adsabs/AstroCLIMB huggingface dataset:
Paper: Interior and Gravity Field Models for Uranus Suggest a Mixed-composition Interior: Implications for the Uranus Orbiter and Probe
Authors: Zifan Lin, Sara Seager, Benjamin P. Weiss
Figure caption: Corner plot showing the retrieved core mass fraction (%Core), mantle mass fraction (%Mantle), atmosphere mass fraction (%Atm), central pressure (﹩{\mathrm{log}}_{10}{P}_{{\rm{c}}}﹩, in GPa), central temperature (Tc, in K), heavy element mass fraction in the mantle (Zmantle), and heavy element mass fraction in the atmosphere (Zatm) of Uranus. Here, the mixed H2O–H/He composition is assumed (see Section 2.3). The dashed lines in the histograms outline 3σ ranges, while the  ±  values in the titles are 1σ ranges. Interior retrieval predicts a small core, massive mantle, and significant mixing of heavy elements into the atmosphere and mixing of light elements into the mantle.
Paper: Interior and Gravity Field Models for Uranus Suggest a Mixed-composition Interior: Implications for the Uranus Orbiter and Probe
Authors: Zifan Lin, Sara Seager, Benjamin P. Weiss
Figure caption: CMS model convergence for the validation run (Jupiter model with n = 1 polytrope, NL = 128, NM = 48). The lines show the change in Jn between consecutive steps, defined as ΔJn = Jn,s+1 − Jn,s, where s is the step number. Colors represent (from darkest to lightest) n = 0 to n = 30 harmonics. The higher-order harmonics reach convergence with ΔJn ∼10−13 more rapidly, while J2 is converged after ∼80 steps with ΔJn ∼10−11, comparable to the theoretical precision limit of Gaussian quadrature (∼10−12).
Paper: Transport and Mixing in Planetary Polar Vortices with Annular and Monopolar Potential Vorticity Structures
Authors: Jacob Shultis, William Seviour, Darryn Waugh, Anthony Toigo
Figure caption: CA calculations for both the annular and monopolar scenarios at 300, 400, and 500 K isentropic surfaces initialized at LS = 267°, with examples of contour progression after 3 sols for both annular (a), (d), (g) and monopolar (b), (e), (h) vortices with colors corresponding to similar regions of the vortices: outside vortex (green), vortex edge (red), and vortex interior (yellow). Stretching rates (per sol; solid line) vs. latitudinal PV gradient (10−5 K m2 kg−1 s−1 deg−1; dashed line) (c), (f), (i), with red lines notating the annular case and blue lines notating the monopolar case.
Paper: Transport and Mixing in Planetary Polar Vortices with Annular and Monopolar Potential Vorticity Structures
Authors: Jacob Shultis, William Seviour, Darryn Waugh, Anthony Toigo
Figure caption: CA stretching rates (fill) and PV (contours) for the time period LS = 267° to LS = 272° for both the annular (a) and monopolar (b) vortices by isentropic surface and equivalent latitude. The annular polar vortex shows a sloping of the location of the mixing barrier toward the pole with height associated with the location of the maximum latitudinal PV gradient until it becomes more monopolar and the barrier is then more constant in space.
Paper: Transport and Mixing in Planetary Polar Vortices with Annular and Monopolar Potential Vorticity Structures
Authors: Jacob Shultis, William Seviour, Darryn Waugh, Anthony Toigo
Figure caption: Idealized passive decay tracer with 1200 sol lifetime initialized at LS = 240° from the equator to 30°N now represented on pressure surfaces. Tracer relative mixing ratio (fill), meridional stream function (red contours; solid lines mean clockwise circulation and dashed lines represent counterclockwise circulation), and potential temperature surfaces (black contours) all averaged over 5 sol periods for three different time periods. The black dashed line indicates the tracer source region. In the subvortex region of both polar vortices there is transport of tracer from the midlatitudes into the polar regions, however in the annular case this tracer is then able to make its way upwards into the polar vortex interior.
Paper: Transport and Mixing in Planetary Polar Vortices with Annular and Monopolar Potential Vorticity Structures
Authors: Jacob Shultis, William Seviour, Darryn Waugh, Anthony Toigo
Figure caption: Idealized passive decay tracer with 1200 sol lifetime initialized from the equator to 30°N, showing the end of the 90 sol CA period. (a), (b): tracer relative mixing ratio (fill) and PV (red contours) with height. Panels (c), (d): 300 K and (e), (f) 200 K isentropic level distributions of tracer (fill) and PV (red contours). The black dashed line indicates the tracer source region. By the end of this 90 sol period, the polar regions aloft remain isolated from the midlatitudes, however below the annular polar vortex there is strong transport of tracers into the polar regions.
Paper: Transport and Mixing in Planetary Polar Vortices with Annular and Monopolar Potential Vorticity Structures
Authors: Jacob Shultis, William Seviour, Darryn Waugh, Anthony Toigo
Figure caption: Idealized passive decay tracer with 1200 sol lifetime initialized from 80° north to the pole, showing the end of the 90 sol CA period. Panels (a), (b): tracer relative mixing ratio (fill) and PV (red contours) with height. Panels (c), (d): 300 K, and (e), (f): 200 K isentropic level distributions of tracer (fill) and PV (red contours). The black dashed line in all panels indicates the latitudinal limit of the tracer source region. By the end of this 90 sol period, the tracer remains isolated to the polar region with no sign of it crossing the polar vortex edge.
Paper: Transport and Mixing in Planetary Polar Vortices with Annular and Monopolar Potential Vorticity Structures
Authors: Jacob Shultis, William Seviour, Darryn Waugh, Anthony Toigo
Figure caption: CA stretching rates (fill) and PV (contours) for both annular (panels (a), (b), and (c)) and monopolar (panels (d), (e), and (f)) vortices with time, for three isentropic surfaces of 300, 400, and 500 K. Over the course of this 90 sol period, both polar vortices maintain a mixing barrier associated with the strongest latitudinal gradient of the PV.
Paper: A Pluto–Charon Sonata. V. Long-term Stability of the HST State Vector
Authors: Scott J. Kenyon, Benjamin C. Bromley
Figure caption: Lifetime of each model Pluto–Charon satellite system as a function of the mass factor f for calculations with (from left to right within each group) fS,K = 1.0 (purple points), 1.5 (blue points), 2.0 (green points), and 3.0 (orange points). The horizontal gray dotted line indicates the current age of the Sun. The light blue horizontal lines indicate the median lifetime of the full set of calculations with f = 1.0, 1.25, or 1.5 and any fS,K.
Paper: Transport and Mixing in Planetary Polar Vortices with Annular and Monopolar Potential Vorticity Structures
Authors: Jacob Shultis, William Seviour, Darryn Waugh, Anthony Toigo
Figure caption: Latitudinal gradient of zonally averaged zonal wind (in meters per second per degree; dashed lines) and stretching rates (solid lines) for planetWRF at 300 K initialized at LS = 267° (left) and shallow water with strong relaxation ﹩{t}_{r}﹩ = 0.25 (right) results. In both cases the maximum wind shear is equatorward of the mixing barrier at the polar vortex edge.
Paper: Reprocessing the NEAT Data Set: Preliminary Results
Authors: C. R. Nugent, J. M. Bauer, O. Benitez, M. Blain, N. D'Souza, S. Garimella, M. Goldwater, Y. Kim, H. C. G. Larsen, T. Linder, K. Mackowiak, Z. McGinnis, E. Pan, C. C. Pedersen, P. Sadhwani, F. Spoto, N. J. Tan, P. Vereš, C. Xue
Figure caption: The nine features identified by the machine learning model. This set of images represents how the thumbnails were divided into regions by the algorithm to allow for classification. To be classified as a positive source, an image needed to have bright pixels corresponding to the bright regions in the center middle and bottom middle squares, for example. This represents the model used; similar models with slightly more or fewer features would have also been successful for the classification used in this work.
Paper: Reprocessing the NEAT Data Set: Preliminary Results
Authors: C. R. Nugent, J. M. Bauer, O. Benitez, M. Blain, N. D'Souza, S. Garimella, M. Goldwater, Y. Kim, H. C. G. Larsen, T. Linder, K. Mackowiak, Z. McGinnis, E. Pan, C. C. Pedersen, P. Sadhwani, F. Spoto, N. J. Tan, P. Vereš, C. Xue
Figure caption: Two regions from a TriCam “a” camera image taken on 2001 November 20. These regions are from two different CCD regions on the same camera and show characteristic noise and artifacts. The NEAT TriCam images are morphologically different from modern CCD images, with more noise and artifacts.
Paper: Reprocessing the NEAT Data Set: Preliminary Results
Authors: C. R. Nugent, J. M. Bauer, O. Benitez, M. Blain, N. D'Souza, S. Garimella, M. Goldwater, Y. Kim, H. C. G. Larsen, T. Linder, K. Mackowiak, Z. McGinnis, E. Pan, C. C. Pedersen, P. Sadhwani, F. Spoto, N. J. Tan, P. Vereš, C. Xue
Figure caption: A NEAT TriCam image frame before (left) and after (right) background subtraction. Algorithmic background subtraction was chosen as it produced uniform results over a range of frames and allowed for the detection of faint sources.
Paper: Reprocessing the NEAT Data Set: Preliminary Results
Authors: C. R. Nugent, J. M. Bauer, O. Benitez, M. Blain, N. D'Souza, S. Garimella, M. Goldwater, Y. Kim, H. C. G. Larsen, T. Linder, K. Mackowiak, Z. McGinnis, E. Pan, C. C. Pedersen, P. Sadhwani, F. Spoto, N. J. Tan, P. Vereš, C. Xue
Figure caption: Example output of helper software used to create and evaluate the machine learning model. A false positive (left) and an example of a misclassified positive source (right) are shown. Users can use the left or right arrow keys to reclassify the images, if desired.
Paper: Reprocessing the NEAT Data Set: Preliminary Results
Authors: C. R. Nugent, J. M. Bauer, O. Benitez, M. Blain, N. D'Souza, S. Garimella, M. Goldwater, Y. Kim, H. C. G. Larsen, T. Linder, K. Mackowiak, Z. McGinnis, E. Pan, C. C. Pedersen, P. Sadhwani, F. Spoto, N. J. Tan, P. Vereš, C. Xue
Figure caption: An example of a frame that experienced telescope movement during the exposure. These frames were identified by the pipeline and ignored.
Paper: Reprocessing the NEAT Data Set: Preliminary Results
Authors: C. R. Nugent, J. M. Bauer, O. Benitez, M. Blain, N. D'Souza, S. Garimella, M. Goldwater, Y. Kim, H. C. G. Larsen, T. Linder, K. Mackowiak, Z. McGinnis, E. Pan, C. C. Pedersen, P. Sadhwani, F. Spoto, N. J. Tan, P. Vereš, C. Xue
Figure caption: Comparison between the brightnesses of the new and remeasured observations produced by this work. The reprocessing pipeline successfully finds fainter objects, though it also finds bright (13 mag) observations not previously reported to the Minor Planet Center.
Paper: Reprocessing the NEAT Data Set: Preliminary Results
Authors: C. R. Nugent, J. M. Bauer, O. Benitez, M. Blain, N. D'Souza, S. Garimella, M. Goldwater, Y. Kim, H. C. G. Larsen, T. Linder, K. Mackowiak, Z. McGinnis, E. Pan, C. C. Pedersen, P. Sadhwani, F. Spoto, N. J. Tan, P. Vereš, C. Xue
Figure caption: The speed of the new tracklets is roughly comparable in distribution to the speed of the previously submitted tracklets.
Paper: Recent Tectonic Deformation of the Lunar Farside Mare and South Pole–Aitken Basin
Authors: C. A. Nypaver, T. R. Watters, J. D. Clark
Figure caption: (A) SPA SMR elastic dislocation model (orange lines) and corresponding SPA SMR topographic cross section (blue lines) for the SPA SMR (vert. exag.: 21.4). (B) Modeled fault dip angle (θ), fault depth (Z1–Z2), and SMR topographic relief (h) are shown to scale with quantitative values given in Table 1 (vertical exaggeration: 2.1).
Paper: Recent Tectonic Deformation of the Lunar Farside Mare and South Pole–Aitken Basin
Authors: C. A. Nypaver, T. R. Watters, J. D. Clark
Figure caption: (A) Distribution of farside SMRs (yellow polylines) relative to lunar maria (red polygons) and overlaid onto an LROC Wide Angle Camera global mosaic centered at a 180° meridian. (B) Small-scale image (LROC NAC M1392716156LE) of the SPA SMR cluster showing individual ridge segments (white arrows). (C) Farside SMR cluster directional means (orange lines) overlaid onto the predicted feature orientations that would result from the combination of global contraction, orbital recession, and solid body tides (T. R. Watters et al. 2015; I. Matsuyama et al. 2021).
Paper: Recent Tectonic Deformation of the Lunar Farside Mare and South Pole–Aitken Basin
Authors: C. A. Nypaver, T. R. Watters, J. D. Clark
Figure caption: (A) SPA SMR segment (white arrows) and the associated ridge-adjacent crater-counting area (white box; LROC NAC image M1392716156LE). (B) A cumulative and (C) relative CSFD measurement derived within the designated ridge-adjacent count area (black dots). A PDF fit with a resurfacing correction is assigned to impact craters in the diameter range of 13–23 m to produce an AMA of ﹩{84}_{-10}^{+10}﹩ Ma (green triangles).
Paper: Recent Tectonic Deformation of the Lunar Farside Mare and South Pole–Aitken Basin
Authors: C. A. Nypaver, T. R. Watters, J. D. Clark
Figure caption: (A) Bolyai SMR segment (white arrows) and the associated ridge-adjacent crater-counting area (white box; LROC NAC image M1128679429). (B) A cumulative and (C) relative CSFD measurement derived within the designated ridge-adjacent count area (black dots). A PDF fit with a resurfacing correction is assigned to impact craters in the diameter range of 10–31 m to produce an AMA of ﹩{96}_{-6}^{+6}﹩ Ma (green triangles).
Paper: Recent Tectonic Deformation of the Lunar Farside Mare and South Pole–Aitken Basin
Authors: C. A. Nypaver, T. R. Watters, J. D. Clark
Figure caption: (A) SMR elastic dislocation model (orange lines) and corresponding SPA SMR topographic cross section (blue lines) for the SPA SMR (vert. exag.: 22). (B) Modeled fault dip angle (θ), fault depth (Z1–Z2), and SMR topographic relief (h) are shown to scale with quantitative values given in Table 1 (vert. exag.: 3.9). A ∼5 m elevation offset resulting from background slope was removed from the Aitken crater SMR topographic profile before Coulomb model fitting.
Paper: Recent Tectonic Deformation of the Lunar Farside Mare and South Pole–Aitken Basin
Authors: C. A. Nypaver, T. R. Watters, J. D. Clark
Figure caption: (A) Bolyai Crater SMR elastic dislocation model (orange lines) and corresponding SPA SMR topographic cross section (blue lines) for the Bolyai SMR (vert. exag.: 31.3). (B) Modeled fault dip angle (θ), fault depth (Z1–Z2), and SMR topographic relief (h) are shown to scale with quantitative values given in Table 1 (vert. exag.: 4.2).
Paper: Recent Tectonic Deformation of the Lunar Farside Mare and South Pole–Aitken Basin
Authors: C. A. Nypaver, T. R. Watters, J. D. Clark
Figure caption: A small (∼6 m diameter) impact crater that has been crosscut by the Bolyai SMR (125.3542, −33.1757) shown in (A) NAC M169745132LC (0.52 m px−1, 37.38 incidence angle) and (B) NAC M1128672317LC (0.76 m px−1, 60.4 incidence angle). The equilibrium lifetime of an impact crater with a diameter of ∼6 m is ∼27 Ma. The coordinates, diameters, and equilibrium lifetimes of all crosscut craters identified in the work are documented in Table A1.
Paper: Recent Tectonic Deformation of the Lunar Farside Mare and South Pole–Aitken Basin
Authors: C. A. Nypaver, T. R. Watters, J. D. Clark
Figure caption: (A) Aitken Crater SMR segment (white arrows) and the associated ridge-adjacent crater-counting area (white box; LROC NAC image M1217824555RE). (B) A cumulative and (C) relative CSFD measurement derived within the designated ridge-adjacent count area (black dots). A PDF fit with a resurfacing correction is assigned to impact craters in the diameter range of 15–30 m to produce an AMA of ﹩{160}_{-10}^{+20}﹩ Ma (green triangles).
Paper: Recent Tectonic Deformation of the Lunar Farside Mare and South Pole–Aitken Basin
Authors: C. A. Nypaver, T. R. Watters, J. D. Clark
Figure caption: Large-scale map of the Aitken SMR cluster (green polylines) and surrounding mare (red polylines). The Aitken SMR cluster is predominantly located in the eastern portion of the Aitken crater floor mare deposits. The Aitken SMR segment chosen for dislocation modeling in this work is represented by a yellow star.
Paper: Recent Tectonic Deformation of the Lunar Farside Mare and South Pole–Aitken Basin
Authors: C. A. Nypaver, T. R. Watters, J. D. Clark
Figure caption: Large-scale map of the SPA SMR cluster (green polylines) and surrounding mare (red polylines). This SMR cluster is located in a narrow region of a central SPA mare deposit. The SPA SMR segment chosen for dislocation modeling in this work is represented by a yellow star.
Paper: Recent Tectonic Deformation of the Lunar Farside Mare and South Pole–Aitken Basin
Authors: C. A. Nypaver, T. R. Watters, J. D. Clark
Figure caption: Large-scale map of the Bolyai SMR cluster (green polylines) and surrounding mare (red polylines). The Bolyai SMR cluster is located within the northern Bolyai crater floor mare deposits. The Bolyai SMR segment chosen for dislocation modeling in this work is represented by a yellow star.
Paper: Investigating Temporal and Spatial Variation of Jupiter’s Atmosphere with Radio Observations
Authors: Joanna Hardesty, Chris Moeckel, Imke de Pater
Figure caption: Juno MWR C4 brightness temperature measurements for each PJ superimposed on image slices of Jupiter, taken close to the time that the flyby occurred and plotted between ±45° planetographic latitude. Further information about the visible image slices can be found in Table 1. All MWR brightness temperature values correspond to the same color bar at the center of the image. The HST images are all from project ID GO-14661 (M. Wong 2017; M. H. Wong et al. 2020). Credit for JunoCam maps (PJs 1, 8, and 9): NASA/JPL/SwRI/MSSS/Gerald Eichstädt/John Rogers.
Paper: Investigating Temporal and Spatial Variation of Jupiter’s Atmosphere with Radio Observations
Authors: Joanna Hardesty, Chris Moeckel, Imke de Pater
Figure caption: Similar to Figure 1 but for Juno MWR C6.
Paper: Investigating Temporal and Spatial Variation of Jupiter’s Atmosphere with Radio Observations
Authors: Joanna Hardesty, Chris Moeckel, Imke de Pater
Figure caption: Similar to Figure 1 but for Juno MWR C5.
Paper: Spectral Effects of Shock Darkening on Ordinary Chondrite and Howardite, Eucrite, and Diogenite Meteorites
Authors: Juan A. Sanchez, Vishnu Reddy, Lucille Le Corre, Neil Pearson, Adam Battle
Figure caption: Band I center vs. BAR diagram from M. J. Gaffey et al. (1993). Values measured for ordinary chondrites Chelyabinsk (LL5), Chergach (H5), and Viñales (L6) corresponding to 0%, 50%, and 100% shock darkening (SD) are shown. The increase in SD is represented as an increase in the opacity of the symbols. The polygonal region corresponds to the S(IV) subtype associated with ordinary chondrites (OC). The rectangular zone (BA) includes the pyroxene-dominated basaltic achondrite assemblages (M. J. Gaffey et al. 1993).
Paper: Spectral Effects of Shock Darkening on Ordinary Chondrite and Howardite, Eucrite, and Diogenite Meteorites
Authors: Juan A. Sanchez, Vishnu Reddy, Lucille Le Corre, Neil Pearson, Adam Battle
Figure caption: Molar content of Fa vs. ol/(ol+px) ratio for ordinary chondrites Chelyabinsk (LL5), Chergach (H5), and Viñales (L6) corresponding to 0% and 100% shock darkening (SD). The increase in SD is represented as an increase in the opacity of the symbols. The error bars correspond to the uncertainties derived by J. A. Sanchez et al. (2020), 2.0 mol% for Fa and 0.04 for the ol/(ol+px) ratio. Black dashed boxes represent the range of measured values for each ordinary chondrite subgroup. Gray solid boxes correspond to the uncertainties associated with the spectrally derived values. Figure adapted from T. L. Dunn et al. (2010).
Paper: Spectral Effects of Shock Darkening on Ordinary Chondrite and Howardite, Eucrite, and Diogenite Meteorites
Authors: Juan A. Sanchez, Vishnu Reddy, Lucille Le Corre, Neil Pearson, Adam Battle
Figure caption: Left: spectra of the L6 ordinary chondrites Chico and Renfrow. Right: the same spectra normalized to unity at 1.5 μm.
