adsabs/AstroCLIMB huggingface dataset:
Paper: Mercury’s Hidden Past: Revealing a Volatile-dominated Layer through Glacier-like Features and Chaotic Terrains
Authors: J. Alexis P. Rodriguez, Deborah Domingue, Bryan Travis, Jeffrey S. Kargel, Oleg Abramov, Mario Zarroca, Maria E. Banks, John Weirich, Anthony Lopez, Nicholas Castle, Yan Jianguo, Frank Chuang
Figure caption: Presents plots illustrating the anomalous behavior of liquid sulfur’s viscosity as a function of temperature, which initially decreases, then increases, and subsequently decreases again, as shown by Sofekun et al. (2018). Panel (A) provides a focused view of the viscosity within the temperature range of 115 °C–160 °C. Panel (B) juxtaposes experimental Newtonian viscosity data and semiempirical models for molten sulfur. The significant increase in viscosity, peaking around 190 °C, is attributed to the process of polymerization that predominantly occurs at approximately 160 °C. Sulfur in the S8 form demonstrates highly fluid characteristics for temperatures below 160 °C and above approximately 300 °C, as reported by Sofekun et al. (2018).
Paper: Mercury’s Hidden Past: Revealing a Volatile-dominated Layer through Glacier-like Features and Chaotic Terrains
Authors: J. Alexis P. Rodriguez, Deborah Domingue, Bryan Travis, Jeffrey S. Kargel, Oleg Abramov, Mario Zarroca, Maria E. Banks, John Weirich, Anthony Lopez, Nicholas Castle, Yan Jianguo, Frank Chuang
Figure caption: (A) MESSENGER MDIS Image N1045992946M showcasing the DTM location centered at coordinates 27.°944 Lat, 120.°277 E Lon. (B) A hillshade interpretation of the DTM, exclusively providing elevation details. (C) DTM visualization conducted under the same incidence and emission angle as the spacecraft image, revealing both height and albedo aspects. Each panel within the figure spans an area of 17 km across.
Paper: Mercury’s Hidden Past: Revealing a Volatile-dominated Layer through Glacier-like Features and Chaotic Terrains
Authors: J. Alexis P. Rodriguez, Deborah Domingue, Bryan Travis, Jeffrey S. Kargel, Oleg Abramov, Mario Zarroca, Maria E. Banks, John Weirich, Anthony Lopez, Nicholas Castle, Yan Jianguo, Frank Chuang
Figure caption: (A) MESSENGER MDIS Image N1015454462M showcasing the DTM location centered at coordinates 28.°340 Lat, 120.°283 E Lon. (B) A DTM rendering using shaded relief or hillshade, providing elevation information. (C) DTM rendering under the identical incidence and emission angle as the spacecraft image, delivering both elevation and albedo data. All panels in the figure span an area of 17 km across.
Paper: Mercury’s Hidden Past: Revealing a Volatile-dominated Layer through Glacier-like Features and Chaotic Terrains
Authors: J. Alexis P. Rodriguez, Deborah Domingue, Bryan Travis, Jeffrey S. Kargel, Oleg Abramov, Mario Zarroca, Maria E. Banks, John Weirich, Anthony Lopez, Nicholas Castle, Yan Jianguo, Frank Chuang
Figure caption: (A) MESSENGER MDIS Image N1046021896M illustrating the DTM location centered at coordinates 27.°620 Lat, 120.°442 E Lon. (B) A hillshade rendition of the DTM, solely presenting elevation data. (C) A DTM rendition that matches the incidence and emission angle of the spacecraft image, thereby offering both elevation and albedo details. Each panel within this figure extends over a span of 17 km.
