adsabs/AstroCLIMB huggingface dataset:
Paper: Jupiter's Banding and Jets May Be Caused by Tides
Authors: Robert H. Tyler
Figure caption: (a) Model of Jupiter’s time-averaged tidal dissipation rate as a function of latitude and nondimensional radius. The dissipation in panel (a) is depth integrated, and the global average is removed to give the three-peak curve in panel (b). This is then regarded as a source/sink of pressure/heating driving geostrophic jets (panel (c)) that show important features in common with the observed jets. Most important in the agreement demonstrated are: the equatorial prograde flow with a local minimum right at the equator, the concentrated activity within the critical latitudes, and the inflection points of band transitions. The most important disagreement seen is the observed asymmetric component of the observations, as this asymmetry is not expected for sectoral tidal forces and spherically symmetric interior parameters.
Paper: Jupiter's Banding and Jets May Be Caused by Tides
Authors: Robert H. Tyler
Figure caption: Nondimensional tidal power ﹩\tilde{{ \mathcal P }}﹩ as a function of the squared adjustment wave speed ﹩{\tilde{c}}_{e}^{2}﹩, and the dissipation timescale ﹩\tilde{T}﹩ (associated with pressure relaxation timescale ﹩{\alpha }_{p}^{-1}﹩). In the underdamped domain (﹩\tilde{T}\gt 1﹩), three cases (A, B, and C) are considered, corresponding with excitation of the first three symmetric eigen (Hough) functions, respectively. Overlain are horizontal green lines showing the locations of eigenvalues ﹩{\tilde{c}}_{e,(\mu )}^{2}﹩.
Paper: Jupiter's Banding and Jets May Be Caused by Tides
Authors: Robert H. Tyler
Figure caption: Background density ρ 0 (panel (a)), and pressure p 0 (panel (b)). The data in the outer shell (panels (c) and (d)) is used in this study.
Paper: Jupiter's Banding and Jets May Be Caused by Tides
Authors: Robert H. Tyler
Figure caption: The gravitational acceleration g (panel (a)) speed of sound ﹩{\tilde{c}}_{s}﹩ (panel (c)) and buoyancy frequency N (panel (e)) and their nondimensional forms (panels (b), (d), and (f)).
Paper: Jupiter's Banding and Jets May Be Caused by Tides
Authors: Robert H. Tyler
Figure caption: Eigenvalues (﹩{\tilde{c}}_{e,(\mu )}^{2}﹩) and eigenfunctions of the horizontal operator L  H . The amplitudes of the spherical-harmonic coefficients show important scattering across higher degrees as the amplitude of the eigenvalue ﹩{\tilde{c}}_{e,(\mu )}^{2}﹩ decreases.
Paper: Jupiter's Banding and Jets May Be Caused by Tides
Authors: Robert H. Tyler
Figure caption: Eigenvalues (plotted as the reciprocal ﹩{\tilde{\nu }}_{(\lambda )}^{-2}﹩) and eigenfunctions of the vertical operator L  V . The eigenfunctions show shorter wavelengths and more focus near the surface for increasing eigenmode.
Paper: Assessing the Distribution of Water Ice and Other Volatiles at the Lunar South Pole with LUVMI-X: A Mission Concept
Authors: Martin J. Losekamm, Janos Biswas, Thibaud Chupin, Michael Deiml, Matthieu Deremetz, Anthony M. Evagora, Guillaume Fau, Jessica Flahaut, Jeremi Gancet, Markus Glier, Christian Gscheidle, Marine Joulaud, Hemanth K. Madakashira, Neil J. Murray, Jörg Neumann, Thomas Pöschl, Lutz Richter, Hannah M. Sargeant, Susanne Schröder, Jae Schwanethal, Simon Sheridan, Diego Urbina, David S. Vogt, Peter Wessels
Figure caption: Drill prototype illuminated by the LVS-dedicated multispectral camera during testing.
