adsabs/AstroCLIMB huggingface dataset:
Paper: Physical and Mutual Orbit Characteristics of Near-Earth Binary Asteroid (163693) Atira
Authors: Aaron P. Deleon, Sean E. Marshall, Tracy M. Becker, Petr Pravec, Ellen S. Howell, Michael C. Nolan, Anne K. Virkki, Edgard G. Rivera-Valentín, Patrick A. Taylor, Bryce T. Bolin, Beth Aponte-Hernández, Israel Cabrera, Peter Kušnirák, Kamil Hornoch, Hana Kučáková
Figure caption: Observed lightcurves (red) and model lightcurves (black) of model 2. The observatory is indicated in parentheses in the individual lightcurve titles. For each panel, the shape model on the right is the simulated plane-of-sky image as observed during the middle of the observation. Note that lightcurves from different dates have different amplitudes, so these different frames are plotted with different ranges along their y-axes.
Paper: Analysis of Enceladus’s Time-variable Space Environment to Magnetically Sound its Interior
Authors: Joachim Saur, Stefan Duling, Alexander Grayver, Jamey R. Szalay
Figure caption: Improved predictability of primary inducing fields when PPO, eccentricity, and magnetospheric effects are included. Blue circles show residual background fields. Black crosses show fits including eccentricity, PPO, and LT effects within a current sheet. Orange, pink, and red symbols represent improved fits when the data are additionally binned into three seasonal blocks during the fitting process.
Paper: Analysis of Enceladus’s Time-variable Space Environment to Magnetically Sound its Interior
Authors: Joachim Saur, Stefan Duling, Alexander Grayver, Jamey R. Szalay
Figure caption: Anomaly dependence of residual magnetic fields stemming from the difference of the observed background magnetic fields and those of Saturn’s internal field and the PPOs (see Equation (2)). The residual fields are displayed as a function of the mean anomaly of the position of measurements by the Cassini spacecraft for either flybys or crossings of Enceladus’s eccentric orbit. The mean anomaly is the angle with respect to the location of Enceladus’s pericenter before the flyby. The mean anomaly is expressed as phase with values lying between 0 and 1, which corresponds to 0° and 360°. Values for selected flybys are shown as differently colored circles. The blue dashed curves display sinusoidal fits to the data with a free phase shift. The blue solid curves represent a sinusoidal fit with the phase shift fixed such that the maxima are at phase  = 0.5.
Paper: Analysis of Enceladus’s Time-variable Space Environment to Magnetically Sound its Interior
Authors: Joachim Saur, Stefan Duling, Alexander Grayver, Jamey R. Szalay
Figure caption: Induction amplitude and phase as a function of conductivity for a three-layer model consisting of a negligibly conducting crust (thickness 5 km), a conducting ocean (thickness 57 km), and a conducting core (radius 194 km). The conductivities of the core and the ocean are free parameters. The induction amplitude A and its phase are displayed for Saturn’s synodic rotation and orbital periods as a function of ocean and core conductivities.
Paper: Analysis of Enceladus’s Time-variable Space Environment to Magnetically Sound its Interior
Authors: Joachim Saur, Stefan Duling, Alexander Grayver, Jamey R. Szalay
Figure caption: Overview of flyby properties as a function of flyby number. The top panel displays Cassini’s distance from Enceladus at closest approach during flybys. The middle panel shows the distance of Enceladus from Saturn, with the orange line representing the average distance to Saturn. The bottom panel displays the expected amplitudes of the inducing field at the surface of Enceladus due to its eccentric orbit as blue circles. Red circles show an approximation for the expected induction amplitudes at closest approach taking into account the altitude of the flyby.
Paper: Analysis of Enceladus’s Time-variable Space Environment to Magnetically Sound its Interior
Authors: Joachim Saur, Stefan Duling, Alexander Grayver, Jamey R. Szalay
Figure caption: Trajectories of close north–south flybys En03, En04, and En05. The arrows indicate the direction of the Cassini spacecraft. Coordinates x, y, and z are in Enceladus IAU system rotated by ﹩{90}^{\circ }﹩ around the z-axis (definition see Section 5) with x approximately along Enceladus's orbital direction, y approximately towards Saturn, and z pointing north.
Paper: Analysis of Enceladus’s Time-variable Space Environment to Magnetically Sound its Interior
Authors: Joachim Saur, Stefan Duling, Alexander Grayver, Jamey R. Szalay
Figure caption: Search for dependence of residual magnetic fields on variability of Enceladus’s plume activity. Residual magnetic fields are the difference between the observed background magnetic fields and those of Saturn’s internal field and the PPOs. Enceladus plume activity is maximum when Enceladus is close to its apocenter (M. M. Hedman et al. 2013). The enhanced plasma production possibly generates a plasma pulse/max that will rotate with Saturn’s magnetic field. The residual fields are displayed as a function of distance with respect to the location of a possible plasma pulse/max.
Paper: Analysis of Enceladus’s Time-variable Space Environment to Magnetically Sound its Interior
Authors: Joachim Saur, Stefan Duling, Alexander Grayver, Jamey R. Szalay
Figure caption: Time dependence of residual magnetic fields stemming from the difference of the observed background magnetic fields and those of Saturn’s internal field and the PPOs (see Equation (2)). The observed magnetospheric background fields are for either flybys or crossings of Enceladus’s eccentric orbit shown as blue circles. Values for selected flybys are shown in differently colored circles. The blue curves display polynomial fits to the data.
Paper: Analysis of Enceladus’s Time-variable Space Environment to Magnetically Sound its Interior
Authors: Joachim Saur, Stefan Duling, Alexander Grayver, Jamey R. Szalay
Figure caption: Saturn LT dependence of residual magnetic fields stemming from the difference of the observed background magnetic fields and those of Saturn’s internal field and the PPOs (see Equation (2)). The observed magnetospheric background fields are for either flybys or crossings of Enceladus’s eccentric orbit. Values for selected flybys are shown as differently colored circles. The blue curves display sinusoidal fits to the data.
Paper: Analysis of Enceladus’s Time-variable Space Environment to Magnetically Sound its Interior
Authors: Joachim Saur, Stefan Duling, Alexander Grayver, Jamey R. Szalay
Figure caption: Data coverage with respect to time, Saturn LT, and mean anomaly during which Cassini measurements at Enceladus’s flybys or at orbit crossings were obtained. Orange circles represent flybys, and blue circles represent orbit crossings.
Paper: Analysis of Enceladus’s Time-variable Space Environment to Magnetically Sound its Interior
Authors: Joachim Saur, Stefan Duling, Alexander Grayver, Jamey R. Szalay
Figure caption: Finite conductivity study for flyby En13. In the labels displaying conductivities, the first number is the conductivity of the ocean and the second number (after “&”) is the conductivity of the core. The observed B  z  component in blue is artificially shifted to directly cross-compare the local observed magnetic field perturbations with the modeled induced fields. The vertical olive-brown arrow displays the contribution due to thermal pressure, and the horizontal dashed lines represent its associated uncertainties. The gray area shows exemplarily the uncertainty range around the 5 & 25 S m–1 case. The sum of our modeled induced fields (gray region) and the magnetic pressure (brown arrow) including their uncertainties is sufficient to account for the observed perturbations shown in blue.
Paper: Analysis of Enceladus’s Time-variable Space Environment to Magnetically Sound its Interior
Authors: Joachim Saur, Stefan Duling, Alexander Grayver, Jamey R. Szalay
Figure caption: Finite conductivity study for flyby En12. In the labels displaying conductivities, the first number is the conductivity of the ocean and the second number (after “&”) is the conductivity of the core. The observed B  z  component in blue is artificially shifted to directly cross-compare the local observed magnetic field perturbations with the modeled induced fields. The vertical olive-brown arrow displays the contribution due to thermal pressure, and the horizontal dashed lines represent its associated uncertainties. The gray area shows exemplarily the uncertainty range around the 5 & 25 S m–1 case. The sum of our modeled induced fields (gray region) and the magnetic pressure (brown arrow) including their uncertainties is sufficient to account for the observed perturbations shown in blue.
Paper: Analysis of Enceladus’s Time-variable Space Environment to Magnetically Sound its Interior
Authors: Joachim Saur, Stefan Duling, Alexander Grayver, Jamey R. Szalay
Figure caption: North polar flyby En13: magnetic field perturbations (blue) in rotated Enceladus IAU coordinates and standard IAU coordinates in parentheses. Colored lines referenced in the left legend display modeled induced fields for a perfectly conducting moon based on different models/components of the primary inducing field. The terminology is introduced in Section 3 and also used in Table 2. Near closest approach magnetic field perturbations are present, which could be consistent with modeled induced field.
