adsabs/AstroCLIMB huggingface dataset:
Paper: Modeling Ice and Dust in Comet C/2017 K2 (Pan-STARRS)’s Coma
Authors: Megan Firgard, Theodore Kareta
Figure caption: The three epochs of NIR reflectance spectra of K2 are shown as black unfilled dots with gray error bars. The data sets are offset vertically along the y-axis, normalized identically, and listed in chronological order from top to bottom. The top spectrum was taken on 2021 April 30 at the NASA IRTF (T. Kareta et al. 2021a) with the SpeX instrument; the middle spectrum was taken on 2022 June 4 at the LDT with the NIHTS instrument; and the bottom spectrum was taken on 2022 September 5 at the Gemini South Telescope with the F2 instrument. The three gray shaded, vertical regions at 1.4, 1.8, and 2.3 μm are areas of high telluric absorption. We clip out most of the data in these regions, except for in the high-altitude IRTF data, where we only exclude the data in the 1.8 and 2.3 μm bands and fit our models through the 1.4 μm band. The regions of interest are the water ice absorption bands at 1.5 and 2.0 μm, which are most present in the 2021 April data and are discussed at length in the text.
Paper: Detection of New Auroral Emissions at Io and Implications for Its Interaction with the Plasma Torus
Authors: Zachariah Milby, Katherine de Kleer, Carl Schmidt
Figure caption: Relationship between Io’s 630.0 nm auroral brightness and distance from the centrifugal equator. The gray lines show fits of both Equation (4) with the scale height fixed at 0.77RJ and a simple constant model. The shaded regions show the uncertainty in the fit (for Equation (4) this corresponds to the amplitude n0; for the constant this corresponds to the uncertainty in its value). These data suggest that the inherent variability of torus electron density with both longitude and on secular timescales may be on the order of factors of 2 to 3. However, the small quantity of observed brightnesses and the gaps in sampling the distance from the centrifugal equator prevent firm conclusions regarding the connection between brightness and upstream plasma density. (Note that the reported uncertainties are from the weighted fit and do not reflect the standard deviation of the data.)(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Detection of New Auroral Emissions at Io and Implications for Its Interaction with the Plasma Torus
Authors: Zachariah Milby, Katherine de Kleer, Carl Schmidt
Figure caption: Dependence of the 630.0 nm/557.7 nm [O I] brightness ratio on electron energy and density assuming electron impact on an atmospheric column of atomic oxygen. The dashed vertical black lines show the typical electron density range of 1200 to 3800 cm−3 experienced by Io through one rotation of Jupiter’s magnetosphere (F. Bagenal & V. Dols 2020). The thick black line shows our average observed ratio of 13.64 ± 0.13. This brightness ratio for electron impact on atomic oxygen is effectively insensitive to the range of typical electron densities, making it diagnostic of the energy of the exciting electrons. However, electron impact on atomic oxygen cannot account for the observed O I 777.4 and 844.6 nm brightnesses. Colored lines highlight contours at a spacing of 0.1 dex. Calculated using CHIANTI v10.1 (K. P. Dere et al. 1997, 2023).(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Detection of New Auroral Emissions at Io and Implications for Its Interaction with the Plasma Torus
Authors: Zachariah Milby, Katherine de Kleer, Carl Schmidt
Figure caption: Best-fit emission model column densities for O (top), O2 as a proxy for SO (middle), and SO2 (bottom). These results assume only direct excitation of O and dissociative excitation of SO and SO2 and do not include any recombination processes. We used a Maxwellian electron distribution centered at 5 eV with a density of 2500 cm−3. Line styles differentiate between the five observation nights as notated in the bottom panel. The variance in the O2 column densities is physically meaningful, but the absolute magnitude is not necessarily representative of the SO column density (see the discussion in Section 4.1).(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Detection of New Auroral Emissions at Io and Implications for Its Interaction with the Plasma Torus
Authors: Zachariah Milby, Katherine de Kleer, Carl Schmidt
Figure caption: Dependence of the 671.6 nm/673.1 nm [S II] brightness ratio on electron number density assuming excitation by 5 eV electrons. The dashed lines show the low- and high-density limits defined in Equations (5) and (6). The solid gray line and shaded region show the observed ratio of 0.40 ± 0.03, which we calculated as the weighted average of the brightnesses in Table 2. Figure based on D. E. Osterbrock & G. J. Ferland (2006), Figure 5.8. Calculated using CHIANTI v10.1 (K. P. Dere et al. 1997, 2023).(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Detection of New Auroral Emissions at Io and Implications for Its Interaction with the Plasma Torus
Authors: Zachariah Milby, Katherine de Kleer, Carl Schmidt
Figure caption: Images of each Cassini/ISS filter and filter combination containing discrete auroral emissions identified in the HIRES spectra. Labels in the upper left corner indicate the filter or filter combination. Table 5 lists the individual file names and observation time for the images displayed for each filter.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Detection of New Auroral Emissions at Io and Implications for Its Interaction with the Plasma Torus
Authors: Zachariah Milby, Katherine de Kleer, Carl Schmidt
Figure caption: Cassini/ISS imaging filter sequence displayed in Figure 5 sorted by the exposure midpoint time (see Table 5) of each image relative to eclipse ingress, which occurred at 2001 January 5 11:03 UTC.