Paper: Assessing the Distribution of Water Ice and Other Volatiles at the Lunar South Pole with LUVMI-X: A Mission Concept
Authors: Martin J. Losekamm, Janos Biswas, Thibaud Chupin, Michael Deiml, Matthieu Deremetz, Anthony M. Evagora, Guillaume Fau, Jessica Flahaut, Jeremi Gancet, Markus Glier, Christian Gscheidle, Marine Joulaud, Hemanth K. Madakashira, Neil J. Murray, Jörg Neumann, Thomas Pöschl, Lutz Richter, Hannah M. Sargeant, Susanne Schröder, Jae Schwanethal, Simon Sheridan, Diego Urbina, David S. Vogt, Peter Wessels
Figure caption: Plasma plumes generated by pulses of different energies on regolith simulant.
Paper: Assessing the Distribution of Water Ice and Other Volatiles at the Lunar South Pole with LUVMI-X: A Mission Concept
Authors: Martin J. Losekamm, Janos Biswas, Thibaud Chupin, Michael Deiml, Matthieu Deremetz, Anthony M. Evagora, Guillaume Fau, Jessica Flahaut, Jeremi Gancet, Markus Glier, Christian Gscheidle, Marine Joulaud, Hemanth K. Madakashira, Neil J. Murray, Jörg Neumann, Thomas Pöschl, Lutz Richter, Hannah M. Sargeant, Susanne Schröder, Jae Schwanethal, Simon Sheridan, Diego Urbina, David S. Vogt, Peter Wessels
Figure caption: The LUVMI-X rover and its instrumentation.
Paper: Assessing the Distribution of Water Ice and Other Volatiles at the Lunar South Pole with LUVMI-X: A Mission Concept
Authors: Martin J. Losekamm, Janos Biswas, Thibaud Chupin, Michael Deiml, Matthieu Deremetz, Anthony M. Evagora, Guillaume Fau, Jessica Flahaut, Jeremi Gancet, Markus Glier, Christian Gscheidle, Marine Joulaud, Hemanth K. Madakashira, Neil J. Murray, Jörg Neumann, Thomas Pöschl, Lutz Richter, Hannah M. Sargeant, Susanne Schröder, Jae Schwanethal, Simon Sheridan, Diego Urbina, David S. Vogt, Peter Wessels
Figure caption: Rover prototype during field testing.
Paper: Composition, Roughness, and Topography from Radar Backscatter at Selk Crater, the Dragonfly Landing Site
Authors: Léa E. Bonnefoy, Antoine Lucas, Alexander G. Hayes, Sébastien Rodriguez, Valerio Poggiali, Daniel E. Lalich, Ralph D. Lorenz, Alice Le Gall
Figure caption: The median radarclinometry-derived DTM obtained for different values of n or ﹩{\varepsilon }_{d}^{{\prime} }﹩ is averaged within each SARTopo footprint along the only SARTopo track that crosses the Selk crater rim (from north to south). The heights obtained from SARTopo and from the DTMs are plotted together on the left for the Acos n  model (top) and the Swift model (bottom), showing good agreement, especially for low values of n and ﹩{\varepsilon }_{d}^{{\prime} }﹩. On the right, we show the best median DTMs, corresponding to n = 1 (top) and ﹩{\varepsilon }_{d}^{{\prime} }=1﹩ (bottom). The sides of the rim parallel to the look direction are grayed out: because the radar is not oriented perpendicularly to most of the expected slopes there, the altitudes in these regions are less reliable. The SARTopo pass crossing the crater is outlined, and an example SARTopo footprint is drawn in red. Note that although the SARTopo footprints overlap, they are 8–10 km long.
