adsabs/AstroCLIMB huggingface dataset:
Paper: Electrostatic Repulsion of Dust from Planetary Surfaces
Authors: F. Chioma Onyeagusi, Felix Jungmann, Jens Teiser, Gerhard Wurm
Figure caption: Distance of an aggregate to an electrode (located at top horizontal axis) over time. Four different regions are marked: (1) accelerated approach due to Coulomb attraction; (2) approach after bouncing with the same polarity; (3) sticking on the electrode; (4) accelerated repulsion due to Coulomb force with the opposite polarity. Parabolic fits are plotted for regions 1, 2, and 4.
Paper: Electrostatic Repulsion of Dust from Planetary Surfaces
Authors: F. Chioma Onyeagusi, Felix Jungmann, Jens Teiser, Gerhard Wurm
Figure caption: Time series of aggregates observed during the drop-tower experiments at one of the copper electrodes (bottom). Particles appear twice due to the copper’s high reflectivity. Upon sticking, small aggregates remain stuck while large aggregates recharge and are repelled. Here, the trajectory of one aggregate is marked showing a rebound, sticking and repulsion after recharging at the electrode within the electric field.
Paper: Electrostatic Repulsion of Dust from Planetary Surfaces
Authors: F. Chioma Onyeagusi, Felix Jungmann, Jens Teiser, Gerhard Wurm
Figure caption: Schematics of the experiment setup (from Steinpilz et al. 2020a).
Paper: Electrostatic Repulsion of Dust from Planetary Surfaces
Authors: F. Chioma Onyeagusi, Felix Jungmann, Jens Teiser, Gerhard Wurm
Figure caption: Composite microscope image of a dust aggregate. Individual dust grains of the compact aggregate are visible as granular texture.
Paper: The Solar Wind Interaction with (1) Ceres: The Role of Interior Conductivity
Authors: A. R. Poppe, S. Fatemi
Figure caption: Hybrid model results for Runs A and Runs B1−3 in the x–y plane, including the solar wind density, solar wind velocity, and magnitude of the interplanetary magnetic field, each normalized to their respective upstream value. These results demonstrate that the inclusion of moderate conductivities within the mantle of Ceres are capable of producing plasma and magnetic field perturbations outside of Ceres.
Paper: The Solar Wind Interaction with (1) Ceres: The Role of Interior Conductivity
Authors: A. R. Poppe, S. Fatemi
Figure caption: Hybrid model results for Run D in the x–y plane, including the (a) solar wind density, (b) solar wind velocity, (c) magnitude of the interplanetary magnetic field with plasma interactions with Ceres, (d) magnitude of the unipolar magnetic field, and (e) magnitude of the total magnetic field. As discussed further in the text, these results demonstrate that the inclusion of unipolar currents within Ceres have only a very minor effect on the overall interaction of Ceres with the solar wind.
Paper: The Solar Wind Interaction with (1) Ceres: The Role of Interior Conductivity
Authors: A. R. Poppe, S. Fatemi
Figure caption: A graphical depiction of the various internal conductivity structures modeled for each set of runs. Runs A and B1 are single-layer models for Ceres with low and moderate internal conductivity, respectfully. Runs B2−B5 explore two-layer models (crust + mantle), while Runs C1−C3 explore three-layer (crust + ocean + mantle) models. Run D explores a single-layer model with contributions from unipolar currents. Radial distances are in units of kilometers and conductivities are in units of siemens per meter.
Paper: The Solar Wind Interaction with (1) Ceres: The Role of Interior Conductivity
Authors: A. R. Poppe, S. Fatemi
Figure caption: Hybrid model results for Runs B3−5 in the x–y plane, including the solar wind density, solar wind velocity, and magnitude of the interplanetary magnetic field, each normalized to their respective upstream value. Note that the relative magnetic field is displayed logarithmically to aid in comparison. These results demonstrate that changes in the upstream plasma conditions can yield variations in Ceres’ interaction with the solar wind, even for constant-interior-conductivity models.
Paper: The Solar Wind Interaction with (1) Ceres: The Role of Interior Conductivity
Authors: A. R. Poppe, S. Fatemi
Figure caption: Hybrid model results for Runs C1−3 in the x–y plane, including the (left) solar wind density, (center) solar wind velocity, and (right) magnitude of the interplanetary magnetic field, each normalized to their respective upstream value. As discussed further in the text, these results demonstrate from a time-independent perspective that inclusion of an ocean as a third layer does not significantly change the overall interaction of Ceres with the solar wind, as compared to the two-layer model results shown in Figures 3 and 4.
Paper: The Solar Wind Interaction with (1) Ceres: The Role of Interior Conductivity
Authors: A. R. Poppe, S. Fatemi
Figure caption: Hybrid model results for Run A in the (a)–(c) x–y and (d)–(f) x–z planes, including the solar wind density, solar wind velocity, and magnitude of the interplanetary magnetic field, each normalized to their respective upstream value. Spatial axes are normalized to units of Ceres radii, R  C  = 735 km. These results model a completely inert and resistive object in the solar wind as a baseline for comparison.
Paper: Thin-shell Tidal Dynamics of Ocean Worlds
Authors: Marc Rovira-Navarro, Isamu Matsuyama, Hamish C. F. C Hay
Figure caption: Ocean tidal dissipation patterns for Enceladus for an unstratified ocean due to the eccentricity and obliquity tide (panels (a) and (b)) and two resonant stratified configurations (panels (c) and (d)). In all cases the dissipation pattern is symmetric with respect to the equator and the 0° meridian.
Paper: Thin-shell Tidal Dynamics of Ocean Worlds
Authors: Marc Rovira-Navarro, Isamu Matsuyama, Hamish C. F. C Hay
Figure caption: Effect of a nonrigid mantle in the tidal response of the ocean and shell. ﹩{\hat{\mu }}_{m}﹩ is computed assuming a Young modulus for the core of E = 170 GPa for all moons except for the mid-sized Saturnian moons, for which we assume a soft deformable core, E = 17 GPa. The core is considered to be homogeneous, and its density is calculated self-consistently to satisfy the mean density constrain.
Paper: Thin-shell Tidal Dynamics of Ocean Worlds
Authors: Marc Rovira-Navarro, Isamu Matsuyama, Hamish C. F. C Hay
Figure caption: Tidal dissipation in an Enceladan ocean of variable thickness obtained with the method presented in this article (solid lines; Section 2.2) and the FEM method used in Rovira-Navarro et al. (2020; filled circles). The comparison is done by turning off self-gravity.
Paper: Thin-shell Tidal Dynamics of Ocean Worlds
Authors: Marc Rovira-Navarro, Isamu Matsuyama, Hamish C. F. C Hay
Figure caption: Inclination damping timescale for different satellites of the solar system for oceans of uniform thickness (panel (a)) and with degree 2 thickness variations (panel (b)). Panel (a) shows inclination damping timescales as a function of the ocean’s damping coefficient (﹩\hat{\alpha }﹩). The value of ﹩\hat{\alpha }﹩ for which the minimum damping timescale is attained and the intervals for which it is below the age of the solar system are indicated with thick and thin marks, respectively. In panel (b) the change in inclination damping timescale as a function of degree 2 ocean thickness variations is shown for the Moon, Titan, and Callisto. In the three cases the ﹩\hat{\alpha }﹩ for which the inclination damping timescale is minimum is used. For the Moon we compute the damping timescale early during its evolution when it had magma ocean and was closer to Earth (a = 20R Earth). The dashed red line indicates the age of the solar system.
Paper: Thin-shell Tidal Dynamics of Ocean Worlds
Authors: Marc Rovira-Navarro, Isamu Matsuyama, Hamish C. F. C Hay
Figure caption: Nondimensional energy dissipation in an unstratified ocean of constant thickness due to the eccentricity and the obliquity tide as a function of Lamb parameter ϵ and effective rigidity γ (panels (a) and (b)) and the inverse of the damping timescale ﹩\hat{\alpha }﹩ (panels (c) and (d)). Bending effects and self-gravity are neglected and a cutoff degree of 30 is used. (e) Dimensional tidal dissipation is computed using the values given in Table 2 and assuming ﹩\hat{\alpha }={10}^{-3}﹩.
