adsabs/AstroCLIMB huggingface dataset:
Paper: Rover Science Autonomy in Planetary Exploration: Field Analog Tests
Authors: Eldar Z. Noe Dobrea, Maria E. Banks, Roger N. Clark, David Wettergreen, Alberto Candela, Amanda Hendrix, Caitlin Ahrens, Ernie Bell, Abigail Breitfeld, Thomas F. Bristow, Sanlyn Buxner, Margaret Hansen, Gregory M. Holsclaw, Paul Knightly, Georgiana Kramer, Nandita Kumari, Melissa D. Lane, Audrey Martin, McKayla L. Meier, Ruby Patterson, Neil Pearson, Thomas Prettyman, Gregg A. Swayze, David Vaniman, Srinivasan Vijayarangan, Faith Vilas, Shawn P. Wright
Figure caption: Photogeological map of site 3, Yellow Cat Flat. Each unit is numbered and depicted in a different color.
Paper: Rover Science Autonomy in Planetary Exploration: Field Analog Tests
Authors: Eldar Z. Noe Dobrea, Maria E. Banks, Roger N. Clark, David Wettergreen, Alberto Candela, Amanda Hendrix, Caitlin Ahrens, Ernie Bell, Abigail Breitfeld, Thomas F. Bristow, Sanlyn Buxner, Margaret Hansen, Gregory M. Holsclaw, Paul Knightly, Georgiana Kramer, Nandita Kumari, Melissa D. Lane, Audrey Martin, McKayla L. Meier, Ruby Patterson, Neil Pearson, Thomas Prettyman, Gregg A. Swayze, David Vaniman, Srinivasan Vijayarangan, Faith Vilas, Shawn P. Wright
Figure caption: Zoë traversing efflorescent salt patches on clay-bearing deposits of the Blue Canyon, AZ—2021 October. The science cameras and spectrometer foreoptics are shown on the mast. A panel antenna allowed communication with a ground station at distances of up to 2 km.
Paper: The 2014–2015 Holuhraun Lava Flow-field in Iceland as a Planetary Analog for Young Volcanic Terrains in Elysium Planitia, Mars
Authors: J. R. C. Voigt, C. W. Hamilton, L. P. Keszthelyi, M. Varnam, S. M. Hibbard, K. M. Stack
Figure caption: Map of the study site showing the relative emplacement timing of materials within the four subfacies groups. The map was generated using a 1 cm pixel−1 basemap and is displayed over UltraCam-Xp data with a resolution of 20 cm pixel−1. The same shades of color indicate the plates that were initially formed as one and were subsequently separated by continuous lava emplacement. Thus, the different shades of color can be seen as the chronological sequence of the different units.
Paper: The 2014–2015 Holuhraun Lava Flow-field in Iceland as a Planetary Analog for Young Volcanic Terrains in Elysium Planitia, Mars
Authors: J. R. C. Voigt, C. W. Hamilton, L. P. Keszthelyi, M. Varnam, S. M. Hibbard, K. M. Stack
Figure caption: Perspective view showing crustal slab characteristics and cross section with inferred isotherms depths. Note that the total crust (∼12 cm thick) includes an upper brittle layer (∼5 cm thick) and underlying viscoelastic layer (∼7 cm thick). The gray region corresponds to the zone where the lava crust is expected to have been in the brittle regime with temperatures <800°C, the red region indicates where the lava is expected to have been in the viscoelastic regime between 800°C and 1070°C, and the orange region shows the upper part of the lava core, where the lava would have been in a fluidal regime with temperatures >1070°C. The irregular shape of each region maps to the shape of the detached crustal slab, and the depths to the rheological transitions correspond to the time when the primary brittle crustal slab detached from the underlying viscoelastic layer. The 5 cm thickness of the brittle crust is recorded in stratigraphy exposed in the foreground (i.e., indicated by the lower dashed line demarking the brittle to viscoelastic transition). Cooling times and other isotherms are inferred using equations from K. Hon et al. (1994) and the equation numbering refers to the equations therein. Please note that these values are approximate because they can vary based on lava composition, volatile content, cooling history, shear strain rate, and other factors that affect the lava’s thermo-rheology.
Paper: The 2014–2015 Holuhraun Lava Flow-field in Iceland as a Planetary Analog for Young Volcanic Terrains in Elysium Planitia, Mars
Authors: J. R. C. Voigt, C. W. Hamilton, L. P. Keszthelyi, M. Varnam, S. M. Hibbard, K. M. Stack
Figure caption: Field photographs providing examples of the different units mapped in Figure 6(a). Plates composed of lava waves. (b) Close-up and (c) approximate cross section of lava waves. (d) Relationship of plates to spreading zone. (e) Close-up of spreading zone, where two plates formed. (f) Fine-scale ridge, identified as compressional ridges of crustal slabs. White arrows point toward overtitled slabs and the black arrow points toward crustal slab overlapping on plate. (g) Topographic depression, identified as an inflation pit in the field.
Paper: The 2014–2015 Holuhraun Lava Flow-field in Iceland as a Planetary Analog for Young Volcanic Terrains in Elysium Planitia, Mars
Authors: J. R. C. Voigt, C. W. Hamilton, L. P. Keszthelyi, M. Varnam, S. M. Hibbard, K. M. Stack
Figure caption: Examples of similar lava morphologies at the Holuhraun eruption site in Iceland and Elysium Planitia on Mars. The left panels ((a) and (c)) display the Holuhraun eruption site, captured using the UltraCam-Xp basemap (2015 September 6) with a pixel scale of 20 cm pixel−1. The right panels ((b) and (d)) show Elysium Planitia on Mars based on HiRISE image with ∼26 cm pixel−1 and the Context camera with 6 m pixel−1 resolution, respectively. (a) Example of a large coherent flat-topped area, referred to as polygonal terrain. (c) Example of smaller flat-topped areas surrounded by hummocky terrain. Both panels (a) and (c) show spiny lava. (b) Polygonal terrain shares many similarities with spiny lava at Holuhraun, such as linear features displayed in the zoom-in of the insets in panels (a) and (b). (d) Lava margin of the Marte Vallis lava with flat-topped areas surrounded by hummocky terrain.
Paper: The 2014–2015 Holuhraun Lava Flow-field in Iceland as a Planetary Analog for Young Volcanic Terrains in Elysium Planitia, Mars
Authors: J. R. C. Voigt, C. W. Hamilton, L. P. Keszthelyi, M. Varnam, S. M. Hibbard, K. M. Stack
Figure caption: Example of rubbly and spiny facies including rafted material and polygonal terrain. (a) Geomorphological map of polygonal terrain near the northern margin of the 2014–2015 Holuhraun lava flow-field. Our focused study location is outlined in black, labeled “Figure 6.” The map overlays a 20 cm pixel−1 UltraCam-Xp basemap. (b) Rafted rubbly crust with newly created space in between forming polygonal terrain. The white arrow indicates the rafting motion.
Paper: The 2014–2015 Holuhraun Lava Flow-field in Iceland as a Planetary Analog for Young Volcanic Terrains in Elysium Planitia, Mars
Authors: J. R. C. Voigt, C. W. Hamilton, L. P. Keszthelyi, M. Varnam, S. M. Hibbard, K. M. Stack
Figure caption: (a)–(b): an example of lava surface of the Marte Vallis flow margin in Elysium Planitia based on HiRISE images (∼26 cm pixel−1). The black box in panel (a) denotes the location of panel (b). (c)–(d): lava surface example of the spiny facies at Holuhraun based on UltraCam-Xp basemap (2015 September 6) with a pixel scale of 20 cm pixel−1. The black box in panel (c) denotes the location of panel (d). Both images exhibit prominent polygonal terrain including linear sinuous features indicating spreading zones, which are marked with arrows.
Paper: The 2014–2015 Holuhraun Lava Flow-field in Iceland as a Planetary Analog for Young Volcanic Terrains in Elysium Planitia, Mars
Authors: J. R. C. Voigt, C. W. Hamilton, L. P. Keszthelyi, M. Varnam, S. M. Hibbard, K. M. Stack
Figure caption: Examples of prominent polygonal terrain with spatially associated ridges on Mars and at Holuhraun. (a) Examples of lava surface close to the Marte Vallis flow margin in Elysium Planitia based on HiRISE image (∼26 cm pixel−1). (b) Lava surface examples of the spiny facies at Holuhraun based on UltraCam-Xp basemap (2015 September 6) with a pixel scale of 20 cm pixel−1. Both panels display prominent polygonal terrain with ridges.