Paper: Composition, Roughness, and Topography from Radar Backscatter at Selk Crater, the Dragonfly Landing Site
Authors: Léa E. Bonnefoy, Antoine Lucas, Alexander G. Hayes, Sébastien Rodriguez, Valerio Poggiali, Daniel E. Lalich, Ralph D. Lorenz, Alice Le Gall
Figure caption: Radarclinometry example over the Selk crater rim from T98, showing the NRCS σ 0 (left), the extracted slopes over the crater rim (middle), and the altitude (right). The slopes are calculated assuming only diffuse scattering from the Swift model, with ﹩{\varepsilon }_{d}^{{\prime} }=1﹩ in this case. Radar look angle is as indicated in the blue arrow.
Paper: Composition, Roughness, and Topography from Radar Backscatter at Selk Crater, the Dragonfly Landing Site
Authors: Léa E. Bonnefoy, Antoine Lucas, Alexander G. Hayes, Sébastien Rodriguez, Valerio Poggiali, Daniel E. Lalich, Ralph D. Lorenz, Alice Le Gall
Figure caption: Variations of the NRCS σ 0 with incidence angle θ within dune fields and plains, both inside and outside of Selk crater. As described in Section 2.3.1, the σ 0 is averaged within each grid cell. Note that the backscattering behavior of both the dune fields and the plains units is consistent inside and outside the crater, pointing to likely similar composition and structure. As in Figure 3, the high σ 0 values around 40° incidence correspond to T121S6 and are likely caused by a calibration anomaly.
Paper: Connections between the Transient Polar Warming and Solstitial Pause on Mars
Authors: Anthony D. Toigo, Darryn W. Waugh
Figure caption: Metrics (see Table 1) at the L  S  = 270° season as a function of obliquity and optical depth. Contouring is done by Delaunay triangulation from the sparsely sampled phase space, and the individual simulations are shown at their appropriate locations in this phase space with their individual metric value shown in red. (A) T pole, (B) ﹩{U}_{\max }﹩, (C) U lat, (D) PV pole, (E) W lat, (F) H R south, (G) ﹩T{{\prime} }_{\max }﹩, (H) ﹩{\sigma }_{\max }﹩, and (I) ﹩{({dU}/{dz})}_{\max }﹩. The light gray shading in all panels highlights regions greater than or less than a representative threshold metric value. Threshold shading is (A) >150 K, (B) >130 m s−1, (C) >65°N, (D) >375 × 10−6 K m2 kg−1 s −1, (E) >20 K sol−1, (F) >1 K sol−1, (G) <6 K, (H) <90 × 10−6 s−1, and (I) <11 × 10−3 s−1. The blue line in all panels is the contour where T pole = 150 K, our threshold for the occurrence of a TPW. Note that the illustrative ε15τ1.25 simulation is not plotted in this figure, as it is the only simulation with an optical depth greater than 1, and there are insufficient other simulations to accurately interpolate contours in that region.
Paper: Connections between the Transient Polar Warming and Solstitial Pause on Mars
Authors: Anthony D. Toigo, Darryn W. Waugh
Figure caption: Zonal-average atmospheric fields as a function of solar longitude and latitude on a constant 10 Pa pressure surface, for (left column) the ε15τ1.25 simulation and (right column) the ε55τ0.30 simulation. (A), (B) Zonal winds (m s−1, black contours and shading) and temperature (K, red contours). Zonal wind contours are every 50 m s−1 between −150 and 150 m s−1. Zonal winds >100 m s−1 are shaded gray, and >150 m s−1 are shaded dark gray. Temperature contours are every 20 K between 140 and180 K. (C), (D) Scaled potential vorticity (10−6 K m2 kg−1 s−1) , with contours every 100 units between 0 and 300, values >200 are shaded gray, and >300 are shaded dark gray. (E), (F) Mean meridional circulation (107 kg s−1) , with contours at values of −1 (dashed), 0 (dotted), and 1, 10, and 30 (solid); values > 1 are shaded gray and >30 are shaded dark gray. (G), (H) Vertical wind, with contours at 0, −10, −50, and −100 mm s−1, values < −20 mm s−1 are shaded gray, and <−50 mm s−1 are shaded dark gray. The solid blue line shows the mean meridional circulation at a contoured value of 1 × 107 kg s−1, as also seen in panels (E) and (F). All fields have been filtered in time with a 30 sol sliding boxcar average.