Paper: Thin-shell Tidal Dynamics of Ocean Worlds
Authors: Marc Rovira-Navarro, Isamu Matsuyama, Hamish C. F. C Hay
Figure caption: Nondimensional energy dissipation in a two-layer stratified ocean of constant thickness as a function of density contrast (1 − r = 1 − ρ 1/ρ 2) and layer partition ﹩{\hat{c}}_{1}^{2}={H}_{1}/{H}_{\mathrm{ocean}}﹩ for different combinations of Lamb parameter ϵ and effective rigidity γ (Table 1). Panels (a) and (d) are obtained for values approximately representative of Enceladus and Europa, ﹩\hat{\alpha }={10}^{-3}﹩, ﹩{\hat{D}}^{(b)}=0﹩, and ξ = 0.
Paper: Thin-shell Tidal Dynamics of Ocean Worlds
Authors: Marc Rovira-Navarro, Isamu Matsuyama, Hamish C. F. C Hay
Figure caption: Nondimensional energy dissipation in an unstratified ocean with degree 2 (panels (a) and (b)) and 3 (panels (c) and (d)) ocean thickness variations. Self-gravity is neglected, and a surface ocean is assumed, ﹩(\xi ,\gamma ,{\hat{D}}^{b})=0﹩; we use ﹩\hat{\alpha }={10}^{-3}﹩. A cutoff degree of 30 is used. The case corresponding to an ocean of constant thickness (﹩{\hat{c}}_{2,0}^{2}={\hat{c}}_{3,0}^{2}=0﹩) is indicated with a white dashed horizontal line.
Paper: Thin-shell Tidal Dynamics of Ocean Worlds
Authors: Marc Rovira-Navarro, Isamu Matsuyama, Hamish C. F. C Hay
Figure caption: Tidal dissipation in Enceladus’s ocean as a function of Rayleigh coefficient and ocean stratification. The thermal output of Enceladus’s south polar terrain is indicated in red (Howett et al. 2011). In all cases, we truncate the system at l = 60.
Paper: Thin-shell Tidal Dynamics of Ocean Worlds
Authors: Marc Rovira-Navarro, Isamu Matsuyama, Hamish C. F. C Hay
Figure caption: Tidal dissipation due to a degree 2 order 1 forcing as a function of forcing frequency and amplitude of ocean thickness variation. For this plot ﹩\hat{\alpha }={10}^{-3}﹩, ϵ = 10−2, γ = 0, ξ = 0, and ﹩{\hat{D}}^{(b)}=0﹩. The dashed lines indicate ﹩{\hat{c}}_{2,0}^{2}=0﹩ and ﹩\hat{\omega }=1﹩.
Paper: Thin-shell Tidal Dynamics of Ocean Worlds
Authors: Marc Rovira-Navarro, Isamu Matsuyama, Hamish C. F. C Hay
Figure caption: A two-layer ocean overlaid by a solid shell of variable thickness. Dashed and solid lines correspond to the unperturbed and perturbed states, respectively.
Paper: Thin-shell Tidal Dynamics of Ocean Worlds
Authors: Marc Rovira-Navarro, Isamu Matsuyama, Hamish C. F. C Hay
Figure caption: Tidal deformation of Enceladus’s ice shell. (a) Surface displacements at t = 0 for an ice shell of uniform (gray) and variable thickness (blue); (b) meridional cut at zero longitude; (c) displacements at the south pole over a tidal period. In all cases, an elastic ice shell is assumed.
Paper: Exploring and Validating Exoplanet Atmospheric Retrievals with Solar System Analog Observations
Authors: Tyler D. Robinson, Arnaud Salvador
Figure caption: Planetary geometric (A  g ;  solid lines) and spherical (A  s ;  dashed lines) albedo as a function of single-scattering albedo from Heng et al. (2021) and rfast for an infinitely deep atmosphere whose medium obeys a Henyey–Greenstein scattering phase function of asymmetry parameter 0.508 (selected to reproduce population-level results for hot Jupiters by Heng et al. 2021).
Paper: Exploring and Validating Exoplanet Atmospheric Retrievals with Solar System Analog Observations
Authors: Tyler D. Robinson, Arnaud Salvador
Figure caption: Reflection spectra for a partially clouded (50% cloud coverage) Earth-like case from the rfast (gray) and SMART (yellow) models. The left panel is for a single-scene, plane-parallel setup. The right panel is for a three-dimensional treatment where plane-parallel calculations are run for pixels on the planetary disk and then spatially integrated.
Paper: Exploring and Validating Exoplanet Atmospheric Retrievals with Solar System Analog Observations
Authors: Tyler D. Robinson, Arnaud Salvador
Figure caption: Layer reflectivity (top left), transmissivity (top right), and emissivity (bottom) as a function of layer extinction optical depth in the rfast model (gray lines) vs. detailed calculations from Hunt (1973) (yellow lines). Limiting cases of pure absorption and forward scattering are considered, where layers have no reflectivity in the pure absorption case.
Paper: Exploring and Validating Exoplanet Atmospheric Retrievals with Solar System Analog Observations
Authors: Tyler D. Robinson, Arnaud Salvador
Figure caption: Transit spectra for a clear-sky Earth-like case from the rfast (gray) and SMART (yellow) models. Scenarios that both include (dashed) and exclude (solid) refraction are shown.
Paper: Exploring and Validating Exoplanet Atmospheric Retrievals with Solar System Analog Observations
Authors: Tyler D. Robinson, Arnaud Salvador
Figure caption: Simulated visible-wavelength reflected light observation of an exo-Earth at resolving power of 140 and a V-band S/N of 20 (points and associated error bars, after Feng et al. 2018). Forward model spread from retrieval analysis as applied to the simulated observation is shown as darker and lighter swaths for 16th–84th and 5th–95th percentiles, respectively.
Paper: Exploring and Validating Exoplanet Atmospheric Retrievals with Solar System Analog Observations
Authors: Tyler D. Robinson, Arnaud Salvador
Figure caption: Phase-dependent planetary reflectivity for infinitely deep Rayleigh and isotropic scattering atmospheres from Madhusudhan & Burrows (2012) as compared to rfast.
Paper: Exploring and Validating Exoplanet Atmospheric Retrievals with Solar System Analog Observations
Authors: Tyler D. Robinson, Arnaud Salvador
Figure caption: Thermal emission spectra for a clear-sky Earth-like case from the rfast (gray) and SMART (yellow) models.
Paper: Exploring and Validating Exoplanet Atmospheric Retrievals with Solar System Analog Observations
Authors: Tyler D. Robinson, Arnaud Salvador
Figure caption: Titan transit spectrum derived from Cassini-VIMS observations (from Robinson et al. 2014). Adopted error bars are 0.1 ppm and are constant with wavelength, as justified in the text. Forward model spread from retrieval analysis is shown as darker and lighter swaths for 16th–84th and 5th–95th percentiles, respectively.
Paper: Exploring and Validating Exoplanet Atmospheric Retrievals with Solar System Analog Observations
Authors: Tyler D. Robinson, Arnaud Salvador
Figure caption: Visualized posterior distribution for a 13-parameter fit to the Cassini-VIMS Titan observations (Figure 17). One-dimensional marginal distributions are shown along the diagonal, with associated 16th/50th/84th percentile values indicated above and shown by the vertical dashed lines. Fiducial “truth” values from which the Figure 17 observed spectrum is obtained are indicated with the vertical solid lines.
Paper: Exploring and Validating Exoplanet Atmospheric Retrievals with Solar System Analog Observations
Authors: Tyler D. Robinson, Arnaud Salvador
Figure caption: Visualized posterior distribution for a 13-parameter fit to the S/N = 20 EPOXI Earth observations in Figure 11. One-dimensional marginal distributions are shown along the diagonal, with associated 16th/50th/84th percentile values indicated above and with vertical dashed lines. When relevant a priori values are well known, a vertical line indicates the characteristic “truth” value for Earth.
Paper: Exploring and Validating Exoplanet Atmospheric Retrievals with Solar System Analog Observations
Authors: Tyler D. Robinson, Arnaud Salvador
Figure caption: Visualized posterior distribution for a 12-parameter fit to the MGS-TES Earth observations in Figure 14. One-dimensional marginal distributions are shown along the diagonal, with associated 16th/50th/84th percentile values indicated above and with the vertical dashed lines.
