adsabs/AstroCLIMB huggingface dataset:
Paper: Depletion of 13C in CO in the Atmosphere of Mars Suggested by ExoMars-TGO/NOMAD Observations
Authors: S. Aoki, K. Shiobara, N. Yoshida, L. Trompet, T. Yoshida, N. Terada, H. Nakagawa, G. Liuzzi, A. C. Vandaele, I. R. Thomas, G. L. Villanueva, M. A. Lopez-Valverde, A. Brines, M. R. Patel, S. Faggi, F. Daerden, J. T. Erwin, B. Ristic, G. Bellucci, J. J. Lopez-Moreno, H. Kurokawa, Y. Ueno
Figure caption:                         Vertical profile of the temperature profiles (a), volume mixing ratio of 12C16O (red with circular symbols), 13C16O (blue with square symbols), 12C18O (green with triangle symbols) (b), and δ values calculated with 13C16O/12C16O ratios (blue with square symbols) and 13C16O/12C18O ratios (green with triangle symbols) (c). These profiles are retrieved from the orbit taken on 2022 March 11 (the fifth orbit shown in Table 1). The results from the other orbits are shown in Figure B1. In the panel (a), the red-solid curve, black-dotted curve, and the blue-dashed curves represent temperature profiles retrieved from order 132, predicted by GEM-Mars model, and combined with retrieval and GEM-Mars model, respectively. The x-axis of the panel (b) is the total CO volume mixing ratio retrieved from 12C16O, 13C16O, or 12C18O lines by assuming the terrestrial isotopic ratio. In other words, the retrieved volume mixing ratios of 12C16O, 13C16O, or 12C18O are multiplied by the terrestrial isotopic ratios (9.86544 × 10−1, 1.10836 × 10−2, and 1.97822 × 10−3, respectively). The red, blue, and green curves would be overlapped if δ value is 0‰.
Paper: Depletion of 13C in CO in the Atmosphere of Mars Suggested by ExoMars-TGO/NOMAD Observations
Authors: S. Aoki, K. Shiobara, N. Yoshida, L. Trompet, T. Yoshida, N. Terada, H. Nakagawa, G. Liuzzi, A. C. Vandaele, I. R. Thomas, G. L. Villanueva, M. A. Lopez-Valverde, A. Brines, M. R. Patel, S. Faggi, F. Daerden, J. T. Erwin, B. Ristic, G. Bellucci, J. J. Lopez-Moreno, H. Kurokawa, Y. Ueno
Figure caption: The contribution of the main and adjacent orders appeared in the NOMAD spectra for order 183 (a), order 184 (b), order 185 (c), and order 186 (d). The synthetic spectra are calculated for the measurements around 30 km tangent height. The differences in color and line type represent the contribution of the different diffraction order (the main order contribution is shown as the bold lines in red, and the adjacent orders are shown in the other colors).
Paper: Depletion of 13C in CO in the Atmosphere of Mars Suggested by ExoMars-TGO/NOMAD Observations
Authors: S. Aoki, K. Shiobara, N. Yoshida, L. Trompet, T. Yoshida, N. Terada, H. Nakagawa, G. Liuzzi, A. C. Vandaele, I. R. Thomas, G. L. Villanueva, M. A. Lopez-Valverde, A. Brines, M. R. Patel, S. Faggi, F. Daerden, J. T. Erwin, B. Ristic, G. Bellucci, J. J. Lopez-Moreno, H. Kurokawa, Y. Ueno
Figure caption: Lower-state energy of the transition (the E″ parameters) of 12C16O (red with circular symbols), 13C16O (blue with triangle symbols), and 12C18O (green with square symbols) lines in diffraction order 183 (a), order 184 (b), order 185 (c), and 186 (d) obtained from HITRAN2020 database.
Paper: Depletion of 13C in CO in the Atmosphere of Mars Suggested by ExoMars-TGO/NOMAD Observations
Authors: S. Aoki, K. Shiobara, N. Yoshida, L. Trompet, T. Yoshida, N. Terada, H. Nakagawa, G. Liuzzi, A. C. Vandaele, I. R. Thomas, G. L. Villanueva, M. A. Lopez-Valverde, A. Brines, M. R. Patel, S. Faggi, F. Daerden, J. T. Erwin, B. Ristic, G. Bellucci, J. J. Lopez-Moreno, H. Kurokawa, Y. Ueno
Figure caption: Vertical profiles (a) and histogram (b) of δ value in CO obtained with 18C16O and 13C16O volume mixing ratio retrieved with original temperature profiles and AOTF transfer function shifted by its uncertainty in the positive direction.
