adsabs/AstroCLIMB huggingface dataset:
Paper: Hot Spot Detections and Volcanic Changes on Io during the Juno Epoch: Orbits PJ5 to PJ55
Authors: Jason E. Perry, Ashley Gerard Davies, David A. Williams, David M. Nelson
Figure caption: Temperatures derived from a single-temperature model fit to 285 Galileo NIMS spectra (A. G. Davies & G. J. Veeder 2023). Davies and Veeder also performed two-temperature, two-area fits to the same data, many of which resulted in better fits to the data. The peak in the temperature distribution is between 450 and 500 K.
Paper: Hot Spot Detections and Volcanic Changes on Io during the Juno Epoch: Orbits PJ5 to PJ55
Authors: Jason E. Perry, Ashley Gerard Davies, David A. Williams, David M. Nelson
Figure caption: (a) PJ51 JIRAM 4.8 μm observation of Tonatiuh and surrounding hot spots shows Tonatiuh in three parts with faint emission between “B” and “C”; (b) the same region in visible light and illuminated by Jupiter-shine from a composite of red and green frames from JunoCam images 57C00022, 57C00023, and 57C00024; (c) a portion of global geologic map from D. A. Williams et al. (2011) and D. A. Williams et al. (2024) covering the region. White outlines were added for the hot spots shown in (a). North is up.
Paper: Hot Spot Detections and Volcanic Changes on Io during the Juno Epoch: Orbits PJ5 to PJ55
Authors: Jason E. Perry, Ashley Gerard Davies, David A. Williams, David M. Nelson
Figure caption: Single-temperature model fit distribution for 657 hot spot detections where all of the hot spot pixel radiance values are within the JIRAM detector linear response curve (see A. Mura et al. 2020; A. G. Davies et al. 2024a), and emission angle is less than 75°. There are 109 other detections where both L- and M-band radiance measurements contain pixels out of the JIRAM detector linear response range. The highest single temperature derived is 1279 K. Not included is a single observation (Marduk A, during PJ25), which is described in the text below.
Paper: Hot Spot Detections and Volcanic Changes on Io during the Juno Epoch: Orbits PJ5 to PJ55
Authors: Jason E. Perry, Ashley Gerard Davies, David A. Williams, David M. Nelson
Figure caption: The location of 325 hot spots identified in Juno JIRAM data up to and including PJ55 by the number of orbits when the hot spot was detected. There are detections in total (excluding a pair of additional detections of Pele from PJ51 data). The number of 2305 detections by orbit for each hot spot is reflected in the size and color of the marker. The distribution of detections reflects Juno’s observing Io from a mostly northern perspective. The background map is a preliminary global base map consisting of Voyager, Galileo, and Juno JunoCam imaging data.
Paper: Hot Spot Detections and Volcanic Changes on Io during the Juno Epoch: Orbits PJ5 to PJ55
Authors: Jason E. Perry, Ashley Gerard Davies, David A. Williams, David M. Nelson
Figure caption: The sum of the spectral radiances of Tonatiuh’s three constituent hot spots has decreased with time but had been steady between orbit 41 (2022 April 9) and orbit 53 (2023 July 31) before dropping off significantly in orbit 55 (2023 October 15). The hollow data points between 2017 and 2020 are measurements that include nonlinear/saturated pixels. These values should be treated as lower limits.
Paper: Hot Spot Detections and Volcanic Changes on Io during the Juno Epoch: Orbits PJ5 to PJ55
Authors: Jason E. Perry, Ashley Gerard Davies, David A. Williams, David M. Nelson
Figure caption: Hot spot powers in bins of 25 GW for 645 hot spot detections where the emission angle is less than 75°, and the M-band and L-band radiance data are within the linear response range of the JIRAM detector. Table 6 contains an additional 121 detections in the detector “linear response” range where emission angle is greater than 75°, and a total of 811 detections including those where at least one pixel is at the top of the acceptable linear response range in the M band.
Paper: Hot Spot Detections and Volcanic Changes on Io during the Juno Epoch: Orbits PJ5 to PJ55
Authors: Jason E. Perry, Ashley Gerard Davies, David A. Williams, David M. Nelson
Figure caption: Central locations of Tonatiuh hot spots measured from JIRAM data compared to yearly average locations for the “Chalybes Regio” hot spot from Keck data. Keck locations calculated from K. de Kleer & I. de Pater (2016b) and K. de Kleer et al. (2019).