Paper: Detection of New Auroral Emissions at Io and Implications for Its Interaction with the Plasma Torus
Authors: Zachariah Milby, Katherine de Kleer, Carl Schmidt
Figure caption: Best-fit emission model O/SO2 mixing ratio calculated from the column densities in Figure 8. Points with lower uncertainty bounds intercepting zero are cut off by the lower axis limit. Though the mixing ratio just after eclipse ingress is typically about 10%, it can vary by more than an order of magnitude.
Paper: Leveraging Ceres to Gain Insights into the Candidate Ocean Worlds of Umbriel and Oberon That Orbit Uranus
Authors: Jennifer E. C. Scully, C. Adeene Denton, Julie C. Castillo-Rogez, Michael M. Sori, Erin J. Leonard, Chloe Beddingfield, Richard Cartwright, Catherine M. Elder, Karl L. Mitchell, Tom A. Nordheim
Figure caption: Views of Wunda crater, Umbriel, and Occator crater, Ceres. Panel (a) shows Wunda crater in an oblique view (indicated by “W”), as well as the central peak in Vuver crater (indicated by “V”). Image number 2684006 is ∼4 km pixel−1. Panel (b) shows Wunda crater, Vuver crater, and two apparently bright patches (indicated by “?”). Image number 2682545 is ∼8 km pixel−1. Panel (c) shows Occator’s faculae in plan view, in image number 36633, which is ∼1 km pixel−1. Panels (d)−(f) show an oblique view of Occator crater (indicated by “O”) in image number 37568, which is ∼400 m pixel−1. In panel (d), the stretch of the image results in the faculae appearing to take up roughly half of the crater interior. Altering the stretch decreases the apparent area of the faculae in panel (e), until a more accurate approximation of the faculae area is shown in panel (f), which has the stretch with the highest maximum DN. Panels (g)−(i) show an oblique view of Wunda crater (indicated by “W”) in image number 2684004, which is ∼4 km pixel−1. Panel (g) shows the one saturated pixel (white square), while panels (h) and (i) show the image with different stretches, as detailed in the text.
Paper: Leveraging Ceres to Gain Insights into the Candidate Ocean Worlds of Umbriel and Oberon That Orbit Uranus
Authors: Jennifer E. C. Scully, C. Adeene Denton, Julie C. Castillo-Rogez, Michael M. Sori, Erin J. Leonard, Chloe Beddingfield, Richard Cartwright, Catherine M. Elder, Karl L. Mitchell, Tom A. Nordheim
Figure caption: Views of Ahuna Mons, Ceres; the mountain on Oberon; and Aeneas crater on Dione. Panel (a) shows a limb view of Ahuna Mons in image number 36633, which is ∼1 km pixel−1. The white box shows the approximate location of panels (b) and (c). Panel (b) is an oblique view of Ahuna Mons, adapted from O. Ruesch et al. (2016). Extensional features can be seen on the top of the mons, along with the steeply sloping talus flanks. The base of Ahuna Mons is ∼17 km wide, and the spatial resolution of the view is ∼135 m pixel−1. Panel (c) is a geomorphic map of Ahuna Mons, highlighting the talus collar (green) and summit (pink), adapted from O. Ruesch et al. (2016). Panel (d) is a view of Oberon’s mountain in image number 2683629, which is ∼5 km pixel−1. The white box shows the location of panel (e). Panel (e) is a smaller portion of image number 2683629, which illustrates how the aspect ratio was calculated via measuring the height (shorter white line) and basal width (longer white line). Panel (f) shows Aeneas crater on Dione, which has a diameter of ∼175 km. The color bar shows heights. Image adapted from J. M. Moore et al. (2004).
