-linear space that we use to interpolate iron distributions from our simulations.
Paper: Reduced Atmospheres of Post-impact Worlds: The Early Earth
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 3B. 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) Oxygen fugacities of the atmosphere, basaltic melt, and peridotitic melt. The FMQ and iron wüstite (IW) buffers are shown for reference (dotted lines). (c) Metallic iron remaining in the melt pool after metal saturation has been reached for each melt-phase composition.
Paper: Reduced Atmospheres of Post-impact Worlds: The Early Earth
Authors: Jonathan P. Itcovitz, Auriol S. P. Rae, Robert I. Citron, Sarah T. Stewart, Catriona A. Sinclair, Paul B. Rimmer, Oliver Shorttle
Figure caption: Comparison of the post-impact atmosphere of this study with the composition of the atmosphere of Zahnle et al. (2020) once cooled to 1900 K.
Paper: Shape Modeling of Dimorphos for the Double Asteroid Redirection Test (DART)
Authors: R. Terik Daly, Carolyn M. Ernst, Olivier S. Barnouin, Robert W. Gaskell, Eric E. Palmer, Hari Nair, Ray C. Espiritu, Sarah Hasnain, Dany Waller, Angela M. Stickle, Michael C. Nolan, Josep M. Trigo-Rodríguez, Elisabetta Dotto, Alice Lucchetti, Maurizio Pajola, Simone Ieva, Patrick Michel
Figure caption: Simulated DRACO and LEIA images. A scaled-down version of Itokawa is a stand-in for Dimorphos, while a scaled-down Ryugu stands in for Didymos. DRACO images (left column) progressively zoom in on the impact site. The highest-resolution LEIA image (right column) is much coarser than the expected DRACO images, which limits the amount of detail that can be seen in the LEIA image. However, LEIA provides alternative viewing geometries and additional limb information that benefit the long-wavelength shape. The LEIA images are 2048 × 2048 vs. DRACO’s 512 × 512 images in Terminal. The upper-right panel shows a 512 × 512 window of the LEIA image below. Comparing the two simulated DRACO images against the upper-right panel gives a good sense for what the finest-spatial-scale LEIA images will look like vs. the required and expected DRACO images.
Paper: Shape Modeling of Dimorphos for the Double Asteroid Redirection Test (DART)
Authors: R. Terik Daly, Carolyn M. Ernst, Olivier S. Barnouin, Robert W. Gaskell, Eric E. Palmer, Hari Nair, Ray C. Espiritu, Sarah Hasnain, Dany Waller, Angela M. Stickle, Michael C. Nolan, Josep M. Trigo-Rodríguez, Elisabetta Dotto, Alice Lucchetti, Maurizio Pajola, Simone Ieva, Patrick Michel
Figure caption: Shape model at various stages of development. Shape model development progresses left to right, top to bottom. In stages (f)–(h), the changes are subtle and primarily occur along the limb. This test is based on simulated images of the scaled-down version of Itokawa.
Paper: Shape Modeling of Dimorphos for the Double Asteroid Redirection Test (DART)
Authors: R. Terik Daly, Carolyn M. Ernst, Olivier S. Barnouin, Robert W. Gaskell, Eric E. Palmer, Hari Nair, Ray C. Espiritu, Sarah Hasnain, Dany Waller, Angela M. Stickle, Michael C. Nolan, Josep M. Trigo-Rodríguez, Elisabetta Dotto, Alice Lucchetti, Maurizio Pajola, Simone Ieva, Patrick Michel
Figure caption: Reconstructed shape models made from simulated images, colored by the type of information used to constrain the shape in a given area. Due to the limited images, only a fraction of the body could be tiled with maplets (gray regions). Limb points (blue) provided additional constraints in a few areas. Scattered points from a single limb (e.g., the Bennu_errors case) indicate errors in the shape model in that location. The bulk of the shape (yellow) was imaged at a high emission angle, was hidden in the dark, or represents unseen portions of the body.
Paper: Shape Modeling of Dimorphos for the Double Asteroid Redirection Test (DART)
Authors: R. Terik Daly, Carolyn M. Ernst, Olivier S. Barnouin, Robert W. Gaskell, Eric E. Palmer, Hari Nair, Ray C. Espiritu, Sarah Hasnain, Dany Waller, Angela M. Stickle, Michael C. Nolan, Josep M. Trigo-Rodríguez, Elisabetta Dotto, Alice Lucchetti, Maurizio Pajola, Simone Ieva, Patrick Michel
Figure caption: Differences in simulated DRACO images in the ideal and error Bennu cases. In the ideal case, there are no spacecraft uncertainties in the trajectory and the body is always centered in the image. In the error case, there is a ∼15 m spacecraft uncertainty and 0.1 mrad pointing uncertainty. In the error case, the body moves around in the camera frame, and the impact point is different than in the ideal case. Compare, for example, the positions of indicated features, as well as the location of the limb and terminator relative to the edges of the images, in the top (ideal) and bottom (error) rows. The times listed are the number of seconds before impact. The offsets are clearest in the T–3 seconds image. The impact sites are located at the center of the T–3 seconds image, in each respective case.
Paper: Shape Modeling of Dimorphos for the Double Asteroid Redirection Test (DART)
Authors: R. Terik Daly, Carolyn M. Ernst, Olivier S. Barnouin, Robert W. Gaskell, Eric E. Palmer, Hari Nair, Ray C. Espiritu, Sarah Hasnain, Dany Waller, Angela M. Stickle, Michael C. Nolan, Josep M. Trigo-Rodríguez, Elisabetta Dotto, Alice Lucchetti, Maurizio Pajola, Simone Ieva, Patrick Michel
Figure caption: Comparison between the simulated 66 cm-scale DRACO images (left), starter shape model (center), and final shape model (right). The final model matches the image much better than the starter model.
Paper: Shape Modeling of Dimorphos for the Double Asteroid Redirection Test (DART)
Authors: R. Terik Daly, Carolyn M. Ernst, Olivier S. Barnouin, Robert W. Gaskell, Eric E. Palmer, Hari Nair, Ray C. Espiritu, Sarah Hasnain, Dany Waller, Angela M. Stickle, Michael C. Nolan, Josep M. Trigo-Rodríguez, Elisabetta Dotto, Alice Lucchetti, Maurizio Pajola, Simone Ieva, Patrick Michel
Figure caption: Six views of the truth shape models used for shape models tests. Three truth models were used: (a) a triaxial ellipsoid, (b) a shrunken Itokawa, and (c) a shrunken Bennu. The view is sized to best fit each model; the models themselves are different sizes.