Paper: Astrobiology eXploration at Enceladus (AXE): A New Frontiers Mission Concept Study
Authors: K. Marshall Seaton, Szilárd Gyalay, Gaia Stucky de Quay, Ethan R. Burnett, C. Adeene Denton, Bryce Doerr, Kamak Ebadi, Stephanie Eckert, Ian. T. W. Flynn, Casey I. Honniball, Shayna Hume, Corbin L. Kling, Julian C. Marohnic, Julia Milton, Claire A. Mondro, Raquel G. Nuno, Caoimhe M. Rooney, Beck E. Strauss, Alfred Nash, Jennifer E. C. Scully
Figure caption: Schematic overview of science closure for crater morphology mapping (Objective 4). The top row summarizes Task 1, which utilizes crater depth and diameter to characterize crater shallowing as a function of space to identify potential paleo plume sources (a) and (b). The bottom row summarizes Task 2, which uses elliptical crater orientation to quantify potential ice shell reorientation (c) and (d). (a) Schematic diagram of Enceladus and key geometries for Task 1. Dashed lines are the swath from the north polar to the SPT. This hypothetical swath intersects a potential paleo plume source (black square). Blue circles symbolize mapped craters. (b) Hypothesized relationship between depth/diameter ratio (d/D) along a latitudinal swath from the north pole to the SPT, with each individual crater plotted as a blue data point (see panel (a)). If craters become shallower (decrease in d/D) only with increasing proximity to the SPT (light gray fitted line), this suggests the present-day SPT was the main source of plume deposit fallout for the duration of its geologic record. However, if there is a crater shallowing signal that points to another source location (dip in black fitted line), this would suggest there was another source of deposit fallout (a paleo plume). (c) Schematic diagram of Enceladus with elliptical crater populations (blue circles), which are likely to have major axis orientations (ø) aligned to its east–west orbit (see the text for an in-depth explanation). The present-day north pole is shown, in addition to a potential paleo north pole at a slight angle. (d) Rose diagram depicting the orientations of mapped elliptical craters (i.e., binned frequency distribution of orientations). If there is only a strong east–west contribution (gray-outlined bins), this would suggest the present-day ice shell and north pole configuration have been in place for the duration of its geologic record. If there is another significant contribution at a different orientation (black-outlined bin), this would suggest reorientation of the ice shell, as measured by the elliptical crater population alignment.
Paper: Astrobiology eXploration at Enceladus (AXE): A New Frontiers Mission Concept Study
Authors: K. Marshall Seaton, Szilárd Gyalay, Gaia Stucky de Quay, Ethan R. Burnett, C. Adeene Denton, Bryce Doerr, Kamak Ebadi, Stephanie Eckert, Ian. T. W. Flynn, Casey I. Honniball, Shayna Hume, Corbin L. Kling, Julian C. Marohnic, Julia Milton, Claire A. Mondro, Raquel G. Nuno, Caoimhe M. Rooney, Beck E. Strauss, Alfred Nash, Jennifer E. C. Scully
Figure caption: Schematic representation of how gravity is extrapolated from the Doppler shift of a transmitted radio tone. The AXE spacecraft would emit a radio signal, and its frequency would change depending on whether the spacecraft is accelerating or decelerating relative to Earth. If the spacecraft is traveling away from Earth, an accelerating spacecraft will decrease its radio frequency while a decelerating spacecraft will increase its radio frequency. If the spacecraft is traveling toward Earth, an accelerating spacecraft will increase its radio frequency while a decelerating spacecraft will decrease its radio frequency. Because the frequency of the original radio tone is known, the Doppler shift in this tone can be used to calculate the change in velocity resulting from changing acceleration due to gravity from Enceladus. We note that the recorded changes in acceleration would only be the component pointed toward Earth. Because our mission requires gravity data from every flyby and adequate illumination for photography ∼6000 km to or from Enceladus (see our science mission profile in Section 5.1), the line of sight to Earth is approximately parallel to the flyby path. Knowledge of the angle between Enceladus’ center of mass and the flyby path with respect to the AXE spacecraft could then be used to calculate the change in gravity as a whole, which can be corrected for distance to the center of Enceladus to obtain the distribution of gravity across the surface (pictured). At large length scales (low spherical harmonic degree), topographic highs are compensated for by thickening of the ice shell. Because the average ice shell thickness is finite, a thicker ice shell results in a higher detected gravity despite isostatic compensation. Gravity and topography are most correlated at the shortest wavelengths, where gravity is entirely due to uncompensated topography. The wavelengths over which this correlation changes can be used to calculate the average ice shell thickness. Whether the shell is compensated at a given wavelength is also affected by the ice shell’s rheology and thus would need to be taken into account (Akiba et al. 2022).
Paper: Astrobiology eXploration at Enceladus (AXE): A New Frontiers Mission Concept Study
Authors: K. Marshall Seaton, Szilárd Gyalay, Gaia Stucky de Quay, Ethan R. Burnett, C. Adeene Denton, Bryce Doerr, Kamak Ebadi, Stephanie Eckert, Ian. T. W. Flynn, Casey I. Honniball, Shayna Hume, Corbin L. Kling, Julian C. Marohnic, Julia Milton, Claire A. Mondro, Raquel G. Nuno, Caoimhe M. Rooney, Beck E. Strauss, Alfred Nash, Jennifer E. C. Scully
Figure caption: Range of expected (a) amino acid and (b) short-chain fatty acid concentrations in the bulk Enceladus ocean using an expected core aqueous processing depth range of 4–70 km.
Paper: Astrobiology eXploration at Enceladus (AXE): A New Frontiers Mission Concept Study
Authors: K. Marshall Seaton, Szilárd Gyalay, Gaia Stucky de Quay, Ethan R. Burnett, C. Adeene Denton, Bryce Doerr, Kamak Ebadi, Stephanie Eckert, Ian. T. W. Flynn, Casey I. Honniball, Shayna Hume, Corbin L. Kling, Julian C. Marohnic, Julia Milton, Claire A. Mondro, Raquel G. Nuno, Caoimhe M. Rooney, Beck E. Strauss, Alfred Nash, Jennifer E. C. Scully
Figure caption: AXE interplanetary cruise and flyby trajectories, including associated deep space maneuvers (DSM) and C3, decl. (Dec.), altitude (Alt.), and Δv required for each phase of the mission, as well as the corresponding velocity of the spacecraft during each phase (V∞ ). (a) Gravity assists from Earth, Venus, and Jupiter would be utilized during the interplanetary cruise phase to reach the Saturn system. (b), (c) Pump-down and DSMs required to tailor spacecraft trajectories such that Enceladus can be targeted with the appropriate inclination, altitude, and velocity for science operations.
Paper: Astrobiology eXploration at Enceladus (AXE): A New Frontiers Mission Concept Study
Authors: K. Marshall Seaton, Szilárd Gyalay, Gaia Stucky de Quay, Ethan R. Burnett, C. Adeene Denton, Bryce Doerr, Kamak Ebadi, Stephanie Eckert, Ian. T. W. Flynn, Casey I. Honniball, Shayna Hume, Corbin L. Kling, Julian C. Marohnic, Julia Milton, Claire A. Mondro, Raquel G. Nuno, Caoimhe M. Rooney, Beck E. Strauss, Alfred Nash, Jennifer E. C. Scully
Figure caption: Enceladus plume eruption mechanisms in response to tidal forcing. In an open-crevasse scenario (a), tidal forcing throughout the orbital phase of Enceladus is expected to result in vent width variations (c) that are consistent along the strike of the vent. For a purely cryovolcanic scenario involving point-source eruptions (b), these vent width variations are expected to be localized to the immediate vicinity of the vent.
