adsabs/AstroCLIMB huggingface dataset:
Paper: The Water Activity of Mars-relevant Multicomponent Brines: The Changing Influence of Perchlorate on Habitability over Time
Authors: Adam H. Stevens, Charles S. Cockell
Figure caption: Water activity isolines showing limits of habitability for all tested combinations of salts. Red areas should be uninhabitable as they are below 0.55 a  w , yellow shows where habitability will be possible for the most extreme known organisms (0.55 < a  w  < 0.65), and green shows where brines of that combination of salts should be habitable (a  w  > 0.65).
Paper: The Water Activity of Mars-relevant Multicomponent Brines: The Changing Influence of Perchlorate on Habitability over Time
Authors: Adam H. Stevens, Charles S. Cockell
Figure caption: (a) An initially habitable magnesium sulfate dominated brine becoming enriched in magnesium perchlorate remains habitable until the concentration of perchlorate reaches ∼75% of saturation. (b) An initially habitable magnesium perchlorate dominated brine becoming enriched in calcium chloride becomes uninhabitable well before either salt reaches saturation.
Paper: Stereophotoclinometry on the OSIRIS-REx Mission: Mathematics and Methods
Authors: R. W. Gaskell, O. S. Barnouin, M. G. Daly, E. E. Palmer, J. R. Weirich, C. M. Ernst, R. T. Daly, D. S. Lauretta
Figure caption: Three main loops of SPC (right) with inputs (left) for generating the final set of DTMs. Convergence of the spacecraft (S/C) position and attitude and the regional DTM’s surface and center end the SPC estimation process (Palmer et al. 2022).
Paper: The Water Activity of Mars-relevant Multicomponent Brines: The Changing Influence of Perchlorate on Habitability over Time
Authors: Adam H. Stevens, Charles S. Cockell
Figure caption: Water activity residual (modeled value–measured value) for all measured multicomponent brines, plotted against the total ionic strength of the mixed solution. Line of best fit shown for all values. Error bars are estimated 0.01 a  w  variation in laboratory measurements.
Paper: The Water Activity of Mars-relevant Multicomponent Brines: The Changing Influence of Perchlorate on Habitability over Time
Authors: Adam H. Stevens, Charles S. Cockell
Figure caption: Same data as in Figure 5, but separated by salt combination. No pattern of a particular ion or ions increasing the error in calculations is evident.
Paper: The Water Activity of Mars-relevant Multicomponent Brines: The Changing Influence of Perchlorate on Habitability over Time
Authors: Adam H. Stevens, Charles S. Cockell
Figure caption: Comparison of calculated and measured water activity for NaCl solution and MgSO4 solution. Error bars are estimated 0.01 a  w  measurement error.
Paper: The Water Activity of Mars-relevant Multicomponent Brines: The Changing Influence of Perchlorate on Habitability over Time
Authors: Adam H. Stevens, Charles S. Cockell
Figure caption: Comparison of calculated water activity from our model vs. those calculated using a different method from experimentally measured heat capacities of Toner & Catling (2016).
Paper: Are NH3 and CO2 Ice Present on Miranda?
Authors: Riley A. DeColibus, Nancy J. Chanover, Richard J. Cartwright
Figure caption: Left panel: a close-up of the most promising NH3-bearing synthetic models from Figure 6, compared to the UT201008 GNIRS spectrum of Miranda’s leading hemisphere. The synthetic spectra are described in Table 8. Small periodic variations are visible in the synthetic spectra due to resonances from the calculated Mie scattering solutions. Right panel: a demonstration of the lack of CO2 ice features on Miranda’s trailing hemisphere, compared to the trailing hemisphere of Ariel (Cartwright et al. 2022). We include several Hapke model spectra: pure CO2 ice (10 μm grains), a base model (Table 8), the base model with 10% areally mixed CO2 ice (27.5 μm grains), and the base model with 10% intimately mixed CO2 ice (27.5 μm grains). We also include a laboratory spectrum of a H2O:CO2 ice molecular mixture (Bernstein et al. 2005), which displays a prominent 2.13 μm 2ν 3 overtone band. Note that this forbidden overtone does not appear in pure CO2 ice or the model spectra of H2O:CO2 ice intimate mixtures.
Paper: Are NH3 and CO2 Ice Present on Miranda?