Paper: The 2014–2015 Holuhraun Lava Flow-field in Iceland as a Planetary Analog for Young Volcanic Terrains in Elysium Planitia, Mars
Authors: J. R. C. Voigt, C. W. Hamilton, L. P. Keszthelyi, M. Varnam, S. M. Hibbard, K. M. Stack
Figure caption: Examples of lava coils within polygonal terrain in (a) Athabasca Valles in Elysium Planitia (HiRISE image with ∼26 cm pixel−1) and (b) and (c) at Holuhraun (UAS image 10 cm pixel−1 and field picture, respectively). Note the different scales of the lava coils. (c) The relief of the lava rose is roughly 10 cm.
Paper: Lucy L′Ralph In-flight Calibration and Results at (152830) Dinkinesh
Authors: Amy A. Simon, Hannah H. Kaplan, Dennis C. Reuter, Matthew Montanaro, William M. Grundy, Allen W. Lunsford, Gerald E. Weigle, Richard P. Binzel, Joshua Emery, Jessica Sunshine, Carly Howett, Harold F. Levison, Simone Marchi, Keith S. Noll, John Spencer
Figure caption: Spectra of Dinkinesh and Selam. (a) MVIC I/F for Dinkinesh closest approach (red) and at lower phase on departure (black). Selam is shown at closest approach and has a similar spectral shape to Dinkinesh (blue). (b) Simultaneously fit MVIC I/F scans phase corrected to 30°. (c) LEISA Dinkinesh spectrum from closest approach (black) and at higher phase on departure (red). Selam at closest approach again shows a nearly identical spectral shape to Dinkinesh. (d) Simultaneously fit LEISA scans phase corrected to 30° and with a phase reddening correction.
Paper: Lucy L′Ralph In-flight Calibration and Results at (152830) Dinkinesh
Authors: Amy A. Simon, Hannah H. Kaplan, Dennis C. Reuter, Matthew Montanaro, William M. Grundy, Allen W. Lunsford, Gerald E. Weigle, Richard P. Binzel, Joshua Emery, Jessica Sunshine, Carly Howett, Harold F. Levison, Simone Marchi, Keith S. Noll, John Spencer
Figure caption: Dinkinesh spectral comparisons. (a) The composite MVIC and LEISA departure scan Dinkinesh data corrected to 30° phase. (b) The short-wavelength spectrum, normalized at 1.5 μm, with comparisons to other S- and Sq-type asteroid spectra (R. P. Binzel et al. 2001, 2004, L. E. McGraw et al. 2022, D. D. Polishook et al. 2023). (c) Dinkinesh’s 3 μm absorption band, normalized at 2.9 μm, compared with that of Ganymed and Themis (A. S. Rivkin & J. P. Emery 2010, L. E. McGraw et al. 2022).
Paper: Lucy L′Ralph In-flight Calibration and Results at (152830) Dinkinesh
Authors: Amy A. Simon, Hannah H. Kaplan, Dennis C. Reuter, Matthew Montanaro, William M. Grundy, Allen W. Lunsford, Gerald E. Weigle, Richard P. Binzel, Joshua Emery, Jessica Sunshine, Carly Howett, Harold F. Levison, Simone Marchi, Keith S. Noll, John Spencer
Figure caption: Locations of the centers of the 1.5 μm peak and 2 μm absorption in LL (blue diamonds), L (green triangles), and H (red squares) ordinary chondrites. These ordinary chondrite subtypes are distinguishable in this parameter space. The measured parameters for the Dinkinesh spectra (filled circles—black is the close approach spectrum, and magenta is the departure spectrum) are shown to agree with LL and L chondrites.
Paper: Lucy L′Ralph In-flight Calibration and Results at (152830) Dinkinesh
Authors: Amy A. Simon, Hannah H. Kaplan, Dennis C. Reuter, Matthew Montanaro, William M. Grundy, Allen W. Lunsford, Gerald E. Weigle, Richard P. Binzel, Joshua Emery, Jessica Sunshine, Carly Howett, Harold F. Levison, Simone Marchi, Keith S. Noll, John Spencer
Figure caption: Comparison of Dinkinesh with representative asteroids and their corresponding chondrites. (a) Dinkinesh’s spectrum (black points), continuum-removed and normalized at 1.5 μm, compared with those of Hebe, Massalia, and Eunomia (R. P. Binzel et al. 2019). (b) The same comparison, but with average ordinary chondrite subtype spectra (T. L. Dunn et al. 2010).
Paper: Lucy L′Ralph In-flight Calibration and Results at (152830) Dinkinesh
Authors: Amy A. Simon, Hannah H. Kaplan, Dennis C. Reuter, Matthew Montanaro, William M. Grundy, Allen W. Lunsford, Gerald E. Weigle, Richard P. Binzel, Joshua Emery, Jessica Sunshine, Carly Howett, Harold F. Levison, Simone Marchi, Keith S. Noll, John Spencer
Figure caption: Dinkinesh closest approach views from MVIC and LEISA. The top panel shows the MVIC pan band image showing Dinkinesh (right) and Selam (left), while the bottom panel shows a single frame acquired near the center of the LEISA scan. The middle panel shows the changing range and phase angles during each of the LEISA and MVIC observations.
Paper: Earth as an Exoplanet: Investigating the Effects of Cloud Variability on the Direct-imaging of Atmospheres
Authors: Soumil Kelkar, Prabal Saxena, Ravi Kopparapu, Joy Monteiro
Figure caption: (a) The wavelength-dependent surface albedos of the five surface types—ocean, snow, grass, soil, and forest. The albedo values have been taken from the USGS spectral library (R. Kokaly et al. 2017). The significant increase in the albedos of forest and grass at roughly 0.7 μm corresponds to the characteristic vegetation red edge signal, which indicates the presence of surface vegetation. (b) The vertical abundance profiles for the dominant gases and aerosols present in the atmosphere. The abundance of each constituent is denoted by its disk-integrated mass fraction in each layer of the atmosphere. These are modern Earth values derived from the MERRA-2 data corresponding to 2019 March 20th 00:00 UTC.
Paper: Earth as an Exoplanet: Investigating the Effects of Cloud Variability on the Direct-imaging of Atmospheres
Authors: Soumil Kelkar, Prabal Saxena, Ravi Kopparapu, Joy Monteiro
Figure caption: The top panel shows the different rotational configurations of the exo-Earth labeled by a rotational phase. These images only depict how the portion of the surface visible to the observer changes with rotation and do not imply that the planet is cloudless. The plots show the reflected light spectra for the different rotational phases as simulated by PSG for a cloudy and a cloud-free exo-Earth respectively. The entire wavelength bandpass is separated into three regions—(i) ultraviolet (UV) (0.2–0.5  μm), (ii) visible (VIS) (0.5–1  μm), and (iii) near-infrared (1–2 μm). The simulated error bars have been removed for the sake of visual clarity. The cloudy planet shows a higher continuum in the reflected light, which is attributed to the enhanced albedo in the presence of clouds. The spectrum of a cloudy planet also shows a higher degree of variation between rotational phases due to variable cloud patchiness.
Paper: Earth as an Exoplanet: Investigating the Effects of Cloud Variability on the Direct-imaging of Atmospheres
Authors: Soumil Kelkar, Prabal Saxena, Ravi Kopparapu, Joy Monteiro
Figure caption: The top panel shows the evolution of the monthly averaged global cloud mass across MERRA-2’s historic record from 1984 to 2023. The dashed and the dotted lines represent the maximum and minimum of the data, which correspond to the months of 1999 July and 1987 February respectively. The solid line represents the mean, which is closest to the 2011 January monthly averaged data. The faint blue curve represents the actual data while the dark blue curve is the rolling average over a window of 7 months. The bottom panels depict trends in cloud cover variability over seasonal and diurnal timescales. The left panel shows the trends in global cloud mass across a year, and the boxes have been constructed using monthly averaged data from 1984 to 2023. The right panel depicts the diurnal trend, and the boxes are plotted using instantaneous 3 hr data for all days in the month of 1999 July. For both these panels, the dark blue line represents the median, the edges of the box extend from the first quartile (Q1) to the third quartile (Q3), the whiskers extend to the farthest data points within 1.5 times the interquartile range (Q3–Q1) from the box, and the outliers are data points beyond this range.