Paper: Depletion of 13C in CO in the Atmosphere of Mars Suggested by ExoMars-TGO/NOMAD Observations
Authors: S. Aoki, K. Shiobara, N. Yoshida, L. Trompet, T. Yoshida, N. Terada, H. Nakagawa, G. Liuzzi, A. C. Vandaele, I. R. Thomas, G. L. Villanueva, M. A. Lopez-Valverde, A. Brines, M. R. Patel, S. Faggi, F. Daerden, J. T. Erwin, B. Ristic, G. Bellucci, J. J. Lopez-Moreno, H. Kurokawa, Y. Ueno
Figure caption: Vertical profiles (a) and histogram (b) of δ value in CO obtained with 18C16O and 13C16O volume mixing ratio retrieved with original temperature profiles and AOTF transfer function shifted by its uncertainty in the negative direction.
Paper: Depletion of 13C in CO in the Atmosphere of Mars Suggested by ExoMars-TGO/NOMAD Observations
Authors: S. Aoki, K. Shiobara, N. Yoshida, L. Trompet, T. Yoshida, N. Terada, H. Nakagawa, G. Liuzzi, A. C. Vandaele, I. R. Thomas, G. L. Villanueva, M. A. Lopez-Valverde, A. Brines, M. R. Patel, S. Faggi, F. Daerden, J. T. Erwin, B. Ristic, G. Bellucci, J. J. Lopez-Moreno, H. Kurokawa, Y. Ueno
Figure caption: Vertical profiles (a) and histogram (b) of δ values in CO obtained with 12C18O and 13C16O volume mixing ratio retrieved with original AOTF transfer function and temperature profiles shifted by −5 K.
Paper: Depletion of 13C in CO in the Atmosphere of Mars Suggested by ExoMars-TGO/NOMAD Observations
Authors: S. Aoki, K. Shiobara, N. Yoshida, L. Trompet, T. Yoshida, N. Terada, H. Nakagawa, G. Liuzzi, A. C. Vandaele, I. R. Thomas, G. L. Villanueva, M. A. Lopez-Valverde, A. Brines, M. R. Patel, S. Faggi, F. Daerden, J. T. Erwin, B. Ristic, G. Bellucci, J. J. Lopez-Moreno, H. Kurokawa, Y. Ueno
Figure caption: Vertical profiles (a) and histogram (b) of δ values in CO obtained with 12C18O and 13C16O volume mixing ratio retrieved with original AOTF transfer function and temperature profiles shifted by +5 K.
Paper: Depletion of 13C in CO in the Atmosphere of Mars Suggested by ExoMars-TGO/NOMAD Observations
Authors: S. Aoki, K. Shiobara, N. Yoshida, L. Trompet, T. Yoshida, N. Terada, H. Nakagawa, G. Liuzzi, A. C. Vandaele, I. R. Thomas, G. L. Villanueva, M. A. Lopez-Valverde, A. Brines, M. R. Patel, S. Faggi, F. Daerden, J. T. Erwin, B. Ristic, G. Bellucci, J. J. Lopez-Moreno, H. Kurokawa, Y. Ueno
Figure caption: Vertical profiles (a) and histogram (b) of δ values in CO obtained with 12C18O and 13C16O volume mixing ratio retrieved with original AOTF transfer function and temperature profiles.
Paper: Depletion of 13C in CO in the Atmosphere of Mars Suggested by ExoMars-TGO/NOMAD Observations
Authors: S. Aoki, K. Shiobara, N. Yoshida, L. Trompet, T. Yoshida, N. Terada, H. Nakagawa, G. Liuzzi, A. C. Vandaele, I. R. Thomas, G. L. Villanueva, M. A. Lopez-Valverde, A. Brines, M. R. Patel, S. Faggi, F. Daerden, J. T. Erwin, B. Ristic, G. Bellucci, J. J. Lopez-Moreno, H. Kurokawa, Y. Ueno
Figure caption: Vertical profiles (a) and histogram (b) of δ 13C values in CO obtained with 12C16O and 13C16O volume mixing ratio retrieved with original AOTF transfer function and temperature profiles shifted by −5 K.