Authors: Riley A. DeColibus, Nancy J. Chanover, Richard J. Cartwright
Figure caption: Left panel: synthetic spectra generated with a Hapke–Mie modeling program to investigate potential absorption features in the 2.2 μm region, compared to the UT201008 GNIRS spectrum of Miranda’s leading hemisphere (bottom, binned by 10 pixels). The synthetic spectra are described in Table 8. The left panel includes comparison spectra, in which a small percentage of the 27.5 μm H2O ice in the base model is replaced with an additional component of different composition, with a grain size of 10 μm. Vertical lines are placed at 2.21 and 2.24 μm. Right panel: as the left panel, but using synthetic spectra of the corresponding pure (100%) ices at 10 μm grain size, scaled by a factor of 0.1. The observed GNIRS spectrum is divided by the base model.
Paper: Are NH3 and CO2 Ice Present on Miranda?
Authors: Riley A. DeColibus, Nancy J. Chanover, Richard J. Cartwright
Figure caption: Left panel: the UT201008 GNIRS spectrum of Miranda’s leading hemisphere (gray error bars at native resolution, black error bars binned by 5 pixels) compared to several laboratory-measured absorbance spectra of NH-bearing species (digitized from Figures 6 and 14 of Moore et al. 2007). The laboratory spectra are arbitrarily scaled and offset. We also include a reflectance spectrum of NH4Cl at 90 K from Fastelli et al. (2022). Right panel: arbitrarily scaled linear combinations of the lab spectra with our synthetic base model for qualitative comparison of band shapes and locations. Vertical lines are placed at 2.21 and 2.24 μm.
Paper: Are NH3 and CO2 Ice Present on Miranda?
Authors: Riley A. DeColibus, Nancy J. Chanover, Richard J. Cartwright
Figure caption: Left panel: our base model of Miranda’s spectrum compared to 5% areal mixtures of NH4-bearing minerals and thermonatrite. The mixture spectra were normalized to match the base model at 1.754 μm, then offset in increments of 0.1. The vertical line marks the mean wavelength of our 2.2 μm band measurements at 2.218 μm. Right panel: NH4-bearing mineral reflectance spectra measured at 90 K from Fastelli et al. (2022) and thermonatrite measured at 93 K from De Angelis et al. (2019).
Paper: Are NH3 and CO2 Ice Present on Miranda?
Authors: Riley A. DeColibus, Nancy J. Chanover, Richard J. Cartwright
Figure caption: Left panel: sources of spectral contamination in K band. The atmospheric transmission curves for telluric species are plotted as the fraction of light transmitted and have correct scaling relative to each other. The solar spectrum has been divided by a 5777 K blackbody spectrum. The plotted Miranda spectrum is a grand average of all TripleSpec spectra. The scaling on the solar, airglow, and Miranda spectra are arbitrary for visualization purposes. The wavelengths of the absorption features of interest in this work are annotated below the Miranda spectrum: the CO2 ice triplet and the 2.13 μm band are marked in blue, and features associated with NH3-bearing species are marked in green. Right panel: inset zoom for the box marked in the left panel. Note the “spike” residuals in the Miranda spectrum that closely match the OH and solar lines.
Paper: Effects of the Librationally Induced Flow in Mercury’s Fluid Core with an Outer Stably Stratified Layer
Authors: Fleur Seuren, Santiago A. Triana, Jérémy Rekier, Ankit Barik, Tim Van Hoolst
Figure caption: Structure of the core flow in response to the m = 2 libration forcing for Ek = 10−9, with (left) the radial (u  r ) and horizontal (﹩{({{u}_{\theta }}^{2}+{{u}_{\phi }}^{2})}^{1/2}﹩) as a function of the radial coordinate near the CMB and (right) the radial vorticity ﹩{\xi }_{r}=\hat{{\boldsymbol{r}}}\,\cdot \,{\boldsymbol{\nabla }}\times u﹩ at the (local) maximum of horizontal kinetic energy that is indicated by the vertical lines in the left figures. The top panels correspond to the fluid motions in a neutrally stratified core (N 0 = 0), and the bottom panels correspond to the motions in a core with a stably stratified outer layer with N 0 = 100.