Paper: Leveraging Ceres to Gain Insights into the Candidate Ocean Worlds of Umbriel and Oberon That Orbit Uranus
Authors: Jennifer E. C. Scully, C. Adeene Denton, Julie C. Castillo-Rogez, Michael M. Sori, Erin J. Leonard, Chloe Beddingfield, Richard Cartwright, Catherine M. Elder, Karl L. Mitchell, Tom A. Nordheim
Figure caption: Predicted lighting conditions on Umbriel and Oberon during example flybys in an example UOP tour included in the UOP Concept Study for the 2023–2032 Decadal Survey (A. Simon et al. 2021), viewed using NASA’s “Eyes on the Solar System” (https://eyes.nasa.gov/apps/solar system/#/home). The previously unobserved portions of the surfaces are in gray. (a) Predicted lighting conditions on Umbriel during an example flyby on 06/22/47. Wunda crater is the bright patch in the middle of the image. (b) Predicted lighting conditions on Umbriel during an example flyby on 10/03/47. Wunda crater is the bright patch in the top center of the image. (c) Predicted lighting conditions on Oberon during an example flyby on 07/28/47. The mountain on Oberon is within the previously imaged area on the right. (d) Predicted lighting conditions on Oberon during an example flyby on 12/09/47. The mountain on Oberon is within the previously imaged area on the right.
Paper: Crater Retention Timescales of Brain Coral Terrain Record Past Climatic Change on Mars
Authors: Alexander M. Morgan, Eldar Z. Noe Dobrea, Kyle A. Pearson, Alphan Altinok
Figure caption: CSFDs for the four study areas fit to the W. K. Hartmann & I. J. Daubar (2016) production function. Absolute ages use the G. G. Michael (2013) iteration of the W. K. Hartmann (2005) chronology function. Blue squares are fresh craters, red triangles are fresh and degraded craters, and green circles are all craters. Unfilled symbols are those data points that do not lie along segments that match the production function.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Crater Retention Timescales of Brain Coral Terrain Record Past Climatic Change on Mars
Authors: Alexander M. Morgan, Eldar Z. Noe Dobrea, Kyle A. Pearson, Alphan Altinok
Figure caption: Examples of the three degradation classes of craters. Fresh craters contain minimal infill and have a clearly defined rim. Moderately degraded craters have either some infill or a crater rim that appears modified by brain coral terrain cells. Heavily degraded craters are mostly to completely infilled by brain coral terrain or flat-topped deposits (“oyster shells” as termed by N. Mangold 2003). All frames are at the same scale; north is up. Frame (a) is clipped from HiRISE image ESP_044717_2205; all other frames are clipped from HiRISE image ESP_044717_2205. Illumination is from the left.
Paper: Crater Retention Timescales of Brain Coral Terrain Record Past Climatic Change on Mars
Authors: Alexander M. Morgan, Eldar Z. Noe Dobrea, Kyle A. Pearson, Alphan Altinok
Figure caption: Example crater plot with artificial data illustrating the interpretation of two CSFDs. The surface marked with green squares formed at time t3, but some resurfacing processes have since begun that have preferentially removed craters smaller than D1. Because the curve does not resteepen, this process continues to present. The surface marked with red triangles formed at t5. Sometime after t5, a process of unknown duration preferentially removed craters smaller than D2. The timing of the onset of this resurfacing process is not knowable from the CSFD, but it ended around t4 when craters began to accumulate along the production function. See Section 2 of the text for further discussion. Figure adapted from N. Mangold (2003).
Paper: Crater Retention Timescales of Brain Coral Terrain Record Past Climatic Change on Mars
Authors: Alexander M. Morgan, Eldar Z. Noe Dobrea, Kyle A. Pearson, Alphan Altinok
Figure caption: Examples of (a) CCF, (b) LDA, (c) LVF, and (d) plains, the four landform types with surficial brain coral terrain that were examined in this study. Arrows indicate the downslope direction. Images are from the Context Camera mosaic (J. L. Dickson et al. 2024). Frames centered on (16.68°E, 42.02°N), (24.35°E, 38.68°N), (34.55°E, 41.0°N), and (176.52°E, 41.99°N). All frames are at the same scale; north is up. Illumination is from the left in all frames.
