adsabs/AstroCLIMB huggingface dataset:
Paper: Blue Marble, Stagnant Lid: Could Dynamic Topography Avert a Waterworld?
Authors: Claire Marie Guimond, John F. Rudge, and Oliver Shorttle
Figure caption: The competition between the ocean basin capacity and the surface water budget with increasing planet mass, expressed in terms of Earth ocean volumes. The three panels are based on, from left to right, the 1st percentile value, solar value, and 99th percentile value of expected mantle heat production across rocky exoplanets (Nimmo et al. 2020). Basin capacities as a function of planet mass are calculated from either the pure dynamic topography spectral model (dashed purple lines) or the red-noise model (dotted red lines). The empirical Venus model overlaps the pure dynamic topography and is not shown. Random rheological parameters propagate through the model; the resulting 1σ variation is represented by the swaths. In the background, the solid contours follow lines of constant surface water as a fraction of planet mass (note a modern Earth value of ∼200 ppm). Thermal histories refer to a 4.5 Gyr planet with a core mass fraction of 0.33.
Paper: Blue Marble, Stagnant Lid: Could Dynamic Topography Avert a Waterworld?
Authors: Claire Marie Guimond, John F. Rudge, and Oliver Shorttle
Figure caption: Various scalings for the maximum surface water capacity set by a planet’s peak elevation, expressed as a fraction of the total planet mass. The yellow lines show the peak topography balanced by crustal rock strength alone, which scales approximately with ﹩{M}_{p}^{-0.9};﹩ line widths correspond to different assumptions about the maximum strength with a fixed crust density of 2700 kg m−3. The thick green line shows pure dynamic topography with the coolest mantles considered, given a dry olivine rheology (﹩\propto {M}_{p}^{-0.8}﹩). The thin green line is the same for the hottest mantles (﹩\propto {M}_{p}^{-1.2}﹩). Scalings assume the mass–radius relation in Equation (7) and a red-noise-like topographic spectral structure. Points with error bars are estimates of the surface water inventories of planets e–g in the TRAPPIST-1 system from Agol et al. (2021), for different possible values of the core mass fraction (CMF). Note that their analysis suggests cores most likely smaller than the Earth-like CMF of 33%. Our thermal evolution model does not include tidal heating, which would push the TRAPPIST-1 planets toward higher mantle temperatures. For context, the labeled blue stars show the maximum ocean masses that could be contained on Venus, Earth, and Mars, plus Earth’s actual ocean mass.
Paper: Blue Marble, Stagnant Lid: Could Dynamic Topography Avert a Waterworld?
Authors: Claire Marie Guimond, John F. Rudge, and Oliver Shorttle
Figure caption: Top: dimensionless 1D power spectral densities of dynamic topography from 2D numerical convection simulations, normalized to an rms power of unity. In purple triangles is the model dynamic topography spectrum obtained from a loglinear fit to the Ra1 = 108, Δη = 107 case. Bottom: the model dynamic topography spectrum shown with the observed overall topography of Venus (yellow triangles; Wieczorek 2015) and a theoretical spectrum with a power-law dependence ∝k−2 (red circles), corresponding to red noise.
Paper: Blue Marble, Stagnant Lid: Could Dynamic Topography Avert a Waterworld?
Authors: Claire Marie Guimond, John F. Rudge, and Oliver Shorttle
Figure caption: A synthetic topography map, obtained from a random power spectrum (﹩{l}_{\max }=53﹩) consistent with the numerically modeled “baseline” dynamic topography spectrum (see text for details on randomization). This map has a peak elevation of 820 m and an rms elevation of 190 m. The nominal planet has a mass of 1 M⊕, dry olivine rheology, and a solar radiogenic heating budget.
Paper: Orientale Ejecta at the Apollo 14 Landing Site Implies a 200-million-year Stratigraphic Time Shift on the Moon
Authors: Stephanie C. Werner, Benjamin Bultel, Tobias Rolf, and Vera Assis Fernandes
Figure caption: Spectral analysis of the Apollo 14 landing site using M3 data. (a) Map depicting the results of the spectral data analysis based on the combination of three spectral criteria (see Table 1) into a color scheme of red-green-blue (R: BD930; G: BD1250; B: BD1900). The defining characteristics of the Landing-Site Unit show up in green in the spectral criteria map for the surfaces rich in low-calcium pyroxene and feldspar (typical highland rocks) and in purple for surfaces corresponding to material with pyroxene poorer in calcium and lack of a feldspar signature. We outlined the morphologically and spectrally defined unit in white for crater statistics. (b) Map showing the combined spectral criteria that evaluates the variations of the absorption near 2000 nm (R: BD1900; G: BD2020; B: BD2300). (c) Map of the relative feldspar abundance based on the absorption band at 1250 nm. (d, e, f, g) Zoom-in to Cone crater and the astronaut track (cyan line) as outlined in panel (a) (white rectangle in panel (a)). The zoom-in for panel (a) is shown in panel (d), for panel (b) in panel (e), for panel (c) in panel (f), and in panel (g) the panchromatic image data. Panel (d) shows the clear relationship between the ejecta Cone crater and spectral features (purple). The astronauts’ track touches the rim of Cone crater in the center of the map.
Paper: Orientale Ejecta at the Apollo 14 Landing Site Implies a 200-million-year Stratigraphic Time Shift on the Moon
Authors: Stephanie C. Werner, Benjamin Bultel, Tobias Rolf, and Vera Assis Fernandes
Figure caption: Comparison of laboratory sample and M3 remote-sensing spectra. The two M3 remote-sensing spectra represent the spectral features of the Landing-Site Unit (green) and the Cone crater ejecta blanket (purple). Sample spectra are plotted according to the collection sites, either in green when they were picked in the Landing-Site Unit on top of the plot or in purple when the collections sites are located on the Cone crater ejecta blanket at the bottom of the plot. Black short vertical lines indicate centers of absorptions. Dotted lines indicate centers of main absorptions seen on the spectral units at the Apollo 14 landing site.
Paper: Orientale Ejecta at the Apollo 14 Landing Site Implies a 200-million-year Stratigraphic Time Shift on the Moon
Authors: Stephanie C. Werner, Benjamin Bultel, Tobias Rolf, and Vera Assis Fernandes
Figure caption: Crater statistics for the Apollo 14 landing site. (a) Image of the landing site area including the outline of the Landing-Site Unit according to the combined spectral and morphological data (white line); the white dot marks the landing site; craters are marked as red circles according to their diameters. North is up. (b) Crater size–frequency distributions (CFSD) for the craters observed in panel (a) and previous measurements (Neukum et al. 1975; Robbins 2014) for comparison; error bars show standard deviation. (c) The CFSD analysis: craters (magenta) measure the exposure of the original surface and date the Imbrium ejecta emplacement; craters (green) formed in the Orientale ejecta blanket and date its emplacement; craters (gray) may be in saturation equilibrium (Gault 1970) and are not used for dating. Gray curves indicate best-fit crater-production functions for the green and magenta colored sections or the crater-saturation equilibrium curve, respectively. (d) The CSFD in a differential instead of the cumulative histogram; colored bars mark the crater size range defining the fit ranges for age determination, and dashed lines mark the kinks. (e) The CSFD as the so-called relative crater frequency (with respect to a simple power law) and three levels of geometric saturation (1%, standard: ∼5%, 10%) after Gault (1970).
Paper: Orientale Ejecta at the Apollo 14 Landing Site Implies a 200-million-year Stratigraphic Time Shift on the Moon
Authors: Stephanie C. Werner, Benjamin Bultel, Tobias Rolf, and Vera Assis Fernandes
Figure caption: Crater statistics for the Apollo 14 landing site in comparison to Imbrium and Orientale. Crater size–frequency distributions (CFSD) for the craters observed in the Landing-Site Unit are as shown in Figure 3, and those of Imbrium basin and Orientale basin are as derived by Fassett et al. (2012); error bars show standard deviation. Using isochrones representing the crater frequencies observed at the Apollo 14 site of the surviving and resurfacing crater populations, we can show that the latter is very well in agreement with the measurement by Fassett et al. (2012) for Orientale, and the surviving population also matches the Imbrium relative age.
Paper: Orientale Ejecta at the Apollo 14 Landing Site Implies a 200-million-year Stratigraphic Time Shift on the Moon
Authors: Stephanie C. Werner, Benjamin Bultel, Tobias Rolf, and Vera Assis Fernandes
Figure caption: Nearside map of the Moon showing the thorium (Th) content. The Apollo 14 landing site features high values of Th. Peak values correlate with impact sites of young craters (shown by their names in the map) with extensive rayed ejecta patterns in the crater diameter range of 5–20 km. No high thorium content correlates with the impact sites of Copernicus or Tycho craters, both prominent rayed impact structures on the lunar nearside. Elevated Th abundance is observable within the entire region of Oceanus Procellarum and most mare units in its vicinity. The light-gray dashed line marks the suggested edge of the Imbrium basin.
Paper: Compositional Maps of the Lunar Polar Regions Derived from the Kaguya Spectral Profiler and the Lunar Orbiter Laser Altimeter Data
Authors: Myriam Lemelin, Paul G. Lucey, and Alex Camon
Figure caption: Reflectance calculated for a high-signal north polar point (85.716724°N, 112.59965°W) in orbit 294. Top: data from all three SP detectors (VIS, NIR1, and NIR2). Bottom: data extracted for this study (VIS and NIR1).
Paper: Compositional Maps of the Lunar Polar Regions Derived from the Kaguya Spectral Profiler and the Lunar Orbiter Laser Altimeter Data
Authors: Myriam Lemelin, Paul G. Lucey, and Alex Camon
Figure caption: Different gridded data products for Schrödinger crater. (a) Gridded Spectral Profiler 1064 nm reflectance data showing the location and spatial density of spectral measurements. (b) Interpolated data. (c) Spectral Profiler 1064 nm reflectance data scaled to the LOLA 1064 nm reflectance data. (d) Interpolated data. Variations in reflectance due to topography are removed.
Paper: Compositional Maps of the Lunar Polar Regions Derived from the Kaguya Spectral Profiler and the Lunar Orbiter Laser Altimeter Data
Authors: Myriam Lemelin, Paul G. Lucey, and Alex Camon
Figure caption: Calibrated Spectral Profiler 1064 nm reflectance and 955.4/752.8 nm reflectance ratio for both polar regions. Low Spectral Profiler ratios are mostly associated with less optically mature surfaces and surfaces containing higher iron abundances. High 1064 nm reflectance is mostly associated with surfaces containing low iron abundances and less optically mature surfaces.
Paper: Compositional Maps of the Lunar Polar Regions Derived from the Kaguya Spectral Profiler and the Lunar Orbiter Laser Altimeter Data
Authors: Myriam Lemelin, Paul G. Lucey, and Alex Camon
Figure caption: Derivation of the polar FeO algorithm using Spectral Profiler and Lunar Prospector gridded data between 50° and 90°N/S at a spatial resolution of 15 km pixel–1.
Paper: Compositional Maps of the Lunar Polar Regions Derived from the Kaguya Spectral Profiler and the Lunar Orbiter Laser Altimeter Data
Authors: Myriam Lemelin, Paul G. Lucey, and Alex Camon
Figure caption: Error in mineral abundance between our model and the mineral abundances measured by the LSCC. The model uses the refined optical constants of Lucey (1998) to minimize the difference in mineral abundances between our model and the LSCC data. The comparison uses Spectral Profiler wavelengths between 746.8 and 1555.5 nm. Olivine is shown in green, low-calcium pyroxene in blue, high-calcium pyroxene in red, and plagioclase in black. The correlation (r) between the two data sets is 93%, and the rms error in mineral abundance estimation is 9 wt.%.
Paper: Compositional Maps of the Lunar Polar Regions Derived from the Kaguya Spectral Profiler and the Lunar Orbiter Laser Altimeter Data
Authors: Myriam Lemelin, Paul G. Lucey, and Alex Camon
Figure caption: North and south polar maps of FeO abundance. Top: calibrated Spectral Profiler data at 1 km pixel–1, Bottom: Lunar Prospector data at 15 km pixel–1. The data are shown in polar stereographic projection between 50°–90°N (left) and 50°–90°S (right) in latitude with 20% transparency over the Wide Angle Camera global mosaic.
Paper: Compositional Maps of the Lunar Polar Regions Derived from the Kaguya Spectral Profiler and the Lunar Orbiter Laser Altimeter Data
Authors: Myriam Lemelin, Paul G. Lucey, and Alex Camon
Figure caption: Average FeO by latitude for Lunar Prospector and Spectral Profiler data at 15 km pixel–1. The error bars represent plus or minus one standard deviation from the Spectral Profiler FeO abundances.
Paper: Compositional Maps of the Lunar Polar Regions Derived from the Kaguya Spectral Profiler and the Lunar Orbiter Laser Altimeter Data
Authors: Myriam Lemelin, Paul G. Lucey, and Alex Camon
Figure caption: North and south polar maps of OMAT. The data are shown in polar stereographic projection between 50°–90°N (left) and 50°–90°S (right) in latitude.
Paper: Compositional Maps of the Lunar Polar Regions Derived from the Kaguya Spectral Profiler and the Lunar Orbiter Laser Altimeter Data
Authors: Myriam Lemelin, Paul G. Lucey, and Alex Camon
Figure caption: North and south polar maps of plagioclase and olivine abundances. The data are shown in polar stereographic projection between 50°–90°N (left) and 50°–90°S (right) in latitude with transparency over the Wide Angle Camera global mosaic.
Paper: Compositional Maps of the Lunar Polar Regions Derived from the Kaguya Spectral Profiler and the Lunar Orbiter Laser Altimeter Data
Authors: Myriam Lemelin, Paul G. Lucey, and Alex Camon
Figure caption: North and south polar maps of low- and high-calcium pyroxene abundances. The data are shown in polar stereographic projection between 50°–90°N (left) and 50°–90°S (right) in latitude with transparency over the Wide Angle Camera global mosaic.
Paper: Compositional Maps of the Lunar Polar Regions Derived from the Kaguya Spectral Profiler and the Lunar Orbiter Laser Altimeter Data
Authors: Myriam Lemelin, Paul G. Lucey, and Alex Camon
Figure caption: North and south polar maps of nanophase iron abundance. The data are shown in polar stereographic projection between 50°–90°N (left) and 50°–90°S (right) in latitude.
Paper: Compositional Maps of the Lunar Polar Regions Derived from the Kaguya Spectral Profiler and the Lunar Orbiter Laser Altimeter Data
Authors: Myriam Lemelin, Paul G. Lucey, and Alex Camon
Figure caption: North and south polar maps of the correlation coefficient between the modeled and observed spectra. The data are shown in polar stereographic projection between 50°–90°N (left) and 50°–90°S (right) in latitude with transparency over the Wide Angle Camera global mosaic.
Paper: Compositional Maps of the Lunar Polar Regions Derived from the Kaguya Spectral Profiler and the Lunar Orbiter Laser Altimeter Data
Authors: Myriam Lemelin, Paul G. Lucey, and Alex Camon
Figure caption: Average OMAT value by latitude for each polar region. The OMAT values analyzed are constrained to sunlit and nearly flat surfaces with slopes shallower than 5°. In both polar regions, the OMAT values display a steady increase poleward of ∼60°, reaching a high of ∼0.5 near both poles.