Paper: Effects of the Librationally Induced Flow in Mercury’s Fluid Core with an Outer Stably Stratified Layer
Authors: Fleur Seuren, Santiago A. Triana, Jérémy Rekier, Ankit Barik, Tim Van Hoolst
Figure caption: (a) Example of the Reynolds number near the CMB in function of the Ekman number when the core is stably stratified with stratification parameters N 0 = 100, r ICB = 0.4, r C = 0.7, and h = 0.1 and the mantle is forced by the radial components of libration, m = 2 (blue) and −2 (red). The expected value of the Reynolds number at Mercurial conditions, Ek = 2 × 10−13, assuming a linear relationship between ﹩\mathrm{log}(\mathrm{Re})﹩ and ﹩\mathrm{log}(\mathrm{Ek})﹩, is indicated with a circle. (b) Extrapolated Reynolds numbers of the m = 2 core flow response near Mercury’s CMB for different stratification strengths N 0. The blue circle represents the Reynolds number estimated from the left panel. The slightly irregular behavior for 10 ≲ N 0 ≲ 102.5 is an artifact of the numerical method not being precise enough to determine the location of maximum horizontal velocity when the peak of the horizontal flow profile is less pronounced.
Paper: Effects of the Librationally Induced Flow in Mercury’s Fluid Core with an Outer Stably Stratified Layer
Authors: Fleur Seuren, Santiago A. Triana, Jérémy Rekier, Ankit Barik, Tim Van Hoolst
Figure caption: Magnetic field induced by the core flow resulting from the radial components of libration given an outer stably stratified layer with N 0 = 100, h = 0.1, r C = 0.7, and r ICB = 0.4 and assuming a conductive layer at the base of the mantle with c = 10−4 and ﹩c^{\prime} ={10}^{-4}﹩. (a) The rms value of the radial magnetic field b  r  at the CMB as a function of the Ekman number in response to the m = 2 and −2 libration forcing. (b) Radial magnetic field at the core surface induced by the m = 2 forcing component for Ek = 10−10.
Paper: Effects of the Librationally Induced Flow in Mercury’s Fluid Core with an Outer Stably Stratified Layer
Authors: Fleur Seuren, Santiago A. Triana, Jérémy Rekier, Ankit Barik, Tim Van Hoolst
Figure caption: Division of the total kinetic energy ﹩{{ \mathcal E }}_{\mathrm{kin}}﹩ and CMB viscous torque Γ ν,z  of the core flow, computed for different magnetic field conditions, by a reference solution, denoted by the black vertical line.
Paper: Effects of the Librationally Induced Flow in Mercury’s Fluid Core with an Outer Stably Stratified Layer
Authors: Fleur Seuren, Santiago A. Triana, Jérémy Rekier, Ankit Barik, Tim Van Hoolst
Figure caption: Division of the total kinetic energy ﹩{{ \mathcal E }}_{\mathrm{kin}}﹩ and CMB viscous torque Γ ν,z  of the core flow, computed at different values of the smoothness parameter h, by a reference solution, denoted by the black vertical line.
Paper: Effects of the Librationally Induced Flow in Mercury’s Fluid Core with an Outer Stably Stratified Layer
Authors: Fleur Seuren, Santiago A. Triana, Jérémy Rekier, Ankit Barik, Tim Van Hoolst
Figure caption: Comparison of horizontally averaged profiles of radial (〈u  r 〉), latitudinal (〈u  θ 〉), and azimuthal (〈u  ϕ 〉) velocities from MagIC and Kore. The top panel shows comparison case 1 with no stable layer, while the bottom panel shows comparison case 2 with a stably stratified layer.
Paper: Effects of the Librationally Induced Flow in Mercury’s Fluid Core with an Outer Stably Stratified Layer
Authors: Fleur Seuren, Santiago A. Triana, Jérémy Rekier, Ankit Barik, Tim Van Hoolst
Figure caption: Division of the total kinetic energy ﹩{{ \mathcal E }}_{\mathrm{kin}}﹩ and CMB viscous torque Γ ν,z  of the core flow, computed at different values of the inner core radius r ICB, by a reference solution, denoted by the black vertical line.
Paper: Effects of the Librationally Induced Flow in Mercury’s Fluid Core with an Outer Stably Stratified Layer
Authors: Fleur Seuren, Santiago A. Triana, Jérémy Rekier, Ankit Barik, Tim Van Hoolst
Figure caption: Division of the total kinetic energy ﹩{{ \mathcal E }}_{\mathrm{kin}}﹩ and CMB viscous torque Γ ν,z  of the core flow, computed at different values of the convective core radius r C, by a reference solution, denoted by the black vertical line.
