adsabs/AstroCLIMB huggingface dataset:
Paper: Constraining Ocean and Ice Shell Thickness on Miranda from Surface Geological Structures and Stress Modeling
Authors: Caleb Strom, Tom A. Nordheim, D. Alex Patthoff, Sherry K. Fieber-Beyer
Figure caption: Same as Figures 13 and 14 but showing the results for stress models with obliquity values other than 15°. Tidal stress is modeled for obliquity values of 1°, 3°, 5°, and 10°. Note that in all models, the pattern of tidal stress magnitude increasing significantly for ice shells ≤30 km in thickness is the same as for the models with 15°. Only the magnitude is different. Also note that tidal stress magnitude for obliquity tides only exceeds 1000 kPa for ice shells ≤30 km thick assuming ≥1E14 Pa-s lower ice shell viscosity.
Paper: Constraining Ocean and Ice Shell Thickness on Miranda from Surface Geological Structures and Stress Modeling
Authors: Caleb Strom, Tom A. Nordheim, D. Alex Patthoff, Sherry K. Fieber-Beyer
Figure caption: A south pole projection plot made in SatStressGUI showing the stress across the surface of Miranda from obliquity tidal stress. The obliquity is 1°. The lower ice shell thickness is 2 km, the lower ice shell viscosity is 1E15 Pa-s, and the upper brittle crust thickness is 1 km. Red and positive represent tensile stress. Note the asymmetric antipodal stress pattern where one hemisphere is predominantly in tension while the other hemisphere is predominantly in compression with a mixture in the center near the south pole.
Paper: Constraining Ocean and Ice Shell Thickness on Miranda from Surface Geological Structures and Stress Modeling
Authors: Caleb Strom, Tom A. Nordheim, D. Alex Patthoff, Sherry K. Fieber-Beyer
Figure caption: For a brittle crust thickness of 5 km, the pattern of increasing stress from polar wander magnitude with decreasing lower ice shell thickness is the same as for 1 km brittle crust thickness, except the magnitude range is much lower and there is no spike in stress magnitude increase for extremely thin ice shells. Circles and triangles are added for clarity.
Paper: Constraining Ocean and Ice Shell Thickness on Miranda from Surface Geological Structures and Stress Modeling
Authors: Caleb Strom, Tom A. Nordheim, D. Alex Patthoff, Sherry K. Fieber-Beyer
Figure caption: A SatStressGUI plot showing stress from 1° of polar wander. The plot shows an asymmetric antipodal stress pattern with compression in one hemisphere and extension on the other hemisphere, with a mixture near the south pole. In this example, the lower ice shell thickness is 2 km with a 1 km thick brittle upper ice shell and a lower ice shell viscosity of 1E15 Pa-s. Note the higher stress magnitude compared to Figure 6.
Paper: Constraining Ocean and Ice Shell Thickness on Miranda from Surface Geological Structures and Stress Modeling
Authors: Caleb Strom, Tom A. Nordheim, D. Alex Patthoff, Sherry K. Fieber-Beyer
Figure caption: For brittle crust thickness of 5 km, the pattern of change in the tidal stress with the change in ice shell thickness (increasing stress with decreasing ice shell thickness) is the same as the results for 1 km brittle crust thickness, except for a notable difference in magnitude and the lack of the spike in stress magnitude increase seen for extremely thin ice shells for 1 km brittle crust thickness. Shapes are added for clarity and do not represent data points.
Paper: Constraining Ocean and Ice Shell Thickness on Miranda from Surface Geological Structures and Stress Modeling
Authors: Caleb Strom, Tom A. Nordheim, D. Alex Patthoff, Sherry K. Fieber-Beyer
Figure caption: For a brittle ice shell thickness of 5 km and obliquity tidal stress, the pattern, where stress magnitude increases as ice shell thickness decreases, is the same as the case for 1 km, except the tidal stress magnitudes are lower and there is not a spike in stress magnitude for extremely thin ice shells (<3 km).