Paper: Compositional Maps of the Lunar Polar Regions Derived from the Kaguya Spectral Profiler and the Lunar Orbiter Laser Altimeter Data
Authors: Myriam Lemelin, Paul G. Lucey, and Alex Camon
Figure caption: Average abundance of nanophase iron (NPFe) by latitude for each polar region. The nanophase iron values analyzed are constrained to sunlit, nearly flat surfaces (slopes shallower than 5°) and surfaces with FeO content lower than 10 wt.%. In both polar regions, nanophase iron abundances display a steady decrease poleward of ∼60°–70°, reaching a low of ∼0.2 wt.% near both poles. Nanophase iron is approximately three times less abundant at the poles than in the equatorial region (50°).
Paper: Compositional Maps of the Lunar Polar Regions Derived from the Kaguya Spectral Profiler and the Lunar Orbiter Laser Altimeter Data
Authors: Myriam Lemelin, Paul G. Lucey, and Alex Camon
Figure caption: Iron and plagioclase content of the Artemis region (84°–90°S). Black polygons represent permanently shaded regions from Mazarico et al. (2011), while gray polygons represent the 11 water ice–bearing permanently shaded regions identified by Lemelin et al. (2021) as high-priority exploration sites. The six potential Artemis sites identified by NASA (2020) are shown as white circles.
Paper: Compositional Maps of the Lunar Polar Regions Derived from the Kaguya Spectral Profiler and the Lunar Orbiter Laser Altimeter Data
Authors: Myriam Lemelin, Paul G. Lucey, and Alex Camon
Figure caption: Optical OMAT of the south polar and Artemis regions (84°–90°S). Bright OMAT rays extend from Tycho and De Forest craters into the Artemis region. OMAT values between 30° and 50°S are derived from the Kaguya Multiband Imager data (Lemelin et al. 2019), and OMAT values between 50° and 90°S are derived from the Kaguya Spectral Profiler data herein.
Paper: Kronoseismology. VI. Reading the Recent History of Saturn’s Gravity Field in Its Rings
Authors: M.M. Hedman, P.D. Nicholson, M. El Moutamid, and S. Smotherman
Figure caption: Comparisons of three high-quality normal optical depth (τn) profiles obtained from three different times during the Cassini mission (the year and day numbers are provided in the colored labels), focusing on the waves designated W84.82 and W84.86. In this case, the wavelengths of the wave patterns around 84,825 and 84,865 km clearly shorten over the course of the Cassini mission. The wave packet around 84,825 km also steadily moves outward over time.
Paper: Kronoseismology. VI. Reading the Recent History of Saturn’s Gravity Field in Its Rings
Authors: M.M. Hedman, P.D. Nicholson, M. El Moutamid, and S. Smotherman
Figure caption: Comparisons of three high-quality normal optical depth (τn) profiles obtained from three different times during the Cassini mission (the year and day numbers are provided in the colored labels), focusing on the wave designated W86.40. The wavelength of this pattern around 86,410 km clearly shortens over the course of the Cassini mission. Furthermore, the wave appears to be shifting inward over time, with the region of the highest-amplitude variations shifting from about 86,420 km to around 86,405 km during this 8 yr period.
Paper: Kronoseismology. VI. Reading the Recent History of Saturn’s Gravity Field in Its Rings
Authors: M.M. Hedman, P.D. Nicholson, M. El Moutamid, and S. Smotherman
Figure caption: Comparisons of three high-quality normal optical depth (τn) profiles obtained from three different times during the Cassini mission (the year and day numbers are provided in the colored labels), focusing on the wave designated W85.67. The wavelength of this pattern around 85,670 km clearly shortens over the course of the Cassini mission. Furthermore, the wave appears to be shifting inward over time, with the leftmost part of the wave being much closer to the plateau edge at 85,660 km by the end of the Cassini Mission.
Paper: Kronoseismology. VI. Reading the Recent History of Saturn’s Gravity Field in Its Rings
Authors: M.M. Hedman, P.D. Nicholson, M. El Moutamid, and S. Smotherman
Figure caption: The results of a wavelet analysis of a density wave driven by a planetary normal mode. The top panel shows the normal optical depth (τn) profile of the density wave W84.64 from the Rev 106 RCas occultation. The bottom panel shows the peak value of the wavelet power ratio ﹩{ \mathcal R }﹩ for wavelengths between 0.2 and 2 km for the observations from Epoch 1 as functions of radius and pattern speed. The latter is expressed in terms of offsets in both the assumed pattern speed δΩp and resonant radius δr from the nominal values given at the top of the plot. In this case, the entire wave has the same pattern speed, and so the peak signals at all radii fall along a horizontal line. This is a characteristic found in most waves generated by satellites or planetary normal modes.
Paper: Kronoseismology. VI. Reading the Recent History of Saturn’s Gravity Field in Its Rings
Authors: M.M. Hedman, P.D. Nicholson, M. El Moutamid, and S. Smotherman
Figure caption: The results of a wavelet analysis of the waves W84.82 and W84.86, showing the same optical depth profile and peak ﹩{ \mathcal R }﹩ data computed in the same way as Figure 4. In this case, not only do the two waves have different pattern speeds, but each wave also shows variations in its pattern speed with radius. These trends are parallel to the diagonal dotted line, which corresponds to the local pattern speed of a wave at that location. Note also that additional wavelet signals are found along this line interior to W84.82, which likely correspond to additional wave fragments not obvious in the profile.
Paper: Kronoseismology. VI. Reading the Recent History of Saturn’s Gravity Field in Its Rings
Authors: M.M. Hedman, P.D. Nicholson, M. El Moutamid, and S. Smotherman
Figure caption: The results of a wavelet analysis of the wave W86.40, showing the same optical depth profile and peak ﹩{ \mathcal R }﹩ data computed in the same way as Figure 4. There are clear variations in the wave’s pattern speed with radius that follow a trend similar to the diagonal dotted line that corresponds to the expected local pattern speed. In this case, the peak signals appear to occur at pattern speeds that correspond to a location 10–20 km interior to the observed location.
Paper: Kronoseismology. VI. Reading the Recent History of Saturn’s Gravity Field in Its Rings
Authors: M.M. Hedman, P.D. Nicholson, M. El Moutamid, and S. Smotherman
Figure caption: The results of a wavelet analysis of the wave W85.67, showing the same optical depth profile and peak ﹩{ \mathcal R }﹩ data computed in the same way as Figure 4. There are clear variations in the wave’s pattern speed with radius that follow a trend similar to the diagonal dotted line that corresponds to the expected local pattern speed. In this case the peak signals appear to occur at pattern speeds that correspond to a location 10–20 km exterior to the observed location.
Paper: Kronoseismology. VI. Reading the Recent History of Saturn’s Gravity Field in Its Rings
Authors: M.M. Hedman, P.D. Nicholson, M. El Moutamid, and S. Smotherman
Figure caption: The results of a wavelet analysis of the region around 86,570 km, including the W86.58 and W86.59 waves, showing the same optical depth profile and peak ﹩{ \mathcal R }﹩ data computed in the same way as Figure 4. This region shows signals with a range of pattern speeds, only two of which were previously identified as wave-like.
Paper: Kronoseismology. VI. Reading the Recent History of Saturn’s Gravity Field in Its Rings
Authors: M.M. Hedman, P.D. Nicholson, M. El Moutamid, and S. Smotherman
Figure caption: The results of a wavelet analysis of the region around 85,950 km, showing the same optical depth profile and peak ﹩{ \mathcal R }﹩ data computed in the same way as Figure 4. Although there is not an obvious wave in the profile, m = 3 signals are visible throughout this region with a range of pattern speeds.
Paper: Kronoseismology. VI. Reading the Recent History of Saturn’s Gravity Field in Its Rings
Authors: M.M. Hedman, P.D. Nicholson, M. El Moutamid, and S. Smotherman
Figure caption: An overview of all of the m = 3 patterns in the middle C ring. The top panel shows the normal optical depth profile, while the bottom panel shows the peak value of the wavelet power ratio ﹩{ \mathcal R }﹩ for wavelengths between 0.2 and 2 km for the observations from Epoch 1 as functions of radius and the difference from the expected local pattern speed at each radius.