Paper: Depletion of 13C in CO in the Atmosphere of Mars Suggested by ExoMars-TGO/NOMAD Observations
Authors: S. Aoki, K. Shiobara, N. Yoshida, L. Trompet, T. Yoshida, N. Terada, H. Nakagawa, G. Liuzzi, A. C. Vandaele, I. R. Thomas, G. L. Villanueva, M. A. Lopez-Valverde, A. Brines, M. R. Patel, S. Faggi, F. Daerden, J. T. Erwin, B. Ristic, G. Bellucci, J. J. Lopez-Moreno, H. Kurokawa, Y. Ueno
Figure caption: Vertical profiles (a) and histogram (b) of δ 13C values in CO obtained with 12C16O and 13C16O volume mixing ratio retrieved with original AOTF transfer function and temperature profiles shifted by +5 K.
Paper: Relation of Gravity, Winds, and the Moment of Inertia of Jupiter and Saturn
Authors: Burkhard Militzer, William B. Hubbard
Figure caption: Predictions from two- and three-layer models for Jupiter’s interior that were constructed under different assumptions and match J 2 exactly. Colors label models consistently across all panels, but not all curves are shown in every panel for clarity. The numbers specify the assumed transition pressure in GPa between molecular and metallic layers so that models can be traced across different panels. Panel (b) compares the abundance of heavy elements in the outer molecular layer, Z 1, with the value of the protosolar nebula, 1.53% (Lodders 2010). No winds were included except for the last models shown in light-blue. Only the brown curves refer to models with a compact core (6 Earth masses, rocky composition). The light-green star shows the preferred model from Hubbard & Militzer (2016), while the pentagons and triangles indicate other compact core models based on the EOSs by Militzer & Hubbard (2013) and Saumon et al. (1995).
Paper: Relation of Gravity, Winds, and the Moment of Inertia of Jupiter and Saturn
Authors: Burkhard Militzer, William B. Hubbard
Figure caption: Panels (a), (b), and (c) show the MoI of hypothetical planets with prescribed q rot and J 2 values. The solid lines show the ensemble average of abstract models with 50 constant-density spheroids. The predictions from physical giant interior models that match the spacecraft measurements of Jupiter and Saturn are shown for comparison. The dashed lines in panel (b) are the prediction from the Radau–Darwin Equation (16) that becomes exact in the limit of small q rot and large J 2. In this limit, the 50-spheroid models are forced to approach the uniform-density limit of MoI = ﹩\tfrac{2}{5}﹩. One can also approach this limit with two-spheroid calculations. Hence, in panel (d) we show how the volume fraction of the inner spheroid changes as a function of q rot. As the fraction approaches unity, the choices for q rot and J 2 imply a constant planet.
Paper: Relation of Gravity, Winds, and the Moment of Inertia of Jupiter and Saturn
Authors: Burkhard Militzer, William B. Hubbard
Figure caption: Probability density distributions of Jupiter’s and Saturn’s MoI values. The top panel illustrates how the range of likely MoI values shrinks as models with eight constant-density spheroids are required first to match only Jupiter’s J 2 value, then to match J 2 and J 4, and then to reproduce the measured values for J 2 through J 6. The second panel shows that the range of likely MoI values shrinks further when this calculation is instead performed with 50 constant-density spheroids (see Figure 3). The third panel shows the same trend in four-spheroid models of Saturn. The bottom panel shows predictions from models that match Saturn’s J 2 through J 6. As the number of spheroids is increased, models tend to cluster in a narrower MoI interval. With 50-spheroid models that match J 2 through J 6, we obtained a range of 0.26393–0.26398 for Jupiter’s MoI. (Between 5 × 105 and 6 × 107 models were constructed to compute every individual MoI histogram.)
Paper: Relation of Gravity, Winds, and the Moment of Inertia of Jupiter and Saturn
Authors: Burkhard Militzer, William B. Hubbard
Figure caption: Probability density distributions of normalized moments of inertia derived from different ensembles of interior models matching even and odd gravity harmonics up to J 10. All models include a dilute core and contributions from winds. The red circles represent our reference models with five layers. When four-layer models are constructed by removing either the helium rain layer or the core transition layer, the MoI distribution hardly changes. If the 1 bar temperature is increased from 166.1 to 170 K, the MoI increases by only ∼10−5. Slightly larger changes are seen when the density of the hydrogen−helium mixture is reduced over pressure intervals from 10 to 100 or from 50 to 500 GPa. In the caption, we specify the size of the ensemble that was used for each histogram.