Paper: Zonal and Regional Jupiter Brightness Trends from the Hubble Outer Planet Atmospheres Legacy Program
Authors: Amy A. Simon, Michael H. Wong
Figure caption: AOI and CI for the latitudes shown in Figure 13, from the scans in Figures 5–8, using the 13 dates with observations in all four filters. (a) The NEB shows limited changes primarily in CI, while the EZ changed dramatically in both over the period of this study. (b) The NTrZ (19° north) mostly varies in CI, with 2020 as an outlier, consistent with Figure 18. (c) The NTB jet (24° north) varies in AOI and CI in a manner similar to the EZ, but with rapid changes occurring after convective outbreaks.
Paper: Zonal and Regional Jupiter Brightness Trends from the Hubble Outer Planet Atmospheres Legacy Program
Authors: Amy A. Simon, Michael H. Wong
Figure caption: Oval BA maps centered at −33°, spanning ±7° of latitude and ±15° of longitude. These maps span the UV to near-IR, using the F275W (top), F395N (middle), and FQ889N (bottom) filters. In 2021, the F395N brightness temporarily increased, even though no effects were seen in the other filters.
Paper: Zonal and Regional Jupiter Brightness Trends from the Hubble Outer Planet Atmospheres Legacy Program
Authors: Amy A. Simon, Michael H. Wong
Figure caption: The NEB from 2019 to 2022. These color strip maps (red: F631N; green: F502N; blue: F395N; identical scaling between dates) span a limited latitude range to highlight the rapid changes that occur in the NEB from 10° to 20° latitude. A dark appearance with convective streamers, such as 2019 and 2020, is common. In 2020, the overlying haze is darker from ∼20° to 35°, perhaps due to the active plume and NEB expansion.
Paper: Zonal and Regional Jupiter Brightness Trends from the Hubble Outer Planet Atmospheres Legacy Program
Authors: Amy A. Simon, Michael H. Wong
Figure caption: Brightness trends in Oval BA. Meridional scans across Oval BA center; note that several dates had to be shifted to align the core region, notably 2021. Bottom: averaging over −33° to −33.°5 to encompass the core region and over −32° to −32.°5 for the collar.
Paper: Imaging Spectroscopy: Earth and Planetary Remote Sensing with the PSI Tetracorder and Expert Systems from Rovers to EMIT and Beyond
Authors: Roger N. Clark, Gregg A. Swayze, K. Eric Livo, Philip G. Brodrick, Eldar Noe Dobrea, Srinivasan Vijayarangan, Robert O. Green, David Wettergreen, Alberto Candela, Amanda Hendrix, Carlos Pérez García-Pando, Neil C. Pearson, Melissa D. Lane, Adolfo González-Romero, Xavier Querol
Figure caption: Tetracorder results for a portion of the FRAGMENT study area in Morocco. The scene is a crop from EMIT cube emit20230206t101334_o03707_s000_l2a_rfl_b0106_v01. The salmon colored regions are mainly areas containing hematite–goethite mixtures. The green areas, jarosite, are a misidentification caused by a deficiency in the spectral libraries used: the green areas appear to be hematite–goethite mixtures with grain sizes not represented in the libraries. The white box is the area where abundances were derived and reported in Table 9. This is a Tetracorder 5.27 standard product with expert system 5.27e1. All code and spectral libraries are in the Zenodo repository (R. N. Clark 2024) and on GitHub to reproduce this image.
Paper: Imaging Spectroscopy: Earth and Planetary Remote Sensing with the PSI Tetracorder and Expert Systems from Rovers to EMIT and Beyond
Authors: Roger N. Clark, Gregg A. Swayze, K. Eric Livo, Philip G. Brodrick, Eldar Noe Dobrea, Srinivasan Vijayarangan, Robert O. Green, David Wettergreen, Alberto Candela, Amanda Hendrix, Carlos Pérez García-Pando, Neil C. Pearson, Melissa D. Lane, Adolfo González-Romero, Xavier Querol
Figure caption: Model spectra of a layered surface with larger grain sizes deeper down (red line) result in increasing band depths in spectral regions with lower absorption coefficients and match the lab data (black line). Such layered media enhances weak bands, like the 1.04 μm absorption, exactly as observed in the Saturn system. Nonlayered models (green and blue curves) cannot match the observed lab spectrum (black curve), but the layered model (red curve) shows a close match. Nonlayered models can only match band depths for some absorptions, whereas the layered model closely matches all. This new model is derived from the R. N. Clark et al. (2012) radiative transfer algorithms plus Clark & Roush (1984) Equations (18)–(24). See Table 7 for derived band depths.
