adsabs/AstroCLIMB huggingface dataset:
Paper: Using Rover-analogous Methodology to Discriminate between Volcanic and Sedimentary Origins in Successions Dominated by Igneous Composition
Authors: R. Aileen Yingst, Julie K. Bartley, Barbara A. Cohen, Brian M. Hynek, Linda C. Kah, Richard Archer, Michael Lotto, Jennifer Tuggle Mooney, Justin L. Wang, Brittan Wogsland, Robert F. Coker
Figure caption: Sedimentary structures observed within units 2–6. (a) Scarp face showing cross beds, white shell beds, and scoured surfaces. (b) Close-up image of shell bed scour and one shell bed facies showing more fragmented shells. (c) Outcrop scale image of trough multidirectional cross beds. (d) Bed-scale image showing cobbles embedded within a sandstone bed alongside shell fragments.
Paper: Using Rover-analogous Methodology to Discriminate between Volcanic and Sedimentary Origins in Successions Dominated by Igneous Composition
Authors: R. Aileen Yingst, Julie K. Bartley, Barbara A. Cohen, Brian M. Hynek, Linda C. Kah, Richard Archer, Michael Lotto, Jennifer Tuggle Mooney, Justin L. Wang, Brittan Wogsland, Robert F. Coker
Figure caption: Unit 1 facies as observed by the Tiger team. (a) contextual image of the conglomerates overlying the red toned hyaloclastite. (b) Long-range view of basalt beds. (c) image of the contact between the spheroidally weathering red brown hyaloclastite and the conglomerate scouring into it. (d) Close-up of variable clast compositions within the unstratified conglomerate; the dark-brown clast in the center is ∼60 cm across. (e) Bed variability within the stratified conglomerate, where the finer beds show more intense grading. (f) Close-up of cross-bedded sandstone lens. (g) Alternating finely bedded mudstone and fine sandstone showing a drop stone and scour marks on the bottom of some sandstone beds.
Paper: Using Rover-analogous Methodology to Discriminate between Volcanic and Sedimentary Origins in Successions Dominated by Igneous Composition
Authors: R. Aileen Yingst, Julie K. Bartley, Barbara A. Cohen, Brian M. Hynek, Linda C. Kah, Richard Archer, Michael Lotto, Jennifer Tuggle Mooney, Justin L. Wang, Brittan Wogsland, Robert F. Coker
Figure caption: Sedimentary facies observed within units 7–10. (a) Scarp face showing the cross beds in unit 8 in the foreground sandwiched between the cobbles of units 7 and 9. (b) South-facing image across the gorge showing the step between the boulder-rich base of unit 10 and the matrix-rich upper facies of unit 10. (c) Upstream view showing the light-toned beds replacing the basal boulder-rich facies of unit 10 and terraces within the valley. (d) Hand sample of glacial striations on a clast from unit 10.
Paper: Using Rover-analogous Methodology to Discriminate between Volcanic and Sedimentary Origins in Successions Dominated by Igneous Composition
Authors: R. Aileen Yingst, Julie K. Bartley, Barbara A. Cohen, Brian M. Hynek, Linda C. Kah, Richard Archer, Michael Lotto, Jennifer Tuggle Mooney, Justin L. Wang, Brittan Wogsland, Robert F. Coker
Figure caption: Drone-acquired centimeter-scale image of the unconformity between units 6 and 7, requested by the Rover team.
Paper: Using Rover-analogous Methodology to Discriminate between Volcanic and Sedimentary Origins in Successions Dominated by Igneous Composition
Authors: R. Aileen Yingst, Julie K. Bartley, Barbara A. Cohen, Brian M. Hynek, Linda C. Kah, Richard Archer, Michael Lotto, Jennifer Tuggle Mooney, Justin L. Wang, Brittan Wogsland, Robert F. Coker
Figure caption: Images of unit 2a acquired by (a) the Rover team and (b) the Tiger team. Images are at the same scale.
Paper: The “Snow Line” on Venus’s Maxwell Montes: Varying Elevation Implies a Dynamic Atmosphere
Authors: Andriana Strezoski, Allan H. Treiman
Figure caption: Maxwell’s snow line using Magellan’s Fresnel reflectivity data. Graph shows elevations (from Magellan GTDR) at which the Fresnel reflectivity = ∼0.35, moving around the snow line as in Figure 1 of the main text. Color coding is the same as in Figure 1 (main text), with the SE corner of Maxwell at approximately the transition from yellow to red. Note that the pattern of elevation follows closely to that of Figure 1. Distances are not the same as in Figure 1, because the Fresnel reflectivity data have a greater pixel size than the SAR reflectivity, see Kappraff (1986).
Paper: The “Snow Line” on Venus’s Maxwell Montes: Varying Elevation Implies a Dynamic Atmosphere
Authors: Andriana Strezoski, Allan H. Treiman
Figure caption: Emissivity, Fresnel reflectivity, and their sums on traverses across Maxwell (See Figure 2, main text). Gaps and irregularities near the centers of the profiles (∼350 km) reflect a gap in the emissivity data. Some other irregularities and sums greater than unity likely represent misregistration of emissivity and Fresnel reflectivity footprints, errors associated with extremely steep slopes (profile 2, ∼275 km), and that reflectivity represents partially the orientations of slope facets with respect to the incoming radar beam. Note that the sum is near 0.95 (Plaut 1993) for the flat plains of Lakshmi Planum (left side, profile 2) and the rough highlands of Fortuna Tessera (right sides, both profiles).
Paper: Degradation of the Lunar Surface by Small Impacts
Authors: Patrick O'Brien, Shane Byrne
Figure caption: Crater fluxes required to achieve a small impact erosion rate consistent with the observed maria diffusivity (Fassett & Thomson 2014). The primary crater SFD is given by the NPF (Neukum et al. 2001) down to a diameter of 12 m. For smaller primaries, a steeper-sloped power law is used following LRO observations of fresh craters (Speyerer et al. 2016). The global secondary crater SFD produced by this cratering rate is generated from a Monte Carlo model according to observations of secondary production on airless bodies (O’Brien & Byrne 2021).
Paper: Degradation of the Lunar Surface by Small Impacts
Authors: Patrick O'Brien, Shane Byrne
Figure caption: Kilometer-scale diffusivity (D max = 100 m) from small impacts under a broken power-law cratering rate where the steep branch of the primary SFD has slope λ  p0 and diffusive mass transport extends down to a crater diameter of D min. The solid black contour line represents a zero-slope diffusivity of 5.20 m2 Myr−1, equivalent to the linear diffusivity measured by Fassett & Thomson (2014). The dashed line shows the SFD slope for fresh craters detected by LRO (shaded region is the 95% confidence interval; Speyerer et al. 2016).
Paper: Degradation of the Lunar Surface by Small Impacts
Authors: Patrick O'Brien, Shane Byrne
Figure caption: The small impact diffusion rate, shown here for D max = 100 m, is nonlinear, increasing with topographic gradient. Over 3 Gyr, nonlinear topographic diffusion with a zero-slope diffusivity of 5.20 m2 Myr−1 would degrade a 1 km crater to the same depth as linear diffusion with a diffusivity of 5.5 m2 Myr−1, the average diffusivity measured on the lunar maria (Fassett & Thomson 2014).
Paper: Degradation of the Lunar Surface by Small Impacts
Authors: Patrick O'Brien, Shane Byrne
Figure caption: The small impact diffusion rate is weakly scale dependent. Larger surface features are eroded by a wider range of crater diameters (larger D max) and therefore experience a higher diffusivity. Over the diameter range where eroding impacts produce simple crater morphologies (﹩{D}_{\max }\,\lesssim ﹩ 15 km), the zero-slope diffusivity varies by ∼35%.
Paper: Using Rover-analogous Methodology to Discriminate between Volcanic and Sedimentary Origins in Successions Dominated by Igneous Composition
Authors: R. Aileen Yingst, Julie K. Bartley, Barbara A. Cohen, Brian M. Hynek, Linda C. Kah, Richard Archer, Michael Lotto, Jennifer Tuggle Mooney, Justin L. Wang, Brittan Wogsland, Robert F. Coker
Figure caption: Images from unit 1 requested by the Rover team. (a) Centimeter-scale mosaic showing unconformity between two units. (b) Handlens-scale image acquired from unit 1b (exact location of acquisition unknown). Individual clasts as small as 70–100 μm diameter can be resolved, floating in a finer-grained matrix. (c) Handlens-scale image acquired from unit 1a (exact location of acquisition is at a camera-accessible point farther away in the unit). Texture is indicative of vesicular basaltic lava flows, but it is not clear from this image whether the light-toned interstitial material is a coating or a primary texture. The location of this unit in relation to other units is shown in Figure 5.
Paper: Using Rover-analogous Methodology to Discriminate between Volcanic and Sedimentary Origins in Successions Dominated by Igneous Composition
Authors: R. Aileen Yingst, Julie K. Bartley, Barbara A. Cohen, Brian M. Hynek, Linda C. Kah, Richard Archer, Michael Lotto, Jennifer Tuggle Mooney, Justin L. Wang, Brittan Wogsland, Robert F. Coker
Figure caption: Mesoscale image showing the stratigraphy that is exposed on either side of the channel. Unit designations assigned by the Rover team are noted. Unit 1 is not visible in this image; units 9 and 10 slope away from the viewer at the top of the hill. Persons for scale.
Paper: Using Rover-analogous Methodology to Discriminate between Volcanic and Sedimentary Origins in Successions Dominated by Igneous Composition
Authors: R. Aileen Yingst, Julie K. Bartley, Barbara A. Cohen, Brian M. Hynek, Linda C. Kah, Richard Archer, Michael Lotto, Jennifer Tuggle Mooney, Justin L. Wang, Brittan Wogsland, Robert F. Coker
Figure caption: (a) Geologic context of study area in north Iceland, with the field site indicated by the red square. The inset shows a geologic map of the field site (modified from Figures 3.6 and 5.60 of Eiríksson & Símonarson 2021). (b) Left: stratigraphic section exposed at the field site; North Hill is in the background, with South Hill in the foreground. Right: stratigraphic column of lithologic units within the study region, with height above sea level in meters. The vertical black bar on the right indicates the sequence of units encountered by the team (modified from Figure 5.57 of Eiríksson & Símonarson 2021).
Paper: Using Rover-analogous Methodology to Discriminate between Volcanic and Sedimentary Origins in Successions Dominated by Igneous Composition
Authors: R. Aileen Yingst, Julie K. Bartley, Barbara A. Cohen, Brian M. Hynek, Linda C. Kah, Richard Archer, Michael Lotto, Jennifer Tuggle Mooney, Justin L. Wang, Brittan Wogsland, Robert F. Coker
Figure caption: Full-color orthomosaic of ROI, showing notional locations originally planned for in situ investigation (A–D).
Paper: Using Rover-analogous Methodology to Discriminate between Volcanic and Sedimentary Origins in Successions Dominated by Igneous Composition
Authors: R. Aileen Yingst, Julie K. Bartley, Barbara A. Cohen, Brian M. Hynek, Linda C. Kah, Richard Archer, Michael Lotto, Jennifer Tuggle Mooney, Justin L. Wang, Brittan Wogsland, Robert F. Coker
Figure caption: Mosaic of drone-acquired images showing the location of the only accessible expression of unit 1 (arrow), shown in relation to the sequence of units 2–10 in the main field site.
Paper: Using Rover-analogous Methodology to Discriminate between Volcanic and Sedimentary Origins in Successions Dominated by Igneous Composition
Authors: R. Aileen Yingst, Julie K. Bartley, Barbara A. Cohen, Brian M. Hynek, Linda C. Kah, Richard Archer, Michael Lotto, Jennifer Tuggle Mooney, Justin L. Wang, Brittan Wogsland, Robert F. Coker
Figure caption: Units 2–3 at (a) millimeter scale, (b, c) handlens scale, and (d) submillimeter scale (mosaic) as requested by the Rover team. (a) Three-image mosaic showing transition from unit 2 to unit 3, differentiated by the blue line. Red boxes indicate the location of inset images. (b) Dark, fine-grained portion of unit 3. (c) Light-toned portion of unit 3. (d) Three-image mosaic of potential cross-bedding location in unit 2.
Paper: Using Rover-analogous Methodology to Discriminate between Volcanic and Sedimentary Origins in Successions Dominated by Igneous Composition
Authors: R. Aileen Yingst, Julie K. Bartley, Barbara A. Cohen, Brian M. Hynek, Linda C. Kah, Richard Archer, Michael Lotto, Jennifer Tuggle Mooney, Justin L. Wang, Brittan Wogsland, Robert F. Coker
Figure caption: Drone-acquired true-color orthomosaic of field site mimicking orbital data. Topographic contour intervals of 5 m are overlaid, from 0 to 45 m elevation.
Paper: Numerical Simulations of Drainage Grooves in Response to Extensional Fracturing: Testing the Phobos Groove Formation Model
Authors: Bin Cheng, Erik Asphaug, Ronald-Louis Ballouz, Yang Yu, Hexi Baoyin
Figure caption: Different regimes of granular failure pattern deduced from SSDEM simulations using different cohesion strengths for regolith patches across the surface of Phobos. The simulated cells are expanded and/or shrunk biaxially, the ratio of which is determined by the predicted tidal stresses imposed by the moon’s orbital migration (Hurford et al. 2016). Arrows show the deformation directions. The stress ratio and tensile strength can be used to distinguish between intact deformation, polygonal topology, fragmented segments, and parallel pattern, as indicated by their outline colors. The formation of parallel grooves requires larger cohesion and lower stress ratio. Only one of the patches with similar stress ratio is shown here.
Paper: Numerical Simulations of Drainage Grooves in Response to Extensional Fracturing: Testing the Phobos Groove Formation Model
Authors: Bin Cheng, Erik Asphaug, Ronald-Louis Ballouz, Yang Yu, Hexi Baoyin
Figure caption: Model-predicted geomorphologies of grooves and underlying fractures. Most grooves appear shallow, with depths of 10–30 m and widths of 80–120 m, broadly consistent with observations. Slopes of groove walls are measured to be around ∼25°, close to the angle of repose for loose regolith. The narrow, steeply plunging fractures penetrate deep inside the cohesive layer, morphologically analogous to extensional crevasses on terrestrial glaciers, but here for much weaker materials in much lower gravity. Data are from the simulation case of c  p  = 36 kPa.
Paper: Investigating the Martian Surface at Decametric Scale: Population, Distribution, and Dimension of Heterogeneity from Radar Statistics
Authors: Cyril Grima, Nathaniel E. Putzig, Bruce A. Campbell, Matthew Perry, Sean P. S. Gulick, Russell C. Miller, Aaron T. Russell, Kirk M. Scanlan, Gregor Steinbrügge, Duncan A. Young, Scott D. Kempf, Gregory Ng, Dillon Buhl, Donald D. Blankenship
Figure caption: Maps and associated distributions of derived surface HK parameters. μ values higher than 10 are saturated as they cannot be discriminated with sufficient precision by our estimator. Black contours outline geologic unit boundaries (Tanaka et al. 2014). Red stars indicate Insight (+4°.5) and Curiosity (−4°.6) landing sites. The bottom left panel depicts the distribution of the measured surface echoes in the P  c  − P  n  space and also exhibits red contours outlining the distribution of background noise also shown in Figure 6.
Paper: Investigating the Martian Surface at Decametric Scale: Population, Distribution, and Dimension of Heterogeneity from Radar Statistics
Authors: Cyril Grima, Nathaniel E. Putzig, Bruce A. Campbell, Matthew Perry, Sean P. S. Gulick, Russell C. Miller, Aaron T. Russell, Kirk M. Scanlan, Gregor Steinbrügge, Duncan A. Young, Scott D. Kempf, Gregory Ng, Dillon Buhl, Donald D. Blankenship
Figure caption: Measurement distribution in the 2D P  c  − P  n  space overlapped by approximation of surface roughness parameters as described in Section 4.3 (red grid). Note that ﹩{P}_{{c}_{0}}\approx 76\,{dB}﹩ is set as a flat surface reference with σ  h  = 0.
Paper: Investigating the Martian Surface at Decametric Scale: Population, Distribution, and Dimension of Heterogeneity from Radar Statistics
Authors: Cyril Grima, Nathaniel E. Putzig, Bruce A. Campbell, Matthew Perry, Sean P. S. Gulick, Russell C. Miller, Aaron T. Russell, Kirk M. Scanlan, Gregor Steinbrügge, Duncan A. Young, Scott D. Kempf, Gregory Ng, Dillon Buhl, Donald D. Blankenship
Figure caption: Sketches illustrating three typical regimes depicting the relative evolution of the coherent (P  c , green) and incoherent (P  n , red) power with increasing surface roughness for a nadir-looking radar. Three regimes illustrating milestones in the evolution of the signal powers are placed on the P  c  − P  n  distribution plot (left). Each regime is also illustrated in a surface backscattering radiation pattern (right). Dotted curves depict the evolution with increasing roughness of the relative strength of each type of power component in the normal direction. The area between the dashed curves is the coherent content.
Paper: Investigating the Martian Surface at Decametric Scale: Population, Distribution, and Dimension of Heterogeneity from Radar Statistics
Authors: Cyril Grima, Nathaniel E. Putzig, Bruce A. Campbell, Matthew Perry, Sean P. S. Gulick, Russell C. Miller, Aaron T. Russell, Kirk M. Scanlan, Gregor Steinbrügge, Duncan A. Young, Scott D. Kempf, Gregory Ng, Dillon Buhl, Donald D. Blankenship
Figure caption: Results obtained from our surface picker when run over SHARAD radargrams’ background noise. Each point represents a P  c  and P  n  value associated to a single radargram. The whole cloud of points represents the range of RSR signature that should be expected in the absence of surface echo. Dashed diagonals are coherent content isolines.
Paper: Investigating the Martian Surface at Decametric Scale: Population, Distribution, and Dimension of Heterogeneity from Radar Statistics
Authors: Cyril Grima, Nathaniel E. Putzig, Bruce A. Campbell, Matthew Perry, Sean P. S. Gulick, Russell C. Miller, Aaron T. Russell, Kirk M. Scanlan, Gregor Steinbrügge, Duncan A. Young, Scott D. Kempf, Gregory Ng, Dillon Buhl, Donald D. Blankenship
Figure caption: (a) The recorded surface echo strength is the coherent summation of all the electric fields reflected and diffused at the surface within the scattering volume bounded by the footprint (∼5 km) and the near-surface depth (<15 m). (b) Physical properties of the surface and near surface that can contribute to the coherent and incoherent powers.
Paper: Investigating the Martian Surface at Decametric Scale: Population, Distribution, and Dimension of Heterogeneity from Radar Statistics
Authors: Cyril Grima, Nathaniel E. Putzig, Bruce A. Campbell, Matthew Perry, Sean P. S. Gulick, Russell C. Miller, Aaron T. Russell, Kirk M. Scanlan, Gregor Steinbrügge, Duncan A. Young, Scott D. Kempf, Gregory Ng, Dillon Buhl, Donald D. Blankenship
Figure caption: Error estimators for ﹩{\hat{P}}_{c}﹩, ﹩{\hat{P}}_{n}﹩, and ﹩\hat{\mu }﹩. (Top) Relative bias where warm (resp. cool) colors indicate overestimation (resp. underestimation) from the true value. For ease of use, the ﹩{\hat{P}}_{c}﹩ and ﹩{\hat{P}}_{n}﹩ plots include contours showing the relative bias from the true value in dB by increment of 1. (Bottom) Normalized standard deviation. The power components that are relatively weaker are usually derived with more uncertainty, although a stable domain exists when the coherent content is within ±5 dB (or, to some extent, pm 10 dB).
Paper: Investigating the Martian Surface at Decametric Scale: Population, Distribution, and Dimension of Heterogeneity from Radar Statistics
Authors: Cyril Grima, Nathaniel E. Putzig, Bruce A. Campbell, Matthew Perry, Sean P. S. Gulick, Russell C. Miller, Aaron T. Russell, Kirk M. Scanlan, Gregor Steinbrügge, Duncan A. Young, Scott D. Kempf, Gregory Ng, Dillon Buhl, Donald D. Blankenship
Figure caption: Actual vs. predicted median plots for the coherent content (left) and μ (right).
Paper: Investigating the Martian Surface at Decametric Scale: Population, Distribution, and Dimension of Heterogeneity from Radar Statistics
Authors: Cyril Grima, Nathaniel E. Putzig, Bruce A. Campbell, Matthew Perry, Sean P. S. Gulick, Russell C. Miller, Aaron T. Russell, Kirk M. Scanlan, Gregor Steinbrügge, Duncan A. Young, Scott D. Kempf, Gregory Ng, Dillon Buhl, Donald D. Blankenship
Figure caption: A set of various homodyned K-probability density functions.