Paper: Relation of Gravity, Winds, and the Moment of Inertia of Jupiter and Saturn
Authors: Burkhard Militzer, William B. Hubbard
Figure caption: The top two panels show posterior distributions of gravity harmonics J 2 and J 4 derived from an ensemble of five-layer models. The bottom panels illustrate how the computed MoI correlates with J 2, J 4, and J 6. The dashed lines indicate the Juno gravity measurements from Durante et al. (2020) in Table 1.
Paper: Relation of Gravity, Winds, and the Moment of Inertia of Jupiter and Saturn
Authors: Burkhard Militzer, William B. Hubbard
Figure caption: Comparison of the density profiles of abstract models with that of our physical reference model with five layers. The shaded regions represent the standard deviations in density among the abstract models for a given radius.
Paper: Stereophotoclinometry for OSIRIS-REx Spacecraft Navigation
Authors: Coralie D. Adam, Leilah K. McCarthy, Jason M. Leonard, Robert Gaskell, Peter G. Antreasian, Andrew J. Liounis, Kenneth Getzandanner, Michael C. Moreau, Eric E. Palmer, John Weirich, Olivier S. Barnouin, Jeroen L. Geeraert, Eric M. Sahr, Benjamin Ashman, Derek S. Nelson, John Y. Pelgrift, Erik J. Lessac-Chenen, Daniel Wibben, Bobby G. Williams, Michael G. Daly, Dante S. Lauretta
Figure caption: OSIRIS-REx Proximity Operations Mission Timeline. Adapted from Antreasian et al. (2022).
Paper: Effects of the Librationally Induced Flow in Mercury’s Fluid Core with an Outer Stably Stratified Layer
Authors: Fleur Seuren, Santiago A. Triana, Jérémy Rekier, Ankit Barik, Tim Van Hoolst
Figure caption: Axial viscous ∣Γ ν , z∣ (blue) and electromagnetic torque ∣Γ η , z∣ (orange) as a function of the Ekman number, Ek, applied on the mantle by core motions resulting from the m = 0 component of libration. Dimensionless values can be read from the left axis and dimensional values from the right axis. The lighter lines correspond to the case with no background stratification N(r) = 0 for 0.4 = r ICB ≤ r ≤ r CMB, and the darker lines correspond to the stratified case (Equation (20)) with N 0 = 100, h = 0.1, r C = 0.4, and r ICB = 0.7. Extrapolation to the torques expected in Mercury’s core, represented by the filled circles, is performed along the dotted lines.
Paper: Effects of the Librationally Induced Flow in Mercury’s Fluid Core with an Outer Stably Stratified Layer
Authors: Fleur Seuren, Santiago A. Triana, Jérémy Rekier, Ankit Barik, Tim Van Hoolst
Figure caption: Kinetic energy density of the flow, Ek = 10−8, in response to the (m = 0, ω = 0.67) libration forcing in a nonstratified core with r ICB = 0.4 and N 0 = 0 (left column) and a stratified core with r ICB = 0.4, r C = 0.7, h = 0.1, and N 0 = 100 (right column). The top row displays meridional cuts (ϕ = 0) of the kinetic energy density, while the bottom row shows the total kinetic energy density as a function of the radial coordinate.
Paper: Effects of the Librationally Induced Flow in Mercury’s Fluid Core with an Outer Stably Stratified Layer
Authors: Fleur Seuren, Santiago A. Triana, Jérémy Rekier, Ankit Barik, Tim Van Hoolst
Figure caption: Total kinetic energy density of the librationally induced core flow as a function of the forcing frequency ω near Mercury’s observed libration frequency, ω = 0.67, indicated in each plot by the black vertical line. The top row gives the core response to the three types of libration forcing, m = 0 and ±2, in a neutrally stratified core (N 0 = 0 and r ICB = 0.4), and the bottom row shows the response in a core with an outer stably stratified layer (N 0 = 100, r ICB = 0.4, r C = 0.7, and h = 0.1). Different colored lines correspond to different Ekman numbers: Ek = 10−7 (blue), 10−8 (orange), and 10−9 (gray).
Paper: Effects of the Librationally Induced Flow in Mercury’s Fluid Core with an Outer Stably Stratified Layer
Authors: Fleur Seuren, Santiago A. Triana, Jérémy Rekier, Ankit Barik, Tim Van Hoolst
Figure caption: Eigenvalue spectra of the unforced problem (ϵ = 0) without (N 0 = 0; upper panels) and with (N 0 = 100; lower panels) stratification. Panels (b) and (d) display the damping, ﹩\mathrm{Im}[\omega ]﹩, versus the frequency, ﹩\mathrm{Re}[\omega ]﹩, of the least-damped eigensolutions near the forcing frequency (ω = 0.67) of Mercury’s longitudinal libration, denoted by the vertical black line. The eigensolution with the frequency closest to this libration frequency is marked in both panels with a black square, and meridional cuts of their corresponding kinetic energy density are shown in panels (a) and (c).