Paper: Imaging Spectroscopy: Earth and Planetary Remote Sensing with the PSI Tetracorder and Expert Systems from Rovers to EMIT and Beyond
Authors: Roger N. Clark, Gregg A. Swayze, K. Eric Livo, Philip G. Brodrick, Eldar Noe Dobrea, Srinivasan Vijayarangan, Robert O. Green, David Wettergreen, Alberto Candela, Amanda Hendrix, Carlos Pérez García-Pando, Neil C. Pearson, Melissa D. Lane, Adolfo González-Romero, Xavier Querol
Figure caption: (a). Tetracorder results for two abundance models for goethite, calcite, and gypsum for the image area shown in Figures 26 and 27. This is a Tetracorder 5.27 standard product with expert system 5.27e1. All code and spectral libraries are in the Zenodo repository (R. N. Clark 2024) and on GitHub to reproduce these images. (b). Tetracorder results for two abundance models for illite/muscovite, kaolinite, and montmorillonite for the image area shown in Figures 26 and 27. This is a Tetracorder 5.27 standard product with expert system 5.27e1. All code and spectral libraries are in the Zenodo repository (R. N. Clark 2024) and on GitHub to reproduce these images.
Paper: Imaging Spectroscopy: Earth and Planetary Remote Sensing with the PSI Tetracorder and Expert Systems from Rovers to EMIT and Beyond
Authors: Roger N. Clark, Gregg A. Swayze, K. Eric Livo, Philip G. Brodrick, Eldar Noe Dobrea, Srinivasan Vijayarangan, Robert O. Green, David Wettergreen, Alberto Candela, Amanda Hendrix, Carlos Pérez García-Pando, Neil C. Pearson, Melissa D. Lane, Adolfo González-Romero, Xavier Querol
Figure caption: Tetracorder results for nano-hematite and four abundance models for the image area shown in Figures 26 and 27. This is a Tetracorder 5.27 standard product with expert system 5.27e1. All code and spectral libraries are in the Zenodo repository (R. N. Clark 2024) and on GitHub to reproduce these images.
Paper: Imaging Spectroscopy: Earth and Planetary Remote Sensing with the PSI Tetracorder and Expert Systems from Rovers to EMIT and Beyond
Authors: Roger N. Clark, Gregg A. Swayze, K. Eric Livo, Philip G. Brodrick, Eldar Noe Dobrea, Srinivasan Vijayarangan, Robert O. Green, David Wettergreen, Alberto Candela, Amanda Hendrix, Carlos Pérez García-Pando, Neil C. Pearson, Melissa D. Lane, Adolfo González-Romero, Xavier Querol
Figure caption: Tetracorder results of the eight EMIT minerals for a portion of the FRAGMENT study area in Morocco. The purple areas in the lower right corner are calcite–montmorillonie group mixtures. The scene is a crop from EMIT cube emit20230206t101334_o03707_s000_l2a_rfl_b0106_v01. This is a Tetracorder 5.27 standard product with expert system 5.27e1. All code and spectral libraries are in the Zenodo repository (R. N. Clark 2024) and on GitHub to reproduce this image.
Paper: Imaging Spectroscopy: Earth and Planetary Remote Sensing with the PSI Tetracorder and Expert Systems from Rovers to EMIT and Beyond
Authors: Roger N. Clark, Gregg A. Swayze, K. Eric Livo, Philip G. Brodrick, Eldar Noe Dobrea, Srinivasan Vijayarangan, Robert O. Green, David Wettergreen, Alberto Candela, Amanda Hendrix, Carlos Pérez García-Pando, Neil C. Pearson, Melissa D. Lane, Adolfo González-Romero, Xavier Querol
Figure caption: Example of multistream equations for reflectance, Rs, from a multilayer surface. The multistream model is coded and operational for up to three-layer models.
Paper: Imaging Spectroscopy: Earth and Planetary Remote Sensing with the PSI Tetracorder and Expert Systems from Rovers to EMIT and Beyond
Authors: Roger N. Clark, Gregg A. Swayze, K. Eric Livo, Philip G. Brodrick, Eldar Noe Dobrea, Srinivasan Vijayarangan, Robert O. Green, David Wettergreen, Alberto Candela, Amanda Hendrix, Carlos Pérez García-Pando, Neil C. Pearson, Melissa D. Lane, Adolfo González-Romero, Xavier Querol
Figure caption: Comparison of wet chemistry data from A. González-Romero et al. (2023) converted to iron oxide abundance with Model 4 abundance.
Paper: Imaging Spectroscopy: Earth and Planetary Remote Sensing with the PSI Tetracorder and Expert Systems from Rovers to EMIT and Beyond
Authors: Roger N. Clark, Gregg A. Swayze, K. Eric Livo, Philip G. Brodrick, Eldar Noe Dobrea, Srinivasan Vijayarangan, Robert O. Green, David Wettergreen, Alberto Candela, Amanda Hendrix, Carlos Pérez García-Pando, Neil C. Pearson, Melissa D. Lane, Adolfo González-Romero, Xavier Querol
Figure caption: Tetracorder Model 4 abundance results for quartz + feldspar for the image area shown in Figures 26 and 27. This is a Tetracorder 5.27 standard product with expert system 5.27e1. All code and spectral libraries are in the Zenodo repository (R. N. Clark 2024) and on GitHub to reproduce this image.
Paper: On the Sensitivity of Apophis’s 2029 Earth Approach to Small Asteroid Impacts
Authors: Paul Wiegert
Figure caption: The Opik target plane under 5 × 10−2 m s−1 (left) and 10−1 m s−1 (right) impulses. The impact cross section of the Earth in this case is 2.16 R E (Farnocchia et al. 2013) and is indicated by the blue circle. Any point inside the circle represents a collision with our planet (red crosses). An impulse of 5 × 10−2 m s−1 could just reach Earth if applied early and directed in just the right direction. Impulses of Δv ≳ 10−1 m s−1 may reach Earth over a wider range of impulse directions and timings.
Paper: On the Sensitivity of Apophis’s 2029 Earth Approach to Small Asteroid Impacts
Authors: Paul Wiegert
Figure caption: The probability that an observed on-sky displacement Δθ from the nominal Apophis ephemeris is associated with a target plane displacement Δb < 200 km for different dates within the early and late observing windows. A high probability indicates that Apophis is unlikely to have moved substantially with respect to important keyholes. A horizontal line is drawn at a probability of 0.5.
Paper: On the Sensitivity of Apophis’s 2029 Earth Approach to Small Asteroid Impacts
Authors: Paul Wiegert
Figure caption: The Opik target plane under Δv = 3 × 10−4 m s−1 (left) and 3 × 10−3 m s−1 (right) impulses. Impulses of this order are able to produce displacements of Apophis on the target plane of ∼200 km and ∼1500 km, respectively, in the vertical direction, necessary to move the asteroid into keyholes. However, only very specific (and hence very unlikely) impulses will result in keyhole entry. Some important keyholes identified by Farnocchia et al. (2013) are indicated.
Paper: On the Sensitivity of Apophis’s 2029 Earth Approach to Small Asteroid Impacts
Authors: Paul Wiegert
Figure caption: The on-sky displacement from the nominal Apophis ephemeris at the start (top left) and end (top right) of the early observing window and the start of (bottom left) and 30 days into (bottom right) the late observing window for an impulse Δv = 3 × 10−3 m s−1. Displacements are in arcseconds on the sky. The ephemeris uncertainty in Apophis’s position is less than 0.″01 in all cases, smaller than the size of the plotting symbols.
Paper: On the Sensitivity of Apophis’s 2029 Earth Approach to Small Asteroid Impacts
Authors: Paul Wiegert
Figure caption: A box plot of Δb/Δv over time. The boxes show the inner quartiles with a line at the median, while the whiskers extend across the full range of values. Impacts that occur earlier in time are more effective at moving Apophis on the target plane.
Paper: On the Sensitivity of Apophis’s 2029 Earth Approach to Small Asteroid Impacts
Authors: Paul Wiegert
Figure caption: The solar elongation of Apophis as seen from Earth during 2021–2029. The start of each year is labeled on the x-axis.