Paper: Earth as an Exoplanet: Investigating the Effects of Cloud Variability on the Direct-imaging of Atmospheres
Authors: Soumil Kelkar, Prabal Saxena, Ravi Kopparapu, Joy Monteiro
Figure caption: The wavelength-dependent SNRs of the three gases, O2, O3, and H2O. The top panel shows the results for a cloudy exo-Earth while the bottom panel depicts the same for a cloud-free exo-Earth. The simulations are performed in PSG using a 6 m HWO template and a suitable noise model assuming that the exo-Earth is situated 10 pc away, and the exposure time is set to 24 hr. The corresponding net SNRs for each gas across the entire wavelength region is given in the legend. Clouds enhance the SNRs of all the three gases and hence improve their detectability in an exo-Earth atmosphere. The increase in SNR for each gas is dependent on its vertical distribution with respect to the distribution and opacity of patchy clouds.
Paper: Earth as an Exoplanet: Investigating the Effects of Cloud Variability on the Direct-imaging of Atmospheres
Authors: Soumil Kelkar, Prabal Saxena, Ravi Kopparapu, Joy Monteiro
Figure caption: A global cloud layer of constant 0.1 bar thickness is considered at four different pressure levels—(i) 0.8–0.7 bar, (ii) 0.48–0.38 bar, (iii) 0.34–0.24 bar, and (iv) 0.18–0.08 bar. The top panel shows the reflectance spectra for these four cases with a clear sky spectrum plotted for reference. As before, these simulations are done with a 6 m HWO template with an exposure time of 24 hr for a planet that is 10 pc away. The middle panel shows the SNRs of O2 in the visible band and O3 in the UV band, and the bottom panel shows the SNRs of H2O in the visible and NIR band. As the altitude of the cloud layer increases, the clouds become optically thinner, and thus, their reflectivity reduces leading to a lower continuum in the reflected light spectrum. The trends seen in the SNRs of all the three gases is a reflection of how they are distributed with respect to the global cloud layer.
Paper: Two Possible Orbital Histories of Phobos
Authors: Matija Ćuk, Kaustub P. Anand, David A. Minton
Figure caption: Two sets of five different numerical simulations of Phobos’s noncapture crossing through the Yoder (1:2) semisecular resonance with the Sun at 3.2 RM. In the left-hand panel, we started Phobos with substantial e and i with the postresonance orbit bracketing the “APH branch” nominal orbital history. We can conclude that one set of possible preresonance orbital elements of Phobos is approximately eP = 0.02 and iP ≈ 0﹩\mathop{.}\limits^{\unicode{x000B0}}﹩8. In the right-hand panel, we started Phobos on a circular, planar orbit consistent with recent formation, with the outcome clearly inconsistent with the subsequent orbit of Phobos. Using standard tidal assumptions and ignoring any past ring torques, this crossing happened about 60 Myr ago.
Paper: Two Possible Orbital Histories of Phobos
Authors: Matija Ćuk, Kaustub P. Anand, David A. Minton
Figure caption: Eccentricity of Deimos in a set of 10 simulations of the long-term evolution of Deimos’s orbit that were completed using the S-SIMPL-READ integrator. Each simulation was started with eD = 0.0006 and iD = 1﹩\mathop{.}\limits^{\unicode{x000B0}}﹩8 but with different axial tilts of Mars ranging from 22° and 40°. The evolution of the planetary orbits in all of these simulations is the same and starts from the current configuration.
Paper: Two Possible Orbital Histories of Phobos
Authors: Matija Ćuk, Kaustub P. Anand, David A. Minton
Figure caption: Two sets of 10 different numerical simulations of Phobos’s capture in the Touma (2:3) semisecular resonance with the Sun at 2.94 RM, with the conserved quantity ﹩{C}_{{\rm{T}}}={e}_{{\rm{P}}}^{2}+2{\sin }^{2}{i}_{{\rm{P}}}﹩ consistent with our nominal orbital history. The simulations on the right have initial iP = 0 and Martian tidal Q = 120, while those on the left have initial iP = 0﹩\mathop{.}\limits^{\unicode{x000B0}}﹩25 and Martian Q = 80. In each case, 10 different simulations each had slightly different initial semimajor axes for Phobos, resulting in different times of resonance capture. While the initially planar orbits almost all evolve to eccentricities below eP = 0.01, simulations with a nonzero initial inclination drop out of resonance earlier. Our nominal reconstructed outcome of eP ≈ 0.02 and iP ≈ 0﹩\mathop{.}\limits^{\unicode{x000B0}}﹩7 is within the spread of outcomes.