Paper: Connections between the Transient Polar Warming and Solstitial Pause on Mars
Authors: Anthony D. Toigo, Darryn W. Waugh
Figure caption: Zonal-average fields as a function of latitude and pressure averaged for 30 sols centered on L  S  = 270°, for (left column) the ε15τ1.25 and (right column) the ε55τ0.30 simulations. (A), (B) Zonal winds (m s−1, black contours and shading) and temperature (K, red contours). Zonal wind contours are every 50 m s−1, from −150 m s−1 to 150 m s−1, with two additional contours at −20 and 20 m s−1. Zonal winds >100 m s−1, or <−100 m s−1, are shaded gray, and >150 m s−1, or <−150 m s−1, are shaded dark gray. Temperature contours are every 20 K from 140 to 260 K. (C), (D) Zonal-average mean meridional circulation (106 kg s−1). Mean meridional circulation is contoured logarithmically; contours are shown for −100, −10, −1, 1, 10, 100, and 1000 kg s−1. (E), (F) Zonal-average aerosol heating/cooling rate (K sol−1). Heating rates are contoured at values of 0, 1, 3, 10, and 20 K sol−1, with values >3 K sol−1 shaded gray and >20 K sol−1 shaded dark gray. Blue bars mark the location (50–70°S and 30 Pa) of the heating rate metric that is used in Figures 4 and 5.
Paper: Connections between the Transient Polar Warming and Solstitial Pause on Mars
Authors: Anthony D. Toigo, Darryn W. Waugh
Figure caption: Zonal-average atmospheric fields as a function of season (solar longitude) and latitude on different surfaces, with a 30 sol sliding boxcar average in time, from (left column) the ε15τ1.25 simulation and (right column) the ε55τ0.30 simulation. (A), (B) rms(﹩T^{\prime} ﹩) (K, black contours and shading) and zonal wind (m s−1, red contours) at a constant height of 2.5 km above the surface. rms(﹩T^{\prime} ﹩) contours are every 2.5 K, from 0 to 12.5 K, with values >5 K is shaded gray and >10 K shaded dark gray. (C), (D) Eady growth rate (10−6 s−1, black contours) and zonal wind (m s−1, red contours) at a constant height of 0.2 km above the surface. Growth rate is contoured at 0, 10, 20, and 50 × 10−6 s−1, and values >20 × 10−6 s−1 are shaded gray and >50 × 10−6 s−1 are shaded dark gray. Zonal wind is contoured every 10 m s−1 from −10 to 10 m s−1.
Paper: Connections between the Transient Polar Warming and Solstitial Pause on Mars
Authors: Anthony D. Toigo, Darryn W. Waugh
Figure caption: Key indicating the obliquities and peak seasonal optical depths used in the simulations shown in the rest of the supplemental figures in this appendix. The values are shown in the notation described in Section 2.1. The simulations are displayed with increasing obliquity along rows and increasing optical depth along columns. A blank location indicates that the simulation at the particular combination of obliquity and optical depth was not performed.
Paper: Connections between the Transient Polar Warming and Solstitial Pause on Mars
Authors: Anthony D. Toigo, Darryn W. Waugh
Figure caption: TPW and SP metrics as a function of H R south, the aerosol heating rate at 30 Pa and 60°S. Simulations with the same obliquity are indicated by using the same plotting symbol and color: purple diamonds are for ε = 5°, red triangles are for ε = 15°, black circles are for ε = 25°, green crosses are for ε = 35°, cyan pluses are for ε = 45°, and blue squares are for ε = 55°. Dashed vertical lines are shown at H R south = 20 K sol−1. Panel (F) has been deliberately omitted.
Paper: Assessing the Distribution of Water Ice and Other Volatiles at the Lunar South Pole with LUVMI-X: A Mission Concept
Authors: Martin J. Losekamm, Janos Biswas, Thibaud Chupin, Michael Deiml, Matthieu Deremetz, Anthony M. Evagora, Guillaume Fau, Jessica Flahaut, Jeremi Gancet, Markus Glier, Christian Gscheidle, Marine Joulaud, Hemanth K. Madakashira, Neil J. Murray, Jörg Neumann, Thomas Pöschl, Lutz Richter, Hannah M. Sargeant, Susanne Schröder, Jae Schwanethal, Simon Sheridan, Diego Urbina, David S. Vogt, Peter Wessels
Figure caption: Functional testing of the LCNS charged-particle telescope with a proton beam.
Paper: Assessing the Distribution of Water Ice and Other Volatiles at the Lunar South Pole with LUVMI-X: A Mission Concept
Authors: Martin J. Losekamm, Janos Biswas, Thibaud Chupin, Michael Deiml, Matthieu Deremetz, Anthony M. Evagora, Guillaume Fau, Jessica Flahaut, Jeremi Gancet, Markus Glier, Christian Gscheidle, Marine Joulaud, Hemanth K. Madakashira, Neil J. Murray, Jörg Neumann, Thomas Pöschl, Lutz Richter, Hannah M. Sargeant, Susanne Schröder, Jae Schwanethal, Simon Sheridan, Diego Urbina, David S. Vogt, Peter Wessels
Figure caption: Visual guide (not to scale) to the mission’s concept of operations: contamination analysis of the landing site (a), sampling with the LVS and VOILA (b), scouting for increased hydrogen abundance during traverse (c), investigation of PSR and deployment of a VCAS unit (d), sampling of an area in temporary shadow with VOILA and LVS (e), and drive into PSR (f).
Paper: Assessing the Distribution of Water Ice and Other Volatiles at the Lunar South Pole with LUVMI-X: A Mission Concept
Authors: Martin J. Losekamm, Janos Biswas, Thibaud Chupin, Michael Deiml, Matthieu Deremetz, Anthony M. Evagora, Guillaume Fau, Jessica Flahaut, Jeremi Gancet, Markus Glier, Christian Gscheidle, Marine Joulaud, Hemanth K. Madakashira, Neil J. Murray, Jörg Neumann, Thomas Pöschl, Lutz Richter, Hannah M. Sargeant, Susanne Schröder, Jae Schwanethal, Simon Sheridan, Diego Urbina, David S. Vogt, Peter Wessels
Figure caption: Regions of interest for the LUVMI-X mission, compared to those previously identified by Lemelin et al. (2014) and Flahaut et al. (2020).
Paper: Assessing the Distribution of Water Ice and Other Volatiles at the Lunar South Pole with LUVMI-X: A Mission Concept
Authors: Martin J. Losekamm, Janos Biswas, Thibaud Chupin, Michael Deiml, Matthieu Deremetz, Anthony M. Evagora, Guillaume Fau, Jessica Flahaut, Jeremi Gancet, Markus Glier, Christian Gscheidle, Marine Joulaud, Hemanth K. Madakashira, Neil J. Murray, Jörg Neumann, Thomas Pöschl, Lutz Richter, Hannah M. Sargeant, Susanne Schröder, Jae Schwanethal, Simon Sheridan, Diego Urbina, David S. Vogt, Peter Wessels
Figure caption: LUVMI-X instruments and scientific areas under investigation.
Paper: Assessing the Distribution of Water Ice and Other Volatiles at the Lunar South Pole with LUVMI-X: A Mission Concept
Authors: Martin J. Losekamm, Janos Biswas, Thibaud Chupin, Michael Deiml, Matthieu Deremetz, Anthony M. Evagora, Guillaume Fau, Jessica Flahaut, Jeremi Gancet, Markus Glier, Christian Gscheidle, Marine Joulaud, Hemanth K. Madakashira, Neil J. Murray, Jörg Neumann, Thomas Pöschl, Lutz Richter, Hannah M. Sargeant, Susanne Schröder, Jae Schwanethal, Simon Sheridan, Diego Urbina, David S. Vogt, Peter Wessels
Figure caption: A possible traverse path (red line) on the Shoemaker–Faustini ridge fulfilling all requirements for the mission. Alternate paths for landings outside of the 100 m landing ellipse are shown as dashed green lines.
Paper: Mapping Lunar Swirls with Machine Learning: The Application of Unsupervised and Supervised Image Classification Algorithms in Reiner Gamma and Mare Ingenii
Authors: Frank C. Chuang, Matthew D. Richardson, John R. Weirich, Amanda A. Sickafoose, Deborah L. Domingue
Figure caption: (A) Central portion of the Reiner Gamma swirls, with the study region highlighted in pink. The center of the entire swirl region is located at ∼7.4° N, 301° E on the lunar nearside. (B) Portion of the swirls in Mare Ingenii, with the study region highlighted in pink. The center of the entire swirl region is located at ∼33.24° S, 164.83° E on the lunar farside. The background image in both panels is the 100 m pixel−1 LROC WAC mosaic. North is up and west is to the left.
Paper: Composition, Roughness, and Topography from Radar Backscatter at Selk Crater, the Dragonfly Landing Site
Authors: Léa E. Bonnefoy, Antoine Lucas, Alexander G. Hayes, Sébastien Rodriguez, Valerio Poggiali, Daniel E. Lalich, Ralph D. Lorenz, Alice Le Gall
Figure caption:                         Variations of the NRCS σ                         0 with incidence angle θ within each terrain unit mapped within the ROI. As described in Section 2.3.1, the σ                         0 is averaged within each grid cell, and the error bars are the standard deviation divided by ﹩\sqrt{N}﹩, where N is the number of independent resolution cells within the terrain unit within the grid cell. Each color corresponds to a different SAR swath, as described in the legends. Note that the crater rim backscatter curve presented in this figure is not corrected for local slopes, although it is in Figure 5. The dune and interdune region curves correspond to part of the area of the dune fields unit, with dunes and interdune regions separated only in the swaths in which they are resolved.
Paper: Composition, Roughness, and Topography from Radar Backscatter at Selk Crater, the Dragonfly Landing Site
Authors: Léa E. Bonnefoy, Antoine Lucas, Alexander G. Hayes, Sébastien Rodriguez, Valerio Poggiali, Daniel E. Lalich, Ralph D. Lorenz, Alice Le Gall
Figure caption: Values of the dielectric constant, rms slope, and scattering albedo derived for all eight terrains and for all six combinations of quasi-specular and diffuse scattering models. The values shown in this plot are given in Table 2.
Paper: Composition, Roughness, and Topography from Radar Backscatter at Selk Crater, the Dragonfly Landing Site
Authors: Léa E. Bonnefoy, Antoine Lucas, Alexander G. Hayes, Sébastien Rodriguez, Valerio Poggiali, Daniel E. Lalich, Ralph D. Lorenz, Alice Le Gall
Figure caption: The nine SAR swaths within the ROI. The incidence angle θ is given, and the look direction is shown with a magenta arrow. The NRCS σ 0 is linearly scaled from 0 to 1.5 for all nine swaths. Note that the aspect of the Selk crater ejecta changes with incidence angle, appearing brighter and more widespread in T95 than in T98, for example. The position of the ROI on Titan is shown in the context map at the top, over the VIMS/ISS background from Seignovert et al. (2019), overlaid with a global radar mosaic.