Paper: Exploring and Validating Exoplanet Atmospheric Retrievals with Solar System Analog Observations
Authors: Tyler D. Robinson, Arnaud Salvador
Figure caption: Gas mixing ratio constraints from retrievals performed on the Cassini/VIMS-derived transit spectrum for Titan shown in Figure 17. Gases are represented with different colors, and vertical lines indicate known “truth” values, when available.
Paper: Exploring and Validating Exoplanet Atmospheric Retrievals with Solar System Analog Observations
Authors: Tyler D. Robinson, Arnaud Salvador
Figure caption: Comparison between the retrieved best-fit model from the single-cloud retrievals in Figure A3 (red) and a demonstration with a two-cloud model and a realistic Earth thermal structure profile (yellow).
Paper: Exploring and Validating Exoplanet Atmospheric Retrievals with Solar System Analog Observations
Authors: Tyler D. Robinson, Arnaud Salvador
Figure caption: Same as Figure A1, except that the underlying EPOXI Earth observations have been degraded to a V-band S/N of 10.
Paper: Electrostatic Repulsion of Dust from Planetary Surfaces
Authors: F. Chioma Onyeagusi, Felix Jungmann, Jens Teiser, Gerhard Wurm
Figure caption: Number–size distribution of the milled dust grains that were used to form aggregates as measured by a Mastersizer 3000 by means of wet dispersion.
Paper: Electrostatic Repulsion of Dust from Planetary Surfaces
Authors: F. Chioma Onyeagusi, Felix Jungmann, Jens Teiser, Gerhard Wurm
Figure caption: Charge transfer in a sticking event depending on sticking time. Dashed lines roughly mark the range of times during which ejections of the large grains occur. Ejection of smaller grains is slightly shifted to larger time intervals.
Paper: Electrostatic Repulsion of Dust from Planetary Surfaces
Authors: F. Chioma Onyeagusi, Felix Jungmann, Jens Teiser, Gerhard Wurm
Figure caption: Recharging at the electrodes in sticking collisions. Negatively charged grains recharge positively at the positive electrode and vice versa.
Paper: Electrostatic Repulsion of Dust from Planetary Surfaces
Authors: F. Chioma Onyeagusi, Felix Jungmann, Jens Teiser, Gerhard Wurm
Figure caption: Initial charge distribution measured after grains entered the capacitor.
Paper: Electrostatic Repulsion of Dust from Planetary Surfaces
Authors: F. Chioma Onyeagusi, Felix Jungmann, Jens Teiser, Gerhard Wurm
Figure caption: Charge distribution after recharging on electrodes once grains are ejected after sticking.
Paper: Electrostatic Repulsion of Dust from Planetary Surfaces
Authors: F. Chioma Onyeagusi, Felix Jungmann, Jens Teiser, Gerhard Wurm
Figure caption: Charge on aggregates before and after a bouncing collision. The dashed line marks charge conservation.
Paper: Electrostatic Repulsion of Dust from Planetary Surfaces
Authors: F. Chioma Onyeagusi, Felix Jungmann, Jens Teiser, Gerhard Wurm
Figure caption: Comparison of the precharge on grains and the charge gained during recharge at the electrodes.
Paper: Surviving in Ocean Worlds: Experimental Characterization of Fiber Optic Tethers across Europa-like Ice Faults and Unraveling the Sliding Behavior of Ice
Authors: Vishaal Singh, Christine McCarthy, Matthew Silvia, Michael V. Jakuba, Kathleen L. Craft, Alyssa R. Rhoden, Chris German, Theodore A. Koczynski
Figure caption: (a) LN-cooled biaxial apparatus at LDEO. Tethers were frozen into ice and loads applied as indicated by arrows. Ends of tethers were wrapped around mandrels and passed through the cryostat for monitoring for optical performance. (b) Schematic of the cryostat and load trains (vertical and horizontal) in cross section, showing the double-direct shear configuration of the testing central ice sample and two stationary ice samples with/without tethers.