Paper: Effects of the Librationally Induced Flow in Mercury’s Fluid Core with an Outer Stably Stratified Layer
Authors: Fleur Seuren, Santiago A. Triana, Jérémy Rekier, Ankit Barik, Tim Van Hoolst
Figure caption: Comparison of the structure of the modes at 99% of the outer boundary radius from the two codes MagIC and Kore. This figure shows comparison case 1 with no stable layer.
Paper: Nuclear and Orbital Characterization of the Transition Object (4015) 107P/Wilson–Harrington
Authors: Theodore Kareta, Vishnu Reddy
Figure caption: The newly acquired visible (blue) and archival near-infrared (red) reflectance spectra of (4015) 107P/Wilson–Harrington are shown, along with two dates of complimentary visible photometry (black filled and unfilled circles), normalized to R(λ) = 1.0 at 0.55 μm and aligned such that their median values are identical over the 0.8–0.9 μm wavelength range. The error bars on the visible photometry of Wilson–Harrington are only slightly larger than the data points. The two spectra agree well in curvature and slope in region where they overlap, though the visible spectrum is slightly redder likely due to phase-reddening.
Paper: Nuclear and Orbital Characterization of the Transition Object (4015) 107P/Wilson–Harrington
Authors: Theodore Kareta, Vishnu Reddy
Figure caption: Left: observations of 107P/Wilson–Harrington by the ATLAS Survey (Tonry et al. 2018) through their Orange and Cyan filters are corrected by the object’s heliocentric and geocentric distances and compared against the maximum-likelihood parameter combination models from our Markov Chain Monte Carlo (MCMC) analysis described in detail in the text. Right: the outcome of our MCMC analysis is shown as a corner plot, and the 99.7% confidence intervals for both filters are listed in the top right. As expected, the data and simple straight-line model (H(1, 1, α) = H(1, 1, 0) + β × α) agree well, as we do not measure the object’s brightness at small enough phase angles to probe any possible opposition surge. The slope of either curve is fully compatible with comets or low-albedo asteroids.
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) Morphological map of the Raditladi impact basin (27.°28N, 240.°93W), highlighting the distribution of hollows (yellow), lobate debris aprons bordering the peak ring ridges (red), fractures within the plains enclosed by the peak ring (white lines), and small, moated craters (blue dots). (B) and (C) Detailed views of a lobate feature, with yellow arrows marking its frontal margin and red arrows pointing out clusters of hollows. Panels (D) and (E) illustrate elevation profiles X–X′ and Y–Y′, respectively, indicating the lobe’s projected maximal thicknesses of ∼200 and ∼250 m. These estimates are based on the assumption that the nearly flat terrain at the lobe’s margin (red-circled white dot) persists under the lobate deposit. The pre-hollow topography is approximated by linking the surrounding elevations. This reconstruction suggests the hollows generated a negative relief of about 50–75 m (areas marked by red lines in profile Y–Y′). Data sources: Panel (A) consists of a darkened MESSENGER MDIS global base map (∼166 m px−1; courtesy of NASA/JPL/GSFC). Panel (B) integrates a geo-registered MESSENGER Regional Targeted Mosaic (RTM N01_003828_2238046) and a custom DTM (DTM RAA201_EQv1), whereas panel (C) combines geo-registered RTMs (N01_003828_2238046 & N01_000167_0593484) with a custom DTM (DTM RAB202_EQv1). Detailed information on RTM processing and DTM creation can be found in the supplementary materials.
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) Peak ring sections with flat tops, marked by red arrows. Elevation profiles L–L′ and Z–Z′ chart the topographic changes over steep-sided and flat-topped peak ring sections, respectively. We utilized their topography to generate the profiles for the peak ring’s VRL-shed sequence illustrated in panels (B) and (C). (B) The schematic diagram illustrates the reconstructed stratigraphy of the peak ring, including a VRL zone atop the impact-uplifted basaltic crust. Drawing from our numerical data in Figures 9(B) and (C), we suggest that the impact heat induced a thermal anomaly beneath the peak ring, leading to a partially melted region (medium-tone orange). VRL materials with minimal melt are depicted in light-tone orange. (C) Diagram correlating flat-topped mesas with the hypothesized source of morphologic glaciers. Our theory suggests instability in the peak ring ridges’ upper sections caused ductile flow, leading to the creation of expansive lobate aprons that share morphological traits with glaciers (dark-tone orange). (D), (E) Flow simulations account for factors such as stratigraphic composition, thermal structure, topography, and volatile-rich composition. The simulations display lobate profiles in gravity-induced flow, with runout distance over time being dependent on variables like viscosity, gravity, and substrate slope. The simulation reveals an elevation range of 100–250 m, tapering down to a few tens of meters for the S8 case (E) and a steep front for the halite case (D). The labels T 1 − T 5 denote times of flow evolution, with T 0 representing the initial thickness of the VRL. Late-stage profiles range from hours to days for the S8 flow, while they stretch to millennia for the halite flow. Our simulated profiles closely mirror the observed ones depicted in Figure 2(B). Data sources: (A) These reconstructions incorporate geo-registered RTMs (RTMs N01_000167_0593484 & N01_003828_2238046) and a DTM (DTM RAD202_EQv1). Comprehensive information about the RTM processing and DTM generation can be referenced in the supplementary materials.
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) Moated craters (white arrows) on a morphologic glacier-like lobe, as captured in the geo-registeredRTM (image N01_003818_2236022). Detailed procedures for RTM processing can be found in the supplementary materials, with context and geographic location provided in Figure 2(A). (B) Cross-sectional reconstruction, drawn along line M to M′, postulates the formation of moats due to impact-induced exposure of near-surface, volatile-rich materials along the edges of some small (subkilometer to a few kilometers) craters. (C) The modeling of surface solar heat waves reveals a relatively shallow penetration depth (∼3–8 m), consistent with the long-term retention of volatiles (see Sections 4.2.2.4 and 4.2.2.5). The presented profiles represent the thermal extremes, with the warmest portion of daytime (upper curves) and the coldest point of nighttime (lower curves). This finding, aligning with the hypothesis that hollows are recent geological features, extends the same process to explain the formation of moated craters. The model incorporates a range of parameters, including a peak solar irradiance of 9000 W m−2, emissivity set at 0.95, an albedo of 0.06, and a geothermal flux of 20 mW m−2. Thermal conductivities are specified as K  t  = 3 W m−1 K−1 for intact rock, K  t  = 1.75 W m−1 K−1 for a composite substance, and K  t  = 0.3 W m−1 K−1 for highly porous soil.
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) Overview of the Raditladi impact basin, indicating the region magnified in panel (B), which zeros in on a landslide extending from the southeastern rim (highlighted by a white arrow). Notably, the landslide lacks associated hollows. For comparison, panel (C) introduces the Holbeck landslide from North Yorkshire, England—a coastal landslide—marked by a white arrow. Data source: panel (A) consists of a MESSENGER Mercury global DEM (∼665 m px−1) draped over a MESSENGER MDIS global base map (∼166 m px−1; courtesy of NASA/JPL/GSFC). Panel (B) consists of an MDIS base map (∼166 m pixel−1; courtesy of NASA/JPL/GSFC).
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: View showing the locations of north polar high gravity anomalies interpreted to be locations of craters and basins that were covered by thick stacks of northern-plain-forming lavas before the LHB (Qingyun et al. 2018). The color-coded, band-limited, degree-strength Bouguer anomaly map of the northern high latitudes of Mercury (regions above 45°N) is superimposed on the MESSENGER MDIS global base map. The MDIS base map furnishes a higher spatial resolution, approximating 166 m per pixel.
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) Eminescu crater’s central peak surrounded by high albedo lobate structures. (B) The enlarged view reveals the bright regions as clustered depressions with marginal patchy textures. We suggest these depressions originated from the loss of volatiles in the VRL lobes extending from the peak ring. Data sourced from MESSENGER’s QuickMap tool Regional Targeted Mosaic (RTM).
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: Polar projection of Mercury’s northern region, highlighting the geographical locations of BC, Raditladi Crater (Figure 2(A)), and Eminescu Crater (Figure 6(A)). This image consists of a MESSENGER Mercury global DEM (∼665 m px−1) draped over a MESSENGER Mercury Dual Imaging System (MDIS) global base map (∼166 m px−1; courtesy of NASA/JPL/GSFC).