Paper: Effects of the Librationally Induced Flow in Mercury’s Fluid Core with an Outer Stably Stratified Layer
Authors: Fleur Seuren, Santiago A. Triana, Jérémy Rekier, Ankit Barik, Tim Van Hoolst
Figure caption: Electromagnetic torque at the outer boundary as a function of the thin-wall parameters c and ﹩c^{\prime} ﹩. Triangles mark cases where c is fixed to 10−4 and only ﹩{c}^{{\prime} }﹩ is varied, while circles mark cases where c is equal to ﹩{c}^{{\prime} }﹩ and varied. The results presented here are computed for Ek = 10−6, although they are identical to computations with a different Ekman number.
Paper: Effects of the Librationally Induced Flow in Mercury’s Fluid Core with an Outer Stably Stratified Layer
Authors: Fleur Seuren, Santiago A. Triana, Jérémy Rekier, Ankit Barik, Tim Van Hoolst
Figure caption: Kinetic energy density inside the core for the m = 0 libration forcing as a function of (a) the forcing frequency ω for different profiles of the Brunt–Väisälä frequency at the CMB and (b) the Brunt–Väisälä frequency N 0 at the peak forcing frequency ω = 0.6576 (denoted by the dashed–dotted vertical line). The solid vertical line coincides with the observed libration frequency ω = 0.67 in Mercury, and the remaining model parameters are E = 10−8, r C = 0.7, h = 0.1, and r ICB = 0.4.
Paper: Stereophotoclinometry for OSIRIS-REx Spacecraft Navigation
Authors: Coralie D. Adam, Leilah K. McCarthy, Jason M. Leonard, Robert Gaskell, Peter G. Antreasian, Andrew J. Liounis, Kenneth Getzandanner, Michael C. Moreau, Eric E. Palmer, John Weirich, Olivier S. Barnouin, Jeroen L. Geeraert, Eric M. Sahr, Benjamin Ashman, Derek S. Nelson, John Y. Pelgrift, Erik J. Lessac-Chenen, Daniel Wibben, Bobby G. Williams, Michael G. Daly, Dante S. Lauretta
Figure caption: Differences in the predicted landmark locations vs. the size of the time correction when adjusting the spacecraft pose for the rolling shutter for nine images. The mean landmark residuals in the sample and line directions are −0.30 px and −0.10 px, with standard deviations of 0.11 px and 0.25 px, respectively.
Paper: Stereophotoclinometry for OSIRIS-REx Spacecraft Navigation
Authors: Coralie D. Adam, Leilah K. McCarthy, Jason M. Leonard, Robert Gaskell, Peter G. Antreasian, Andrew J. Liounis, Kenneth Getzandanner, Michael C. Moreau, Eric E. Palmer, John Weirich, Olivier S. Barnouin, Jeroen L. Geeraert, Eric M. Sahr, Benjamin Ashman, Derek S. Nelson, John Y. Pelgrift, Erik J. Lessac-Chenen, Daniel Wibben, Bobby G. Williams, Michael G. Daly, Dante S. Lauretta
Figure caption: Landmark residuals in the (a) pixel, and (b) line components plotted over distance from center of image (Leonard et al. 2020a).
Paper: Earth as a Transiting Exoplanet: A Validation of Transmission Spectroscopy and Atmospheric Retrieval Methodologies for Terrestrial Exoplanets
Authors: Jacob Lustig-Yaeger, Victoria S. Meadows, David Crisp, Michael R. Line, Tyler D. Robinson
Figure caption: One-dimensional marginalized posterior distributions for NIRSpec G395M (blue), NIRSpec PRISM (purple), and MIRI LRS (orange) retrievals. These constraints correspond to 80 stacked transits of TRAPPIST-1e using each instrument, but in this case without randomized noise added to the observations.