Paper: Analysis of Enceladus’s Time-variable Space Environment to Magnetically Sound its Interior
Authors: Joachim Saur, Stefan Duling, Alexander Grayver, Jamey R. Szalay
Figure caption: North polar flyby En12: magnetic field perturbations (blue) in rotated Enceladus IAU coordinates and standard IAU coordinates in parentheses. Colored lines referenced in the left legend display modeled induced fields for a perfectly conducting moon based on different models/components of the primary inducing field. The terminology is introduced in Section 3 and also used in Table 2. Near closest approach magnetic field perturbations are present, which could be consistent with modeled induced field.
Paper: Analysis of Enceladus’s Time-variable Space Environment to Magnetically Sound its Interior
Authors: Joachim Saur, Stefan Duling, Alexander Grayver, Jamey R. Szalay
Figure caption: Conductivity range of Enceladus’s ocean. Both panels show conductivities as a function of salinity and temperature for an ocean assumed to contain only NaCl (left) or a composition similar to seawater on Earth, i.e., based on the thermodynamic equation of state of seawater TEOS-10 (right). The red boxes show the parameter range expected based on current observations and geophysical understanding of Enceladus (more see text).
Paper: Analysis of Enceladus’s Time-variable Space Environment to Magnetically Sound its Interior
Authors: Joachim Saur, Stefan Duling, Alexander Grayver, Jamey R. Szalay
Figure caption: North–south flyby for En05: magnetic field perturbations (blue) in rotated Enceladus IAU coordinates and standard IAU coordinates in parentheses. Colored lines referenced in the left legend display modeled induced fields for a perfectly conducting moon based on different models/components of the primary inducing field. The terminology is introduced in Section 3 and also used in Table 2. Near closest approach magnetic field perturbations are present, which could be consistent with modeled induced field.
Paper: Analysis of Enceladus’s Time-variable Space Environment to Magnetically Sound its Interior
Authors: Joachim Saur, Stefan Duling, Alexander Grayver, Jamey R. Szalay
Figure caption: North–south flyby En04: magnetic field perturbations (blue) in rotated Enceladus IAU coordinates and standard IAU coordinates in parentheses. Colored lines referenced in the left legend display modeled induced fields for a perfectly conducting moon based on different models/components of the primary inducing field. The terminology is introduced in Section 3 and also used in Table 2. Near closest approach magnetic field perturbations are present, which could be consistent with modeled induced field.
Paper: Analysis of Enceladus’s Time-variable Space Environment to Magnetically Sound its Interior
Authors: Joachim Saur, Stefan Duling, Alexander Grayver, Jamey R. Szalay
Figure caption: North–south flyby En03: magnetic field perturbations in rotated Enceladus IAU coordinates and standard IAU coordinates in parentheses. Colored lines referenced in the left legend display modeled induced fields for a perfectly conducting moon based on different models/components of the primary inducing field. The terminology is introduced in Section 3 and also used in Table 2.
Paper: Analysis of Enceladus’s Time-variable Space Environment to Magnetically Sound its Interior
Authors: Joachim Saur, Stefan Duling, Alexander Grayver, Jamey R. Szalay
Figure caption: Trajectories of the close north polar flybys En12 and En13. The arrows indicate the direction of the Cassini spacecraft. Coordinates x, y, and z are in Enceladus IAU system rotated by ﹩{90}^{\circ }﹩ around the z-axis (definition see Section 5) with x approximately along Enceladus's orbital direction, y approximately towards Saturn, and z pointing north.
Paper: Analysis of Enceladus’s Time-variable Space Environment to Magnetically Sound its Interior
Authors: Joachim Saur, Stefan Duling, Alexander Grayver, Jamey R. Szalay
Figure caption: Simulated magnetic field perturbations over Enceladus’s north polar region obtained with idealized MHD modeling. Simulation setups are summarized in Table B1.
Paper: Statistical Analysis of Near-surface Structure and Material Properties on Momentum Transfer in Rubble Pile Targets Impacted by Kinetic Impactors
Authors: Mallory E. DeCoster, Angela M. Stickle, Emma S. G. Rainey, Dawn M. Graninger
Figure caption: (a) The impact site is defined by a 12 m wide, 6 m tall area illustrated by the gray textured box; the impact point is located at x = 0.0 m, y = 81.5 m. (b) Results showing the ratio (R) of the volume of the matrix material (V matrix) to the total volume of the impact site area (V total) for each rubble pile target. Targets falling into the large boulder category are identified manually, and a ratio of 0.4 is used to distinguish between the matrix and small boulder target categories. (c)–(d) Zoomed-in images of the cross-sectional views of three exemplar 2DC rubble pile targets that are representative of each impact site structure category: (c) matrix material; (d) large boulders; (e) small boulders. The multicolored circles are boulders (specific colors have no further meaning), the light gray material represents the matrix material, and the dark gray cylinder is the projectile.