Paper: Spectral Effects of Shock Darkening on Ordinary Chondrite and Howardite, Eucrite, and Diogenite Meteorites
Authors: Juan A. Sanchez, Vishnu Reddy, Lucille Le Corre, Neil Pearson, Adam Battle
Figure caption: Band I center vs. BAR diagram from M. J. Gaffey et al. (1993). Values measured for ordinary chondrites Chico (L6), Ghubara (L5), NWA 4860 (L4), Pampa-C (L4), Renfrow (L6), Tassédet (H5), and Tsarev (L5) are shown. These samples do not show a light/dark structure, but a rather dark and uniform color. The polygonal region corresponds to the S(IV) subtype associated with ordinary chondrites (OC). The rectangular zone (BA) includes the pyroxene-dominated basaltic achondrite assemblages (M. J. Gaffey et al. 1993).
Paper: Spectral Effects of Shock Darkening on Ordinary Chondrite and Howardite, Eucrite, and Diogenite Meteorites
Authors: Juan A. Sanchez, Vishnu Reddy, Lucille Le Corre, Neil Pearson, Adam Battle
Figure caption: Top: reflectance measured at 0.55 μm and spectral slope vs. fraction of shock darkening for ordinary chondrites Chelyabinsk (LL5), Chergach (H5), and Viñales (L6). Bottom: band I and II depths vs. fraction of shock darkening. Uncertainties are smaller than the symbols.
Paper: Spectral Effects of Shock Darkening on Ordinary Chondrite and Howardite, Eucrite, and Diogenite Meteorites
Authors: Juan A. Sanchez, Vishnu Reddy, Lucille Le Corre, Neil Pearson, Adam Battle
Figure caption: Principal components PC2' vs. PC1' diagram from F. E. DeMeo et al. (2009). PC values calculated for ordinary chondrites Chelyabinsk (LL5), Chergach, (H5) and Viñales (L6) corresponding to 0%, 50%, and 100% shock darkening (SD) are depicted with different symbols. The increase in SD is represented as an increase in the opacity of the symbols. The arrow indicates the direction in which shock darkening increases.
Paper: Spectral Effects of Shock Darkening on Ordinary Chondrite and Howardite, Eucrite, and Diogenite Meteorites
Authors: Juan A. Sanchez, Vishnu Reddy, Lucille Le Corre, Neil Pearson, Adam Battle
Figure caption: Left: spectra of the L5 Ghubara, L4 NWA 4860, L4 Pampa-C, H5 Tassédet, and L5 Tsarev. Right: the same spectra normalized to unity at 1.5 μm.
Paper: Spectral Effects of Shock Darkening on Ordinary Chondrite and Howardite, Eucrite, and Diogenite Meteorites
Authors: Juan A. Sanchez, Vishnu Reddy, Lucille Le Corre, Neil Pearson, Adam Battle
Figure caption: PC2’ vs. PC1’ diagram from F. E. DeMeo et al. (2009). PC values calculated for ordinary chondrites Chico (L6), Ghubara (L5), NWA 4860 (L4), Pampa-C (L4), Renfrow (L6), Tassédet (H5), and Tsarev (L5) are depicted with different symbols.
Paper: Spectral Effects of Shock Darkening on Ordinary Chondrite and Howardite, Eucrite, and Diogenite Meteorites
Authors: Juan A. Sanchez, Vishnu Reddy, Lucille Le Corre, Neil Pearson, Adam Battle
Figure caption: Left: spectra of eucrite NWA 7266 corresponding to 0%, 50%, and 100% shock darkening (SD). Right: the same spectra normalized to unity at 1.5 μm.
Paper: Spectral Effects of Shock Darkening on Ordinary Chondrite and Howardite, Eucrite, and Diogenite Meteorites
Authors: Juan A. Sanchez, Vishnu Reddy, Lucille Le Corre, Neil Pearson, Adam Battle
Figure caption: Band I center vs. BAR diagram from M. J. Gaffey et al. (1993). Values measured for diogenite NWA 4664 and eucrites NWA 7266 and NWA 8563 corresponding to different fractions of shock darkening (SD) are shown. The increase in SD is represented as an increase in the opacity of the symbols. The polygonal region corresponds to the S(IV) subtype associated with ordinary chondrites (OC). The rectangular zone (BA) includes the pyroxene-dominated basaltic achondrite assemblages (M. J. Gaffey et al. 1993).