Paper: Double Shadows at the Lunar Poles
Authors: Patrick O'Brien, Shane Byrne
Figure caption: Upper left: a location is doubly shadowed if every visible surface facet along every line of sight is permanently shadowed. Bottom: map with dots showing locations of double shadows identified at 30 m pxl−1 (larger than 5 contiguous pixels). Dashed circles indicate latitude intervals of 2.°5. Dot size is exaggerated but depicts relative area of each DPSR. Inset (upper right) shows resolved double shadows within Shoemaker crater (DPSR area not exaggerated here).
Paper: Double Shadows at the Lunar Poles
Authors: Patrick O'Brien, Shane Byrne
Figure caption: (a)–(c) Horizon method for identifying PSRs in LOLA topography, as described in Section 2.2. (d) Lunar PSRs at 30 m pxl−1 resolution, shown as red filled regions over hillshaded LOLA topography. Dashed circles indicate latitude intervals of 2.°5. The reader is referred to the following repository for full resolution shadow maps: O’Brien & Byrne (2022).
Paper: Double Shadows at the Lunar Poles
Authors: Patrick O'Brien, Shane Byrne
Figure caption: Size-frequency distribution of 30 m pxl−1 PSRs (a) and DPSRs (b) and 5 m pxl−1 DPSRs (c). Dashed lines show the resolution limit at 5 contiguous pixels.
Paper: Double Shadows at the Lunar Poles
Authors: Patrick O'Brien, Shane Byrne
Figure caption: Schematic of method to compute the elevation angle of distant topography (P 2) on a planetary body as seen from point P 1.
Paper: Numerical Simulations of Drainage Grooves in Response to Extensional Fracturing: Testing the Phobos Groove Formation Model
Authors: Bin Cheng, Erik Asphaug, Ronald-Louis Ballouz, Yang Yu, Hexi Baoyin
Figure caption: Tidal stresses driven by the orbital degradation of Phobos in two possible in situ formation scenarios: (a) single giant impact model; (b) moon-ring cycle model. The cohesive layer is assumed to have a rigidity of μ  o  = 108 Pa. Four internal models are adopted, with rigidity of μ  i  = 105, 106, 107, and 108 Pa (boxed labels on black lines). The horizontal shaded region shows the estimated material tensile strength, ∼1 kPa, required to generate parallel grooves. Based on the maximum failure criterion, the orbital history suggests that these grooves probably began forming 1.5–3.8 Ga or 60–90 Ma ago, respectively.
Paper: Numerical Simulations of Drainage Grooves in Response to Extensional Fracturing: Testing the Phobos Groove Formation Model
Authors: Bin Cheng, Erik Asphaug, Ronald-Louis Ballouz, Yang Yu, Hexi Baoyin
Figure caption: Simulated grooves mapped onto Phobos geomorphic mosaic. Rose diagrams show the orientation distributions of predicted grooves at corresponding locations. Some depressions on Phobos form distinct linear, parallel patterns perpendicular to the tensile direction, consistent with the expectations of the tidal fracturing model at midlatitudes. Three significant regions mainly along the equator that seem to contradict with our predictions are highlighted: within the intersecting zone (green), two crosscutting sets with disparate orientations coexist, in which one family is aligned with predicted grooves; near the sub-Mars region (blue), the tidal stresses are almost isotropically tensile and would generate polygonal fractures as predicted in Figure 4; around the trailing apex (yellow), a deficiency of grooves is observed. All data are from simulations for c  p  = 48 kPa.
Paper: Numerical Simulations of Drainage Grooves in Response to Extensional Fracturing: Testing the Phobos Groove Formation Model
Authors: Bin Cheng, Erik Asphaug, Ronald-Louis Ballouz, Yang Yu, Hexi Baoyin
Figure caption:  σ  θ θ  vs. σ  ϕ ϕ  for each RVE of the granular regolith during deformation. The results for different microcohesion values c  p  are shown in different colors as indicated in the legend. The envelopes (dashed lines) give estimations of the material tensile strength T according to the maximum failure criterion.