Paper: Analysis of Enceladus’s Time-variable Space Environment to Magnetically Sound its Interior
Authors: Joachim Saur, Stefan Duling, Alexander Grayver, Jamey R. Szalay
Figure caption: Bulk conductivity range of Enceladus’s core as a function of its porosity and temperature for various assumptions about its salinity. The two-phase system fluid is NaCl–H2O.
Paper: Analysis of Enceladus’s Time-variable Space Environment to Magnetically Sound its Interior
Authors: Joachim Saur, Stefan Duling, Alexander Grayver, Jamey R. Szalay
Figure caption: South polar flyby En14: magnetic field perturbations (blue) in rotated Enceladus IAU coordinates and standard IAU coordinates in parentheses. Colored lines referenced in the left legend display modeled induced fields for a perfectly conducting moon based on different models/components of the primary inducing field. The terminology is introduced in Section 3 and also used in Table 2.
Paper: Analysis of Enceladus’s Time-variable Space Environment to Magnetically Sound its Interior
Authors: Joachim Saur, Stefan Duling, Alexander Grayver, Jamey R. Szalay
Figure caption: South polar flyby En19: magnetic field perturbations (blue) in rotated Enceladus IAU coordinates and standard IAU coordinates in parentheses. Colored lines referenced in the left legend display modeled induced fields for a perfectly conducting moon based on different models/components of the primary inducing field. The terminology is introduced in Section 3 and also used in Table 2.
Paper: Analysis of Enceladus’s Time-variable Space Environment to Magnetically Sound its Interior
Authors: Joachim Saur, Stefan Duling, Alexander Grayver, Jamey R. Szalay
Figure caption: Trajectories of the close south polar flybys En14, En17, En18, and En19. The arrows indicate the direction of the Cassini spacecraft. Coordinates x, y, and z are in Enceladus IAU system rotated by ﹩{90}^{\circ }﹩ around the z-axis (definition see Section 5) with x approximately along Enceladus's orbital direction, y approximately towards Saturn, and z pointing north.
Paper: Analysis of Enceladus’s Time-variable Space Environment to Magnetically Sound its Interior
Authors: Joachim Saur, Stefan Duling, Alexander Grayver, Jamey R. Szalay
Figure caption: South polar flyby En18: magnetic field perturbations (blue) in rotated Enceladus IAU coordinates and standard IAU coordinates in parentheses. Colored lines referenced in the left legend display modeled induced fields for a perfectly conducting moon based on different models/components of the primary inducing field. The terminology is introduced in Section 3 and also used in Table 2.
Paper: Analysis of Enceladus’s Time-variable Space Environment to Magnetically Sound its Interior
Authors: Joachim Saur, Stefan Duling, Alexander Grayver, Jamey R. Szalay
Figure caption: South polar flyby En17: magnetic field perturbations (blue) in rotated Enceladus IAU coordinates and standard IAU coordinates in parentheses. Colored lines referenced in the left legend display modeled induced fields for a perfectly conducting moon based on different models/components of the primary inducing field. The terminology is introduced in Section 3 and also used in Table 2.
Paper: Statistical Analysis of Near-surface Structure and Material Properties on Momentum Transfer in Rubble Pile Targets Impacted by Kinetic Impactors
Authors: Mallory E. DeCoster, Angela M. Stickle, Emma S. G. Rainey, Dawn M. Graninger
Figure caption:  β vs. the ratio of the volume of the matrix material (V matrix) to the total volume (V total) of the impact site. (a) The data are plotted according to their impact site categories with a linear fit (blue line). The range of results from S. D. Raducan et al. (2022) are plotted as dark yellow vertical lines (note that S. D. Raducan et al.'s (2022) results report V matrix/V total for the full target). The boulder packing regimes defined by S. D. Raducan et al. (2022) are also shown: high boulder packing (>35% of the target mass is from boulders) and loose boulder packing (<20% of the target mass is from boulders). Note that S. D. Raducan et al.'s (2022) boulders have similar cohesion (100 MPa) to what is studied here, but weaker (Y o = 0 Pa) matrix material, and both their boulders and matrix contained 35% porosity. (b) The data are organized according to their impact site category and how their matrix material was defined (20% or 60% porosity, and GEO or BDL model with respective cohesions (Y o)). We use a V matrix/V total ratio of 0.4 to delineate between rubble pile target impact site categories. All targets with boulders >6 m at the impact point were sorted into the large boulders category.