Paper: Two Possible Orbital Histories of Phobos
Authors: Matija Ćuk, Kaustub P. Anand, David A. Minton
Figure caption: Six different numerical simulations of Phobos’s capture into the Yoder (1:2) semisecular resonance with the Sun at 3.2 RM when evolving outward due to disk torques. Phobos is assumed to be on a low-e, low-i orbit immediately following formation from a ring (as suggested by RPH). The three simulations on the left-hand side used the initial axial tilt of Mars of 25° (light blue), 35° (green), and 40° (purple), while the three simulation on the right used the initial axial tilt of Mars of 45° (green), 50° (purple), and 55° (light blue).
Paper: Two Possible Orbital Histories of Phobos
Authors: Matija Ćuk, Kaustub P. Anand, David A. Minton
Figure caption: Eccentricity of Deimos in two simulations of the long-term evolution of Deimos’s orbit that start from the present configuration. Green points have been obtained using numerical integrator S-SIMPL, which fully integrated the dynamics of Deimos, eight planets, and the Martian spin axis. The purple points were obtained using the S-SIMPL-READ integrator, in which Deimos’s dynamics is simulated using precalculated positions for the planets and the Martian spin axis.
Paper: Two Possible Orbital Histories of Phobos
Authors: Matija Ćuk, Kaustub P. Anand, David A. Minton
Figure caption: Eccentricity of Deimos during the crossing of the 3:1 Phobos–Deimos MMR as Phobos was migrating inward. If we assume that Phobos had very low eccentricity, there is little effect on Deimos (black points), but if the eccentricity of Phobos was eP = 0.01 (magenta) or eP = 0.02 (green) at the time, Deimos’s eccentricity is excited above the observed value of eD = 0.00027. Using standard assumptions, this crossing happened about 100 Myr ago.
Paper: Two Possible Orbital Histories of Phobos
Authors: Matija Ćuk, Kaustub P. Anand, David A. Minton
Figure caption: Two sets of numerical simulations of Phobos’s crossing of the Yoder (1:2) semisecular resonance with the Sun at 3.2 RM with high initial eccentricity and near-zero inclination. The purpose of these simulations is to model the evolution of Phobos after the end of capture in the Yoder resonance, with the focus on potential separate excitation of Phobos’s inclination. The left-hand panel shows the crossing of the resonance while Phobos is moving outward due to ring torques, while the right-hand panel shows the inward crossing of the resonance by Phobos once tides become dominant. The two simulations on the left-hand side used the initial axial tilt of Mars of 25° and 45°, while the six simulations on the right used these two obliquities and three different net migration rates (equivalent to Martian Q = 80, 100, and 120).
Paper: Two Possible Orbital Histories of Phobos
Authors: Matija Ćuk, Kaustub P. Anand, David A. Minton
Figure caption: Eccentricity of Deimos in two 10 Myr simulations of Deimos’s orbit that were conducted in order to compare numerical integrators. The purple points plot the beginning of one of the S-SIMPL-READ integrations from Figure 11 (with ϵ = 34°); this integration showed the most drastic changes in eD within the first few Myr. The green points plot an integration with the same initial conditions done using S-SIMPL (i.e., with Deimos and the planets integrated directly and together and not in two stages). The overall similarity of the eD changes confirms that S-SIMPL-READ is able to capture the most relevant sources of Deimos’s chaotic dynamics despite being computationally less expensive.
Paper: Two Possible Orbital Histories of Phobos
Authors: Matija Ćuk, Kaustub P. Anand, David A. Minton
Figure caption: Four different numerical simulations of Phobos’s noncapture crossing through the Touma (2:3) semisecular resonance with the Sun at 2.94 RM, with the postresonance orbit of Phobos consistent with our nominal orbital history. We can conclude that one set of possible preresonance orbital elements of Phobos is approximately eP = 0.018 and iP = 0﹩\mathop{.}\limits^{\unicode{x000B0}}﹩8.