Paper: On the Sensitivity of Apophis’s 2029 Earth Approach to Small Asteroid Impacts
Authors: Paul Wiegert
Figure caption: The on-sky position of all clones for the beginning (top) and end (bottom) of the early observing window at two different magnifications. Clones that would impact Earth are indicated by crosses colored by the Δv received.
Paper: On the Sensitivity of Apophis’s 2029 Earth Approach to Small Asteroid Impacts
Authors: Paul Wiegert
Figure caption: The on-sky position of all clones for the beginning of (top) and 30 days into (bottom) the late observing window at two different magnifications. Clones that would impact Earth are indicated by crosses colored by Δv.
Paper: Light Scattering Measurements of KCl Particles as an Exoplanet Cloud Analog
Authors: Colin D. Hamill, Alexandria V. Johnson, Peter Gao
Figure caption: Size distributions and shapes of the three KCl cloud analogs used in this study. (a) Size distribution of the cloud analogs used here. The mean particle radii and total concentrations are provided in the legend. Our small KCl distribution is produced through wet generation (red), which creates a narrow size distribution. The medium (solid blue) and large (dashed blue) KCl distributions are produced through dry generation, which creates broader size distributions with larger particle number densities. (b) and (c) Scanning electron microscope images of small cubic KCl particles produced using wet generation and large cuboid and irregularly shaped KCl particles produced using dry generation, respectively.
Paper: Light Scattering Measurements of KCl Particles as an Exoplanet Cloud Analog
Authors: Colin D. Hamill, Alexandria V. Johnson, Peter Gao
Figure caption: Measured KCl scattering intensities at 532 nm (green) for the (a) small, (b) medium, and (c) large KCl size distributions and DOLP curves for 532 nm for the (d) small, (e) medium, and (f) large KCl size distributions. Positive DOLP values represent preferentially vertically polarized light, and negative DOLP values represent preferentially horizontally polarized light. Intensity values are normalized to unity at a scattering angle of 30°.
Paper: Light Scattering Measurements of KCl Particles as an Exoplanet Cloud Analog
Authors: Colin D. Hamill, Alexandria V. Johnson, Peter Gao
Figure caption: A top-down diagram and corresponding picture of ExCESS. Laser light is passed through an EOM that changes, and rapidly alternates, the polarization state of light before it is directed to the scattering region, where it impinges upon our cloud analog sample. An ND filter mitigates the intensity of scattered light entering the PMT detector. The PMT is mounted onto a stage that rotates around the scattering region where particles are flown in from above (into the page). ExCESS is a compact scattering system, contained within an 18’ × 24’ dark box, that collects measurements from 20° to 169°.
Paper: Light Scattering Measurements of KCl Particles as an Exoplanet Cloud Analog
Authors: Colin D. Hamill, Alexandria V. Johnson, Peter Gao
Figure caption: (Left) Measured PSL scattering intensity for 650 nm diameter PSLs using the 532 nm laser (green). (Right) DOLP for 650 nm diameter PSLs using the 532 nm laser (green), all compared to Mie calculations (black). Intensity values are normalized to unity at a scattering angle of 30°.
Paper: Light Scattering Measurements of KCl Particles as an Exoplanet Cloud Analog
Authors: Colin D. Hamill, Alexandria V. Johnson, Peter Gao
Figure caption: Measured KCl scattering intensities at 532 nm (green) for the (a) small, (b) medium, and (c) large KCl size distributions and DOLP curves at 532 nm for the (d) small, (e) medium, and (f) large KCl size distributions. Mie calculations for the measured size distributions and the refractive index of KCl are shown in black. Our Mie calculations use the size distributions of our three cloud analogs as measured in the laboratory (Figure 1(a)). Intensity values are normalized to unity at a scattering angle of 30°.
Paper: Validation Experiments for In Situ Ne Isotope Analysis on Mars: Gas Separation Flange Assembly Using Polyimide Membrane and Metal Seal
Authors: Yuichiro Cho, Yayoi N. Miura, Hikaru Hyuga, Kenta Shimokoshi, Kazuo Yoshioka, Hiroyuki Kurokawa, Hidenori Kumagai, Naoyoshi Iwata, Satoshi Kasahara, Haruhisa Tabata, Mari Aida, Yoshifumi Saito, Seiji Sugita
Figure caption: Shock response spectrum applied to the flange assembly in each axis and direction with the definition of the coordinates. Each curve represents the spectrum observed at the second impact.