Paper: Crater Retention Timescales of Brain Coral Terrain Record Past Climatic Change on Mars
Authors: Alexander M. Morgan, Eldar Z. Noe Dobrea, Kyle A. Pearson, Alphan Altinok
Figure caption: Comparison of deep learning detections of brain coral (red) compared to manually mapped brain coral (green). HiRISE image PSP_002046_2180_RED centered on 37.744°N, 24.337°E. The image is 7.5 km across, north is up.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Crater Retention Timescales of Brain Coral Terrain Record Past Climatic Change on Mars
Authors: Alexander M. Morgan, Eldar Z. Noe Dobrea, Kyle A. Pearson, Alphan Altinok
Figure caption: Location of the three study areas. Stereographic projection centered on the north pole. Dots indicate the 158 HiRISE images containing mapped brain coral. The background is MOLA topography, where white indicates high elevation.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Simulating the (99942) Apophis Earth Flyby Using a Contact Binary Model
Authors: Hai-Shuo Wang, Paul Sánchez, D.J. Scheeres
Figure caption: Large component (left) and surface (right) mass shifts of the DPC-NB model varying with close encounter trajectory. White blocks indicate system breakup scenarios, where the two cores of the contact binary separate by more than 5 times their initial mutual distance. Orange circles represent the case of Apophis, with q ∼ 6RE and V∞ ∼ 6 km s−1. The orange vertical line shows the disruption distance from theoretical studies.
Paper: Simulating the (99942) Apophis Earth Flyby Using a Contact Binary Model
Authors: Hai-Shuo Wang, Paul Sánchez, D.J. Scheeres
Figure caption: The left panel shows the large component shift as a function of the neck size ratio α for various boulder size ratios η, with a critical elbow point marking the survival condition of a contact binary under weak perturbations, indicating an expected large component shift of about 0﹩\mathop{.}\limits^{\unicode{x000b0}}﹩01. The right panel illustrates the surface mass shift as a function of the neck size ratio α for different boulder size ratios η, showing that the largest surface mass shift is on the centimeter scale.
Paper: Simulating the (99942) Apophis Earth Flyby Using a Contact Binary Model
Authors: Hai-Shuo Wang, Paul Sánchez, D.J. Scheeres
Figure caption: The left panel shows the variation of the critical friction angle ϕc as a function of the orientations (φ, θ). The right panel shows the variation of the critical friction angle ϕc as a function of the mass ratio m1/m2 while φ = θ = 0°, showing that lower friction angles are sufficient to maintain stability across a broad range of configurations.
Paper: Simulating the (99942) Apophis Earth Flyby Using a Contact Binary Model
Authors: Hai-Shuo Wang, Paul Sánchez, D.J. Scheeres
Figure caption: The tensile strength between grains as a function of the cohesive strength of aggregates and the internal friction angle (ϕi). The relationship is approximately proportional.
Paper: Simulating the (99942) Apophis Earth Flyby Using a Contact Binary Model
Authors: Hai-Shuo Wang, Paul Sánchez, D.J. Scheeres
Figure caption: The top row shows an example deformation with trajectory parameters q = 1.5RE and V∞ = 8 km s−1, highlighted in black in Figure 11. The bottom row shows the an example disruption with trajectory parameters q = 1RE and V∞ = 4 km s−1, highlighted in black in Figure 11.
Paper: Simulating the (99942) Apophis Earth Flyby Using a Contact Binary Model
Authors: Hai-Shuo Wang, Paul Sánchez, D.J. Scheeres
Figure caption: Diagram of the forces acting on the two bodies in the DPM during Apophis’ close encounter with Earth.
Paper: Simulating the (99942) Apophis Earth Flyby Using a Contact Binary Model
Authors: Hai-Shuo Wang, Paul Sánchez, D.J. Scheeres
Figure caption: N-body dynamics of the contact binary asteroid in the Apophis center-of-mass inertial coordinate system. Here, q* represents the component positions in the inertial frame ﹩{ \mathcal O }﹩, while r* denotes their relative positions in the center-of-mass frame.
Paper: Evolution of Mercury’s Volatile-bearing Crust within Raditladi Basin
Authors: Deborah L. Domingue, John R. Weirich, J. Alexis P. Rodriguez, Samuel W. Courville, Frank C. Chuang, Matthew D. Richardson, Bryan J. Travis, Eric E. Palmer, Mario Zarroca
Figure caption: Areas I, II, and III (left to right columns) displaying the reflectance image (top row) single-scattering albedo map from the three-parameter solution (bottom row). The blue lines in the reflectance image (top row) display the following boundaries: between the peak ring and the glacial flow, between the peak ring and the basin floor, or between the glacial flow and the basin floor. These lines are repeated in black in the parameter maps. The yellow arrows point to examples of hollows within either the glacial flow or the summits of the peak ring. The red arrows point to examples of high-reflectance materials along the peak walls, and the blue arrows point to examples of moderate-reflectance materials along the peak walls. The thick red line in the area II parameter map shows the demarcation between data quality regions that are apparent in all the parameter maps for the three-parameter solutions, with more extensive angular coverage available below the thick red line. The thinner red lines in the area I maps display regions on the peak walls with high single-scattering albedo properties but do not display high-reflectance values in the image of the area.