Paper: Astrobiology eXploration at Enceladus (AXE): A New Frontiers Mission Concept Study
Authors: K. Marshall Seaton, Szilárd Gyalay, Gaia Stucky de Quay, Ethan R. Burnett, C. Adeene Denton, Bryce Doerr, Kamak Ebadi, Stephanie Eckert, Ian. T. W. Flynn, Casey I. Honniball, Shayna Hume, Corbin L. Kling, Julian C. Marohnic, Julia Milton, Claire A. Mondro, Raquel G. Nuno, Caoimhe M. Rooney, Beck E. Strauss, Alfred Nash, Jennifer E. C. Scully
Figure caption: Schematic representation and description of AXE science operations at Enceladus.
Paper: Col-OSSOS: The Distribution of Surface Classes in Neptune's Resonances
Authors: Rosemary E. Pike, Wesley C. Fraser, Kathryn Volk, J. J. Kavelaars, Michaël Marsset, Nuno Peixinho, Megan E. Schwamb, Michele T. Bannister, Lowell Peltier, Laura E. Buchanan, Susan Benecchi, Nicole J. Tan
Figure caption: The results are presented for the apparent parent populations for the different resonant populations. The different resonances are indicated along the x-axis. The parent populations are a combination of the DE TNOs and CC TNOs, with different percentages of each of the two groups, from 0%–100% calculated in steps of 5%. The distance between the distribution of resonant PC﹩{}_{{grJ}}^{2}﹩ values and parent population PC﹩{}_{{grJ}}^{2}﹩ values is computed with the A-D test, then the significance of that result is obtained by bootstrapping using the input parent population. The large diamonds indicate the least rejectable D-statistic parent population fraction, the small diamonds indicate the 2σ limits, and the smallest (closed) diamonds indicate the 3σ limits based on the D-statistic. The width of each bar is proportional to the D-statistic value at each 5% step. The three different bars for each resonance show the results for slightly different assumptions in the parent populations. The green (left) bar uses the DE and CC populations exactly as defined in Table 1. The teal (middle) bar uses the CC objects as defined in Table 1, but for the DE objects uses only the DE objects with pericenter q > 22. The purple (right) bar uses the CC and DE objects as classified in Table 1 except that the five cold classicals with PC2  grJ  > −0.13 BrightIR surfaces are moved from the CC group to the DE group, as having five low-i objects is consistent with being the low-i tail of the DE inclination distribution; see Section 3.1 for details. Note that the parent population used here is to reproduce the apparent surface distribution and not the intrinsic population ratios of the dynamically excited and cold classical objects, due to detection biases and albedo differences (see the main text for details).
Paper: Col-OSSOS: The Distribution of Surface Classes in Neptune's Resonances
Authors: Rosemary E. Pike, Wesley C. Fraser, Kathryn Volk, J. J. Kavelaars, Michaël Marsset, Nuno Peixinho, Megan E. Schwamb, Michele T. Bannister, Lowell Peltier, Laura E. Buchanan, Susan Benecchi, Nicole J. Tan
Figure caption: Left: the cumulative fraction of PC﹩{}_{{grJ}}^{1}﹩ values. The nonresonant dynamically excited objects (black ‘x’s), dynamically cold classical objects (pink squares), 4:3 resonators (orange triangles), 3:2 resonators (yellow squares), resonant objects within the classical region (green wide ‘x’s), 2:1 resonators (cyan diamonds), and resonant objects with semimajor axes a > 49 au (blue hexagons) are all shown separately. Right: the cumulative fraction of Col-OSSOS targets by PC﹩{}_{{grJ}}^{2}﹩ values, in the same color scheme as the left plot. The gray dashed line indicates the divide between the FaintIR (left) and BrightIR (right) surface classifications at PC﹩{}_{{grJ}}^{2}=-0.13﹩. The cold classical TNOs are dominated by the FaintIR surface classification, but this surface classification is also found in the resonances, including the 4:3 resonance, which is sunward of the current cold classical belt. The nonresonant dynamically excited objects are dominated by the BrightIR surface classification, and their distribution of PC﹩{}_{{grJ}}^{2}﹩ is similar to the resonant a > 49 au objects. Both: the median uncertainty of the points is indicated in the lower right. We resampled the data using a Gaussian distribution and the uncertainty on each point 100 times, and examined the resulting distributions. This resulted in broadening each distribution to very close to the width of the median uncertainty. The uncertainties on specific measurements are presented in the right panel of Figure 2.