Paper: Hot Spot Detections and Volcanic Changes on Io during the Juno Epoch: Orbits PJ5 to PJ55
Authors: Jason E. Perry, Ashley Gerard Davies, David A. Williams, David M. Nelson
Figure caption: The relationship between L/M spectral radiance ratio and temperature, K, using the same emissivity at 3.5 and 4.78 μm.
Paper: Hot Spot Detections and Volcanic Changes on Io during the Juno Epoch: Orbits PJ5 to PJ55
Authors: Jason E. Perry, Ashley Gerard Davies, David A. Williams, David M. Nelson
Figure caption: (a) Galileo SSI mosaic (21ISCOLOR_01; 1999 July) showing Bosphorus Regio at visible wavelengths. At the center of the image is Emakong Patera (119.82°W, 3.33°S). (b) JIRAM 4.8 μm mosaic from 2023 October. A log stretch was used to accentuate fainter hot spots while preserving details within bright areas such as near Seth Patera. Bright streaks related to hot spots in (b) are camera artifacts.
Paper: Hot Spot Detections and Volcanic Changes on Io during the Juno Epoch: Orbits PJ5 to PJ55
Authors: Jason E. Perry, Ashley Gerard Davies, David A. Williams, David M. Nelson
Figure caption: (a) JunoCam mosaic covering Lei-Kung Fluctus. A summed product of JunoCam images from orbit 55 covers the lower right half, while JunoCam frame 57C00022 covers the upper left half. These two JunoCam observations have pixel scales of 7.8 and 1.8 km respectively. (b) JIRAM mosaic from PJ51 sequence JRM_028. The original data has a pixel scale of 8.5 km. Hot spots visible during PJ51 in JIRAM data are labeled with capital letters; lower case labels (g, i, j, o, and p) indicate hot spots that were not detected during PJ51. An outline of Lei-Kung Fluctus taken from the JunoCam data is overlaid.
Paper: Hot Spot Detections and Volcanic Changes on Io during the Juno Epoch: Orbits PJ5 to PJ55
Authors: Jason E. Perry, Ashley Gerard Davies, David A. Williams, David M. Nelson
Figure caption: Close-up (a) of the hot spots in northern Lei-Kung Fluctus observed by Juno/JIRAM in its M-band filter during orbit 55 (2023 October 15). Composite of 17 JIRAM frames with pixel scales ranging from 2.8 to 3.6 km. Hot spots seen during PJ55 are labeled. A log stretch was used to accentuate fainter hot spots while preserving details within bright areas such as at Chors Patera. This same composite is overlain on a JunoCam mosaic in the right image (b). See Figure 11(a) for more details of this mosaic.
Paper: Hot Spot Detections and Volcanic Changes on Io during the Juno Epoch: Orbits PJ5 to PJ55
Authors: Jason E. Perry, Ashley Gerard Davies, David A. Williams, David M. Nelson
Figure caption: Hot spots at Prometheus (1.7°S, 154°W) observed in a composite of six JIRAM M-band images (a) taken during orbit 55 (2023 October 15). Original data with pixel scales ranging from 3.7 to 4.5 km. (b) shows the same JIRAM composite overlaid on Galileo SSI images acquired in 1999 October and 2000 February.
Paper: Hot Spot Detections and Volcanic Changes on Io during the Juno Epoch: Orbits PJ5 to PJ55
Authors: Jason E. Perry, Ashley Gerard Davies, David A. Williams, David M. Nelson
Figure caption: Plot of L-band (3.5 μm) and M-band (4.8 μm) spectral radiance for hot spot detections below 3 GW μm−1 and where no nonlinear pixels were detected. Most detections have an L/M-band ratio below unity. Of the 573 hot spot detections plotted, 27 have an L/M-band ratio above 1. 16 of these detections are from just three hot spot sources: Zamama, Lei-Kung A, and Zal Patera C (36.8°N, 76.1°W).
Paper: Hot Spot Detections and Volcanic Changes on Io during the Juno Epoch: Orbits PJ5 to PJ55
Authors: Jason E. Perry, Ashley Gerard Davies, David A. Williams, David M. Nelson
Figure caption: (a) JIRAM 4.8 μm composite from orbit 53 (2023 July 31) showing the region around southern Lei-Kung Fluctus, Isum Patera, and Bulicame Regio. A log stretch was used to accentuate fainter hot spots while preserving details within bright areas such as near Isum Patera. