adsabs/AstroCLIMB huggingface dataset:
Paper: Uranus Orbiter and Probe: A Radio Science Investigation to Determine the Planet’s Gravity Field, Depth of the Winds, and Tidal Deformations
Authors: Marzia Parisi, A. James Friedson, Chris R. Mankovich, Mark D. Hofstadter, Alex B. Akins, Reza Karimi, Damon F. Landau
Figure caption: Longitudinal sections of Uranus’s wind models in m s−1 featuring (a) shallow and (b) deep winds, as a function of fractional radius.
Paper: Atmospheric Loss in Giant Impacts Depends on Preimpact Surface Conditions
Authors: Simon J. Lock, Sarah T. Stewart
Figure caption: The efficiency of loss is strongly influenced by the relative impedance of the atmosphere, ocean, and ground. Shown is a schematic that gives the relative position (left column) and the thermodynamic state (right) of the different material layers at different stages (rows) in the passage of the shock from the planet into the atmosphere. Left: colors indicate different materials, with rock in black and atmosphere in orange. In the left column, darker shades of these colors indicate material under compression in the shock. Boundaries between materials are shown as thin black lines with their velocities shown as black arrows. The shock wave is indicated by a thick white line. Release waves are shown as white dashed lines and their velocities as white arrows. Where relevant, key dynamic and thermodynamic variables are noted. Right: schematic particle velocity–pressure plots for the impedance-match calculation between rock and atmosphere. Key pressures and particle velocities corresponding to different stages of the thermodynamic evolution of material are given on the axis, as labeled in the left column. Solid lines are shock Hugoniots, the locus of points that a shocked material can reach from an initial starting position. Hugoniots are not thermodynamic paths and the point reached material on each Hugoniot is indicated by a filled symbol. Dashed lines are release curves followed by material decompressing from a shocked states. Release curves are thermodynamic paths and the material moves along these lines. As in the left column, colors indicate different materials. A similar schematic for a planet with an ocean is shown in Figure 3.
Paper: Atmospheric Loss in Giant Impacts Depends on Preimpact Surface Conditions
Authors: Simon J. Lock, Sarah T. Stewart
Figure caption: The presence of an ocean can strongly influence the efficiency of loss. Shown is a schematic that gives the relative position (left column) and the thermodynamic state (right) of the different material layers at different stages (rows) in the passage of the shock from the planet, through the ocean, and into the atmosphere. Left: different materials are indicated by different colors, with rock in black, water in blue, and atmosphere in orange. In the left column, darker shades of these colors indicate material under maximum compression in the shock. Boundaries between materials are shown as thin black lines with their velocities shown as black arrows. The shock wave is indicated by a thick white line. Release waves are shown as white dashed lines and their velocities as white arrows. Where key dynamic and thermodynamic variables apply are noted. Right: schematic particle velocity–pressure plots for the impedance-match calculation between rock, water, and atmosphere. Key pressures and particle velocities corresponding to different stages of the thermodynamic evolution of material are given on the axis, as labeled in the left column. Solid lines are shock Hugoniots, the locus of points that a shocked material can reach from an initial starting position. Hugoniots are not thermodynamic paths and the point reached material on each Hugoniot is indicated by a filled symbol. Dashed lines are release curves followed by material decompressing from a shocked states. Release curves are thermodynamic paths and the material moves along these lines. As in the left column, colors indicate different materials. A similar schematic for the case with no ocean is shown in Figure 2.
Paper: Atmospheric Loss in Giant Impacts Depends on Preimpact Surface Conditions
Authors: Simon J. Lock, Sarah T. Stewart
Figure caption: Atmospheric loss from giant impacts occurs through ejection in impact plumes or from ground motion further from the impact site. A: a schematic of a giant impact a few minutes before first contact, with different material layers indicated by different colors. B: the same collision a few minutes after initial contact. Melted and partially vaporized plumes are extruded from the impact site, carrying away a fraction of the atmosphere and ocean near the contact site. A shock wave (white line) propogates away from the impact site into the rest of the impactor and target. C: a schematic of a giant impact approximately 20 minutes after first contact. The shock wave travels through the planet and breaks out at the surface. The resulting acceleration of the ground drives a shock into the ocean and atmosphere, driving loss. D: a schematic of the 1D simulations performed for this study, which is similar to that used in previous work (Chen & Ahrens 1997; Genda & Abe 2003, 2005). A hydrostatic ocean and atmosphere are initialized at a radius equal to the planetary radius in a spherical geometry. The mantle and core of the planet are not modeled directly and the breakout of the shock from the planet is mimicked by giving the lower boundary of the domain an initial velocity, u G.
Paper: Inferring the CO2 Abundance in Comet 45P/Honda-Mrkos-Pajdušáková from [O I] Observations: Implications for the Source of Icy Grains in Cometary Comae
Authors: Mikayla R. Huffman, Adam J. McKay, Anita L. Cochran
Figure caption: Plot showing water active fraction vs. CO2 abundance. Each color is a different comet. Each marker shape within the colors is a different heliocentric distance or relation to perihelion. The solid black line is a line of best fit that was calculated via orthogonal distance regression. It has an equation of y = (0.66 ± 0.35)x+(−0.1 ± 3.59). The green dashed lines are 1σ  bounds on the best fit line. There is no significant correlation between active fraction and CO2 abundance for this sample of comets.
Paper: Inferring the CO2 Abundance in Comet 45P/Honda-Mrkos-Pajdušáková from [O I] Observations: Implications for the Source of Icy Grains in Cometary Comae
Authors: Mikayla R. Huffman, Adam J. McKay, Anita L. Cochran
Figure caption: Aperture size effects are minor, as shown in this plot of water active fraction vs. CO2 abundance. Each color is a different comet. Each marker shape within the colors is a different heliocentric distance or relation to perihelion. The solid orange line is a line of best fit that was calculated via orthogonal distance regression. It has an equation of y = (0.66 ± 0.35)x + (−0.1 ± 3.59). The orange dashed lines are 1σ bounds on the best-fit line. The red arrows indicate direction and relative magnitude of the shift in CO2 abundance after accounting for aperture size. The solid blue line is a line of best fit using the shifted points and was calculated using orthogonal distance regression. It has an equation of y = (0.65 ± 0.32)x + (1.73 ± 2.69). The blue dashed lines are 1σ bounds on the shifted best-fit line.
Paper: Inferring the CO2 Abundance in Comet 45P/Honda-Mrkos-Pajdušáková from [O I] Observations: Implications for the Source of Icy Grains in Cometary Comae
Authors: Mikayla R. Huffman, Adam J. McKay, Anita L. Cochran
Figure caption: Grotrian diagram for several forbidden oxygen lines. Roughly 90%–95% of emission occurs along the solid line pathway. The other 5%–10% of emission follows the dashed lines. The green solid line is the λ5577 line, the red doublet lines are the λλ6300 and 6364 lines, and the ultraviolet doublet lines (dashed lines) are the λλ2972 and 2958 lines. Adapted from Decock et al. (2013).
Paper: Inferring the CO2 Abundance in Comet 45P/Honda-Mrkos-Pajdušáková from [O I] Observations: Implications for the Source of Icy Grains in Cometary Comae
Authors: Mikayla R. Huffman, Adam J. McKay, Anita L. Cochran
Figure caption: Plots of the fitted Gaussian line profiles (blue lines) for the spectra obtained on UT February 21. The left column shows the cometary line (redward) and the telluric line (blueward). The right column is zoomed in on just the fitted cometary line. The first row is the λ5577 line, the second row is the λ6300 line, and the third row is the λ6364 line.
Paper: Inferring the CO2 Abundance in Comet 45P/Honda-Mrkos-Pajdušáková from [O I] Observations: Implications for the Source of Icy Grains in Cometary Comae
Authors: Mikayla R. Huffman, Adam J. McKay, Anita L. Cochran
Figure caption: Plot showing CO2 abundance vs. heliocentric distance for our sample of comets. Each color is a different comet. Each marker shape within the colors is a different heliocentric distance or relation to perihelion. There is no correlation between CO2 abundance and heliocentric distance for this sample of comets.
Paper: Inferring the CO2 Abundance in Comet 45P/Honda-Mrkos-Pajdušáková from [O I] Observations: Implications for the Source of Icy Grains in Cometary Comae
Authors: Mikayla R. Huffman, Adam J. McKay, Anita L. Cochran
Figure caption: Diagram showing the structure of the code we used to calculate the [O I] line ratio from input spectra. The [O I] line ratio is given by Equation (1), and the red line ratio is given by Equation (2).
Paper: Mini-RF S-band Radar Characterization of a Lunar South Pole–crossing Tycho Ray: Implications for Sampling Strategies
Authors: Edgard G. Rivera-Valentín, Caleb I. Fassett, Brett W. Denevi, Heather M. Meyer, Catherine D. Neish, Gareth A. Morgan, Joshua T. S. Cahill, Angela M. Stickle, G. Wesley Patterson
Figure caption: Controlled polar mosaic of Mini-RF S-band S 1 (i.e., total backscattered power) images in dB scale for areas poleward of 70°S. Color mapping is clipped from the scene median to 1.5× the interquartile range above the upper quartile (Q 3) such that black represents either areas with no data or areas below the median, shades of blue represent terrain with backscatter close to the scene median, and shades of yellow represent terrain near or above Q 3. Magenta arrows point out the location of the studied Tycho ray, and white arrows point out the location of a radar-bright ray from De Forest crater. Regions noted in the text are annotated as A, Newton crater; B, Weichert J crater; and C, De Forest crater. The Haworth candidate landing site is noted with a white square. Image resolution is 0.24 km pixel−1. East longitude is annotated for reference.
Paper: Mini-RF S-band Radar Characterization of a Lunar South Pole–crossing Tycho Ray: Implications for Sampling Strategies
Authors: Edgard G. Rivera-Valentín, Caleb I. Fassett, Brett W. Denevi, Heather M. Meyer, Catherine D. Neish, Gareth A. Morgan, Joshua T. S. Cahill, Angela M. Stickle, G. Wesley Patterson
Figure caption: Intensity of each m-χ decomposition component for (a) red, even bounce; (b) green, depolarized; and (c) blue, odd bounce scattering, as well as (d) CPR, as a function of distance from the center of the ray. Following Figure 4, the black line is the median, and the gray area represents the interquartile range. For comparison, the South Pole upper quartile (top dashed line), median (solid line), and lower quartile (bottom dashed line) values for the studied radar parameters are shown. The mosaic-wide quartile values follow the color coding for each m-χ component, with CPR represented by orange.
Paper: Mini-RF S-band Radar Characterization of a Lunar South Pole–crossing Tycho Ray: Implications for Sampling Strategies
Authors: Edgard G. Rivera-Valentín, Caleb I. Fassett, Brett W. Denevi, Heather M. Meyer, Catherine D. Neish, Gareth A. Morgan, Joshua T. S. Cahill, Angela M. Stickle, G. Wesley Patterson
Figure caption: Power as a function of distance from the ray center produced by collapsing the S 1 controlled polar mosaic between 254°E and 74°E and calculating the median (black line) and interquartile range (gray area) as a function of distance from the ray center. The shaded gray area between the quartiles represents the most likely values across the ray for that given distance from the center. For comparison, the mosaic-wide upper quartile (top dashed magenta line), median (solid magenta line), and lower quartile (bottom dashed magenta line) are shown.