Paper: Col-OSSOS: The Distribution of Surface Classes in Neptune's Resonances
Authors: Rosemary E. Pike, Wesley C. Fraser, Kathryn Volk, J. J. Kavelaars, Michaël Marsset, Nuno Peixinho, Megan E. Schwamb, Michele T. Bannister, Lowell Peltier, Laura E. Buchanan, Susan Benecchi, Nicole J. Tan
Figure caption: Upper panel: the PC﹩{}_{{grJ}}^{2}﹩ values and absolute magnitude in r-band H  r  at discovery. The dynamically excited objects span a large range of values, and the fraction above and below the PC﹩{}_{{grJ}}^{2}﹩ division does not obviously depend on H  r . The different dynamical classifications are consistent with previous figures: nonresonant dynamically excited objects (black circles), dynamically cold classical objects (pink squares), 4:3 resonators (orange triangles), 3:2 resonators (yellow squares), resonant objects within the classical region (green wide ‘x’s), 2:1 resonators (cyan diamonds), and resonant objects with semimajor axes a > 49 au (blue hexagons). Lower panel: the distribution of PC﹩{}_{{grJ}}^{2}﹩ values compared to object size, assuming albedos of 0.14 for PC﹩{}_{{grJ}}^{2}\lt -0.13﹩ and 0.085 for PC﹩{}_{{grJ}}^{2}\gt -0.13﹩. The distribution is shifted slightly compared to the H  r  panel, and the result is that the Plutinos and cold classicals appear to be more comparable in terms of intrinsic size.
Paper: Col-OSSOS: The Distribution of Surface Classes in Neptune's Resonances
Authors: Rosemary E. Pike, Wesley C. Fraser, Kathryn Volk, J. J. Kavelaars, Michaël Marsset, Nuno Peixinho, Megan E. Schwamb, Michele T. Bannister, Lowell Peltier, Laura E. Buchanan, Susan Benecchi, Nicole J. Tan
Figure caption: The population estimates of the intrinsic population required to reproduce the number of BrightIR and FaintIR detections found by Col-OSSOS in each subpopulation. The input model is for H  r  < 12 and is based on the OSSOS TNO model (see the main text for details). The relative intrinsic population sizes required to produce the number of real Col-OSSOS detections vary significantly for different subpopulations. The 3:2 distribution and the resonant a > 49 au distribution are quite similar to the dynamically excited distribution, while the other three resonant subpopulations are in between the cold classical and dynamically excited distribution, suggesting significant contributions to those resonances from both possible parent populations.
Paper: Col-OSSOS: The Distribution of Surface Classes in Neptune's Resonances
Authors: Rosemary E. Pike, Wesley C. Fraser, Kathryn Volk, J. J. Kavelaars, Michaël Marsset, Nuno Peixinho, Megan E. Schwamb, Michele T. Bannister, Lowell Peltier, Laura E. Buchanan, Susan Benecchi, Nicole J. Tan
Figure caption: The orbital distribution of Col-OSSOS TNOs, with surface classification indicated. As in Figure 1, the semimajor axis is scaled by three different amounts, as indicated in the x-axis and separated by gaps, and the symbol shapes are preserved, but the colors of the points indicate BrightIR classification (black) and FaintIR classification (red). The low-inclination and low-eccentricity 4:3 resonator at 36.4 au is particularly evident, as is the classification-inclination dependence, particularly at large-a, noted by Marsset et al. (2019) and Marsset et al. (2023). Neptune is indicated by the large blue circle.