Paper: Statistical Analysis of Near-surface Structure and Material Properties on Momentum Transfer in Rubble Pile Targets Impacted by Kinetic Impactors
Authors: Mallory E. DeCoster, Angela M. Stickle, Emma S. G. Rainey, Dawn M. Graninger
Figure caption: Box plots results for β where data are separated according to (top row) matrix material parameters (note the porosity (%), cohesion (Y o), and constitutive model (GEO or BDL) representing the matrix material within each target type listed in the top-right corner), and (bottom row) impact site structures.
Paper: Statistical Analysis of Near-surface Structure and Material Properties on Momentum Transfer in Rubble Pile Targets Impacted by Kinetic Impactors
Authors: Mallory E. DeCoster, Angela M. Stickle, Emma S. G. Rainey, Dawn M. Graninger
Figure caption: Box plots results for the transient crater width separated according to (top row) matrix material parameters (note the porosity (%), cohesion (Y o), and constitutive model (GEO or BDL) representing the matrix material within each target type listed in the top-right corner), and (bottom row) impact site structures. The data represent the transient crater 500 ms post impact where the transient crater is no longer evolving (see Figure A5 in the SI for details).
Paper: Statistical Analysis of Near-surface Structure and Material Properties on Momentum Transfer in Rubble Pile Targets Impacted by Kinetic Impactors
Authors: Mallory E. DeCoster, Angela M. Stickle, Emma S. G. Rainey, Dawn M. Graninger
Figure caption: Illustrations of eight rubble pile targets resulting in the smallest β values. For each image, the case number corresponding to Table A1 is listed in the top-left corner, and the impact condition, percent porosity of the matrix material, and constitutive model (GEO models contain Y o = 10 Pa, and BDL models contain Y o = 100 kPa) are indicated as figure captions where “LB” = large boulder, “SB” = small boulder, and “M” = matrix. Each illustration shows the initial conditions of the simulation on the left (t = 0). The damage profile of the boulders at t = 150 ms is shown on the right side of each image in addition to the outline of the transient crater (t = 500 ms). Full damage (damage = 1) occurs in the matrix material over the full extent of the area that is depicted; however, it is not shown for clarity.
Paper: Statistical Analysis of Near-surface Structure and Material Properties on Momentum Transfer in Rubble Pile Targets Impacted by Kinetic Impactors
Authors: Mallory E. DeCoster, Angela M. Stickle, Emma S. G. Rainey, Dawn M. Graninger
Figure caption:  β vs. number of boulders ejected. The same data are plotted but color coded differently according to (a) the porosity (ϕ) and material model/strength (GEO models contain Y o = 10 Pa, and BDL models contain Y o = 100 kPa) that represent the matrix material, and (b) by the impact site structure. Specific rubble pile cases are also identified by their case number.
Paper: Statistical Analysis of Near-surface Structure and Material Properties on Momentum Transfer in Rubble Pile Targets Impacted by Kinetic Impactors
Authors: Mallory E. DeCoster, Angela M. Stickle, Emma S. G. Rainey, Dawn M. Graninger
Figure caption: Results from the resolution study of three rubble pile targets representing the three impact site categories (matrix, large boulders, and small boulders) where the matrix material is modeled as 20% porous GEO (Y o = 10 Pa). The left plots show β vs. time for different grid resolutions (cppr), and the right plots show the transient crater width and depth measurements at different times post impact. (a) and (b) show the results for case 15, which represents a matrix-rich impact site; (c) and (d) show the results for case 3, which represents a large boulder impact site; and (e) and (f) show the results for case 19, which represents the small boulder impact site category.
Paper: Statistical Analysis of Near-surface Structure and Material Properties on Momentum Transfer in Rubble Pile Targets Impacted by Kinetic Impactors
Authors: Mallory E. DeCoster, Angela M. Stickle, Emma S. G. Rainey, Dawn M. Graninger
Figure caption: Illustrations of seven of the rubble pile targets resulting in the highest βs. For each image, the case number corresponding to Table A1 is listed in the top-left corner, and the impact site category (where “M” = matrix), percent porosity of the matrix material percent, and constitutive model (GEO models contain Y o = 10 Pa, and BDL models contain Y o = 100 kPa) are indicated as figure captions. Each illustration shows the initial conditions of the simulation on the left (t = 0) where the matrix material is represented in gray and the boulders are multicolored. The damage profile of the boulders at t = 150 ms is shown on the right side of each image in addition to the outline of the transient crater (t = 500 ms). Full damage (damage = 1) occurs in the matrix material over the full extent of the area that is depicted; however, it is not shown for clarity.