Paper: Simulating Secondary Electron and Ion Emission from the Cassini Spacecraft in Saturn’s Ionosphere
Authors: Z. Zhang, R. T. Desai, O. Shebanits, F. L. Johansson, Y. Miyake, H. Usui
Figure caption: Currents onto the Cassini spacecraft’s for two distinct regions: panels (ia–c) show the case of a negative floating potential induced when I SEE = 0.5 μA m−2 and I SIE = 0.05 μA m−2, and panels (iia–c) show the case of a positive floating potential induced when I SEE = 50 μA m−2 and I SIE = 0.5 μA m−2. The upper panels (ia) and (iia) show all the positive and negative currents inclusive, panels (ib) and (iib) show the currents associated with the emitted electrons along with the spacecraft potential, and the lower panels (ic) and (iic) show the currents associated with the emitted ions.
Paper: Simulating Secondary Electron and Ion Emission from the Cassini Spacecraft in Saturn’s Ionosphere
Authors: Z. Zhang, R. T. Desai, O. Shebanits, F. L. Johansson, Y. Miyake, H. Usui
Figure caption: Simulated plasma densities around the Cassini spacecraft. (a) shows the ionospheric ions, (b) shows the secondary emitted ions, (c) shows the inospheric electrons, and (d) shows the secondary emitted electrons. The plasma velocity, v flow, is predominantly along the Y-axis, and the magnetic field, B 0, is approximately antiparallel to this. Specific input parameters can be found in Table 1. The ionospheric electrons are electrostatically displaced upstream, resulting in a combination of ionospheric and secondary electrons surrounding the spacecraft. Electrons wings caused by propagating Langmuir waves further modify the plasma ahead of the spacecraft, and the negatively biased Langmuir Probe is visible as a region devoid of plasma. A schematic of the simulated spacecraft geometry can be found in Figure 1 of Zhang et al. (2021a).
Paper: Simulating Secondary Electron and Ion Emission from the Cassini Spacecraft in Saturn’s Ionosphere
Authors: Z. Zhang, R. T. Desai, O. Shebanits, F. L. Johansson, Y. Miyake, H. Usui
Figure caption: Spacecraft potential dependence upon the secondary electron emission current density (yield) with zero ion emission (blue) and where the ion emission is 10% of the electron emission (red).
Paper: Simulating Secondary Electron and Ion Emission from the Cassini Spacecraft in Saturn’s Ionosphere
Authors: Z. Zhang, R. T. Desai, O. Shebanits, F. L. Johansson, Y. Miyake, H. Usui
Figure caption: Spacecraft potential dependence upon temperature of the emitted electrons.
Paper: OSSOS. XXVII. Population Estimates for Theoretically Stable Centaurs between Uranus and Neptune
Authors: Rosemary C. Dorsey, Michele T. Bannister, Samantha M. Lawler, Alex H. Parker
Figure caption: Orbital phase space of both the initial and final states of the test particles that survived 4.5 Gyr of integration by Zhang & Gladman (2022), used here as the input model for the OSSOS survey simulator to assess the size of the intrinsic population. The crosses and diamonds indicate states of the inner band (a < 25.2 au) and the outer band (a > 25.2 au), respectively. For a comparison between the initial and final states of individual particles, see Figure 6 of Zhang & Gladman (2022).
Paper: OSSOS. XXVII. Population Estimates for Theoretically Stable Centaurs between Uranus and Neptune
Authors: Rosemary C. Dorsey, Michele T. Bannister, Samantha M. Lawler, Alex H. Parker
Figure caption: Overlap of the orbital phase space of the test particles that survived Gyr integration by Zhang & Gladman (2022) (black density plot) and the combined test particle outputs from three planetary migration simulations (green crosses; Nesvorný et al. simulations).
Paper: Mechanical Modification of Chondrule Fine-grained Rims by Dusty Nebular Shocks
Authors: Augusto Carballido, Lorin S. Matthews, Romy D. Hanna, Truell W. Hyde
Figure caption: Lagrangian tracer data at t = 0.80 μs in four of our simulations: run 1 (first row; v imp = 0.5 km s−1, f cloud = 0.005, f FGR = 0.1), run 6 (second row; v imp = 0.5 km s−1, f cloud = 0.1, f FGR = 0.3), run 51 (third row; v imp = 1.0 km s−1, f cloud = 0.1, f FGR = 0.3), and run 87 (fourth row; v imp = 3.0 km s−1, f cloud = 0.1, f FGR = 0.3). The left column shows the chondrule in blue, the FGR in cyan, and the impacting dust in magenta. The middle column shows the maximum temperature recorded up to that time, and the right column shows the maximum recorded pressure. One should note the different temperature and pressure scales in different rows.