Paper: Relation of Gravity, Winds, and the Moment of Inertia of Jupiter and Saturn
Authors: Burkhard Militzer, William B. Hubbard
Figure caption: Posterior distributions of MC ensembles of abstract models for Jupiter’s interior and Saturn’s interior without DR that match the observed values for q rot and J 2. The blue symbols represent measurements of the Juno and Cassini spacecraft, while the red symbols show predictions from models without DR effects. In panel (a), we compare ensembles of models with various numbers of spheroids. Counterintuitively, models with fewer spheroids tend to show a wider range of J 4 and J 6 values (see text). In panels (b) and (c), the background color, the color bar, and the contour lines represent the average MoI as a function of J 4 and J 6. N  S  = 20 spheroids were employed. DR effects alter Saturn’s MoI significantly, while they are less important for Jupiter. Jupiter’s MoI decreases with rising J 6, while it is almost independent of J 4. Conversely, Saturn’s MoI strongly depends on J 4 but still increases with rising J 6.
Paper: Relation of Gravity, Winds, and the Moment of Inertia of Jupiter and Saturn
Authors: Burkhard Militzer, William B. Hubbard
Figure caption: The even gravitational moments J  n  of Jupiter and Saturn vs. degree n. All moments have been scaled by powers of the rotational parameter, q rot, because the ratio ﹩{J}_{n}/{q}_{\mathrm{rot}}^{n/2}﹩ is approximately constant according to the ToF (Zharkov & Trubitsyn 1978). The variation of the ratios with the order n is due to the contribution of higher-order terms in the ToF, captured to high precision in the nonperturbative CMS method. The figure also illustrates that the effects of DR are much stronger for Saturn (blue shaded area) than for Jupiter because Saturn’s winds extend to a greater depth of ∼9000 km (Iess et al. 2018). Saturn models with DR fit the observed moments up to J 12, while uniform rotation models can only fit coefficients up to J 4, or up to J 6 if a density jump is included. Here we compare the Juno measurements with a uniform rotation model for Jupiter’s interior, while the model with DR in Militzer et al. (2022) matches the entire set of gravity coefficients.
Paper: Relation of Gravity, Winds, and the Moment of Inertia of Jupiter and Saturn
Authors: Burkhard Militzer, William B. Hubbard
Figure caption: Models of Jupiter and Saturn based on CMS calculations that match the gravity measurements of both planets. The zonal winds on Saturn are predicted to reach a depth of ∼9000 km, involving ∼7% of the planet’s mass. On Jupiter, they are predicted to reach ∼3000 km and thus involve only 1% of the planet’s mass. Because Jupiter is more massive, the pressure rises more rapidly with depth. Therefore, the helium rain layer, predicted to start approximately at 80–100 GPa, is located closer to the surface. While the gravity measurements for Jupiter imply that the planet has a dilute core, the state of Saturn’s core is less certain. Here we show a model with a compact core constructed to match the gravity measurements.
Paper: Relation of Gravity, Winds, and the Moment of Inertia of Jupiter and Saturn
Authors: Burkhard Militzer, William B. Hubbard
Figure caption: MoI of Saturn computed for different rotation periods that have been assumed in the literature. The physical model with DR matches the measured gravity harmonics J 2–J 12, while models without DR can only match values up to J 6. We prefer the period of 10:33:34 hr ± 55 s because it allows models with DR to match the Voyager measurements of the planet’s polar radius. Under these assumptions, we predict Saturn’s MoI to be equal to 0.2181 ± 0.0002. With a low-order ToF, Helled et al. (2009) predicted Saturn’s MoI to be 2% larger (yellow squares). The green band illustrates the range of predictions with four-spheroid calculations that were reported by Wisdom et al. (2022).
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: Same as Figure 4, but for the rest of the orbits.
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 AOTF transfer function for the order 185 of the NOMAD SO channel (the black curve). The orange and light blue curves show those shifted by one-sigma uncertainty in the Gaussian intensity parameter in the AOTF transfer function.