Paper: Composition, Roughness, and Topography from Radar Backscatter at Selk Crater, the Dragonfly Landing Site
Authors: Léa E. Bonnefoy, Antoine Lucas, Alexander G. Hayes, Sébastien Rodriguez, Valerio Poggiali, Daniel E. Lalich, Ralph D. Lorenz, Alice Le Gall
Figure caption: Sensitivity of the fit to each of four parameters, for each combination of quasi-specular + diffuse model. For this figure, the Swift diffuse scattering model assumes perpendicular polarization angle. For parallel polarization the contribution of ﹩{\varepsilon }_{d}^{{\prime} }﹩ is negligible at all incidence angles (because the transmissivity near the Brewster angles is almost the same for all dielectric constants considered).
Paper: Composition, Roughness, and Topography from Radar Backscatter at Selk Crater, the Dragonfly Landing Site
Authors: Léa E. Bonnefoy, Antoine Lucas, Alexander G. Hayes, Sébastien Rodriguez, Valerio Poggiali, Daniel E. Lalich, Ralph D. Lorenz, Alice Le Gall
Figure caption: Left: mosaic of the incidence-angle-corrected SAR swaths within the ROI. Right: geomorphological map of the ROI. The criteria to differentiate between the six units are detailed in Section 2.2. For easy comparison with previous work, we use a color scheme similar to that of Malaska et al. (2016b).
Paper: Transmission of a Seismic Wave Generated by Impacts on Granular Asteroids
Authors: Paul Sánchez, Daniel J. Scheeres, Alice C. Quillen
Figure caption: Wave speed vs. confining pressure in the simulated systems. The different colors represent the different compression speeds of the piston. The horizontal axis above has been scaled by Young’s modulus of the material, whereas the vertical axis at the right has been scaled by the wave velocity in basalt, v  B  = 5 × 103 m s−1.
Paper: Transmission of a Seismic Wave Generated by Impacts on Granular Asteroids
Authors: Paul Sánchez, Daniel J. Scheeres, Alice C. Quillen
Figure caption: Seismic wave speed vs. stable pressure for all of the constant velocity compression simulations The three trend lines have been added to show how different pressure exponents adjust the data points. The data points represented by the purple triangles labeled as “anomalies” were not taken into account. The horizontal axis above has been scaled by Young’s modulus of the material, whereas the vertical axis at the right has been scaled by the wave velocity in basalt, v  B  = 5 × 103 m s−1.
Paper: Transmission of a Seismic Wave Generated by Impacts on Granular Asteroids
Authors: Paul Sánchez, Daniel J. Scheeres, Alice C. Quillen
Figure caption: (a) Kinetic energy of the particles vs. height and over time, (b) P  yy  component of the stress tensor vs. height and over time, and (c) position of the peak of both kinetic energy and P  yy  vs. time.
Paper: Transmission of a Seismic Wave Generated by Impacts on Granular Asteroids
Authors: Paul Sánchez, Daniel J. Scheeres, Alice C. Quillen
Figure caption: Compression speed vs. the pressure induced by the compression. The different symbols correspond to the confining pressure of the system in which the measurement was carried out. The blue line is a fit of the data with the equation ﹩{P}_{i}=4.36\times {10}^{5}{v}_{c}^{1.18}﹩.
Paper: Transmission of a Seismic Wave Generated by Impacts on Granular Asteroids
Authors: Paul Sánchez, Daniel J. Scheeres, Alice C. Quillen
Figure caption: Time evolution of the vertical velocity profile of the particles inside the container at 0.1 Pa. The piston speed is set at 0.1 m s−1.
Paper: Transmission of a Seismic Wave Generated by Impacts on Granular Asteroids
Authors: Paul Sánchez, Daniel J. Scheeres, Alice C. Quillen
Figure caption: Time evolution of the P  yy  component of the stress tensor of the particles in each slide inside the container at 0.1 Pa. The piston speed is set at 0.1 m s−1.