Paper: Evolution of Mercury’s Volatile-bearing Crust within Raditladi Basin
Authors: Deborah L. Domingue, John R. Weirich, J. Alexis P. Rodriguez, Samuel W. Courville, Frank C. Chuang, Matthew D. Richardson, Bryan J. Travis, Eric E. Palmer, Mario Zarroca
Figure caption: Areas I, II, and III (left to right columns) displaying the reflectance image (top row) and the surface roughness (﹩\bar{\theta }﹩) map from the three-parameter solution (bottom row). The blue lines in the reflectance image (top row) display the following boundaries: between the peak ring and the glacial flow, between the peak ring and the basin floor, or between the glacial flow and the basin floor. These lines are repeated in black in the parameter maps. The yellow arrows point to examples of hollows within either the glacial flow, the peak walls, or the summits of the peak ring. The black arrows point to examples of high-reflectance materials along the peak walls, and the blue arrows point to examples of moderate-reflectance materials along the peak walls The thick red line in the area II parameter map shows the demarcation between data quality regions that are apparent in all the parameter maps for the three-parameter solutions, with more extensive angular coverage available below the thick red line. The thinner red lines in the area I maps display regions on the peak walls with high single-scattering albedo properties but do not display high-reflectance values in the image of the area (top). These regions appear as some of the roughest regions in area I.
Paper: Evolution of Mercury’s Volatile-bearing Crust within Raditladi Basin
Authors: Deborah L. Domingue, John R. Weirich, J. Alexis P. Rodriguez, Samuel W. Courville, Frank C. Chuang, Matthew D. Richardson, Bryan J. Travis, Eric E. Palmer, Mario Zarroca
Figure caption: Hapke’s “hockey-stick” relationship (B. Hapke 2012b) between the scattering function amplitude (b) and the scattering function partition (c) parameters used in the modeling of the Raditladi regions compared to other Mercury studies and the laboratory measurements of A. McGuire & B. Hapke (1995) and the remodeling of those measurements by B. Hartman & D. Domingue (1998). The results for different morphological categories in the study regions are shown in magenta. The area maps along the side of the graph denote the different morphological units examined. Unit 1 in all areas represents the basin floor. Unit 2 represents the flow-like features in areas I and III; in area II, it represents a double crater with possible ejecta. Unit 3 represents the peak ring walls in area I, flow-like features in area II, and hollows fields in area III. Unit 4 represents hollows in area I and peak ring walls in areas II and III. Unit 5 represents interpeak terrains in area I and hollows in areas II and III. Note that the “c values” have been converted to match the formalism in B. Hapke (2012b) due to the different formulation of the single-particle scattering function, as discussed in Section 4. This diagram has been converted to match that in B. Hapke (2012b).
Paper: Evolution of Mercury’s Volatile-bearing Crust within Raditladi Basin
Authors: Deborah L. Domingue, John R. Weirich, J. Alexis P. Rodriguez, Samuel W. Courville, Frank C. Chuang, Matthew D. Richardson, Bryan J. Travis, Eric E. Palmer, Mario Zarroca
Figure caption: Areas I, II, and III (left to right columns) displaying the reflectance image (top row) single particle-scattering function amplitude, b, map from the three-parameter solution (bottom row). The blue lines in the reflectance image (top row) display the following boundaries: between the peak ring and the glacial flow, between the peak ring and the basin floor, or between the glacial flow and the basin floor. These lines are repeated in black in the parameter maps. The yellow arrows point to examples of hollows within either the glacial flow or the summits of the peak ring. The red arrows point to examples of high-reflectance materials along the peak walls, and the black arrows point to examples of moderate-reflectance materials along the peak walls. The thick red line in the area II parameter map shows the demarcation between data quality regions that are apparent in all the parameter maps for the three-parameter solutions, with more extensive angular coverage available below the thick red line. The thinner red lines in the area I maps display regions on the peak walls with high single-scattering albedo properties but do not display high-reflectance values in the image of the area (top). These regions also show anomalously low b values for this area.