Paper: Validation Experiments for In Situ Ne Isotope Analysis on Mars: Gas Separation Flange Assembly Using Polyimide Membrane and Metal Seal
Authors: Yuichiro Cho, Yayoi N. Miura, Hikaru Hyuga, Kenta Shimokoshi, Kazuo Yoshioka, Hiroyuki Kurokawa, Hidenori Kumagai, Naoyoshi Iwata, Satoshi Kasahara, Haruhisa Tabata, Mari Aida, Yoshifumi Saito, Seiji Sugita
Figure caption: Random vibration spectrum applied to the flanges securing the polyimide membrane (Target) and its responses (Flange normal/parallel).
Paper: Validation Experiments for In Situ Ne Isotope Analysis on Mars: Gas Separation Flange Assembly Using Polyimide Membrane and Metal Seal
Authors: Yuichiro Cho, Yayoi N. Miura, Hikaru Hyuga, Kenta Shimokoshi, Kazuo Yoshioka, Hiroyuki Kurokawa, Hidenori Kumagai, Naoyoshi Iwata, Satoshi Kasahara, Haruhisa Tabata, Mari Aida, Yoshifumi Saito, Seiji Sugita
Figure caption: (a, b) Photos of the flanges securing a polyimide sheet. (c) Schematic cross section of the flange.
Paper: Validation Experiments for In Situ Ne Isotope Analysis on Mars: Gas Separation Flange Assembly Using Polyimide Membrane and Metal Seal
Authors: Yuichiro Cho, Yayoi N. Miura, Hikaru Hyuga, Kenta Shimokoshi, Kazuo Yoshioka, Hiroyuki Kurokawa, Hidenori Kumagai, Naoyoshi Iwata, Satoshi Kasahara, Haruhisa Tabata, Mari Aida, Yoshifumi Saito, Seiji Sugita
Figure caption: Schematic gas flow diagram of Ne analysis instrument for Mars lander missions.
Paper: Validation Experiments for In Situ Ne Isotope Analysis on Mars: Gas Separation Flange Assembly Using Polyimide Membrane and Metal Seal
Authors: Yuichiro Cho, Yayoi N. Miura, Hikaru Hyuga, Kenta Shimokoshi, Kazuo Yoshioka, Hiroyuki Kurokawa, Hidenori Kumagai, Naoyoshi Iwata, Satoshi Kasahara, Haruhisa Tabata, Mari Aida, Yoshifumi Saito, Seiji Sugita
Figure caption: Summary of the results of permeation measurements.
Paper: SOHO SWAN Lyα Models Supporting LRO LAMP: 2008–2023
Authors: Wayne R. Pryor, W. Kent Tobiska, Kurt D. Retherford, Cesare Grava, Anthony Egan, Thomas K. Greathouse, G. Randall Gladstone, Eric Quémerais
Figure caption: Top panel: solar Lyα line-integrated flux used as a model input at 1 au from the Sun for 2008–2023. Second panel: rms % fit (middle) to the adjusted SWAN data for the A = 0.5 model (model 55, thin dark line) and for the model formed from using the best-fitting model for each year (thick red line). Third panel: scale factors derived for the SWAN data files (divided by 1.28) to multiply by the heliospheric model before adding a 43 R galactic background to estimate the illumination of the lunar dark side. Thin horizontal lines have been added at 0.6 and 0.8 to guide the eye. The dashed line is a linear fit to the scale factors for the best-fitting model. Fourth panel: the relative response of the SWAN detector to UV stars over the mission. Individual measurements are shown as round dots, along with a piece-by-piece fit to those measurements, preserving two apparent steps in that data. Fifth panel: revised scale factors derived for the fully degradation-adjusted SWAN data values to multiply by the heliospheric model before adding a 43 R galactic background to better estimate the illumination of the lunar dark side. The dashed line is a linear fit to the revised scale factors for the best-fitting model.