Paper: Surviving in Ocean Worlds: Experimental Characterization of Fiber Optic Tethers across Europa-like Ice Faults and Unraveling the Sliding Behavior of Ice
Authors: Vishaal Singh, Christine McCarthy, Matthew Silvia, Michael V. Jakuba, Kathleen L. Craft, Alyssa R. Rhoden, Chris German, Theodore A. Koczynski
Figure caption: Custom sample assembly that allowed pretensioned tethers to be frozen into ice. A small layer of lubrication between central (4.95 × 4.95 × 4.95 cm) and side blocks (3.30 × 4.95 × 4.95 cm), along with the geometry of forcing, causes the ice to break along the dashed lines and shear the tether during loading.
Paper: Surviving in Ocean Worlds: Experimental Characterization of Fiber Optic Tethers across Europa-like Ice Faults and Unraveling the Sliding Behavior of Ice
Authors: Vishaal Singh, Christine McCarthy, Matthew Silvia, Michael V. Jakuba, Kathleen L. Craft, Alyssa R. Rhoden, Chris German, Theodore A. Koczynski
Figure caption: Ice sample fabrication protocol. Polycrystalline ice blocks of controlled grain size, porosity, and impurity content are fabricated using a modified “standard ice” protocol (Cole 1979) (images 1–5). Linden STFOC and HS STFOC tethers are embedded in ice (images 6 and 7), while images of ice away from tether (image 8) were used to characterize the grain size of the ice (uniform over the specimens tested).
Paper: Surviving in Ocean Worlds: Experimental Characterization of Fiber Optic Tethers across Europa-like Ice Faults and Unraveling the Sliding Behavior of Ice
Authors: Vishaal Singh, Christine McCarthy, Matthew Silvia, Michael V. Jakuba, Kathleen L. Craft, Alyssa R. Rhoden, Chris German, Theodore A. Koczynski
Figure caption: An illustration of a cryobot concept with communication tethers deployed in Europa’s potentially tectonic ice shell, highlighting the challenges of surviving across an extreme temperature−pressure gradient and varying lithospheric strength of the shell (Dombard & McKinnon 2006).
Paper: Surviving in Ocean Worlds: Experimental Characterization of Fiber Optic Tethers across Europa-like Ice Faults and Unraveling the Sliding Behavior of Ice
Authors: Vishaal Singh, Christine McCarthy, Matthew Silvia, Michael V. Jakuba, Kathleen L. Craft, Alyssa R. Rhoden, Chris German, Theodore A. Koczynski
Figure caption: Layers of a Linden Photonics Inc. (a) Strong Tether Fiber Optical Cable (STFOC) and (b) High Strength Strong Tether Fiber Optic Cable (HS STFOC). Images modified from Linden Photonics Inc. (2021) Cable Catalog.
Paper: Surviving in Ocean Worlds: Experimental Characterization of Fiber Optic Tethers across Europa-like Ice Faults and Unraveling the Sliding Behavior of Ice
Authors: Vishaal Singh, Christine McCarthy, Matthew Silvia, Michael V. Jakuba, Kathleen L. Craft, Alyssa R. Rhoden, Chris German, Theodore A. Koczynski
Figure caption: 3D model of ice fabrication mold components, custom built for freezing tethers in ice blocks under pretension.
Paper: Surviving in Ocean Worlds: Experimental Characterization of Fiber Optic Tethers across Europa-like Ice Faults and Unraveling the Sliding Behavior of Ice
Authors: Vishaal Singh, Christine McCarthy, Matthew Silvia, Michael V. Jakuba, Kathleen L. Craft, Alyssa R. Rhoden, Chris German, Theodore A. Koczynski
Figure caption: (a) Representative shear stress and velocity vs. time curve for the STFOC tether at 230 K, highlighting (b) peak stress achieved. Panels (c) and (d) show ice-quake events.
Paper: Surviving in Ocean Worlds: Experimental Characterization of Fiber Optic Tethers across Europa-like Ice Faults and Unraveling the Sliding Behavior of Ice
Authors: Vishaal Singh, Christine McCarthy, Matthew Silvia, Michael V. Jakuba, Kathleen L. Craft, Alyssa R. Rhoden, Chris German, Theodore A. Koczynski
Figure caption: Peak stress survived by STFOC and HS STFOC tethers in ice and control ice sample over the range of ice shell temperatures. An asterisk indicates that data were clipped at 1061 kPa owing to calibration limits of vertical load cell, thus representing an underreporting. Load cells were later recalibrated to fix this issue.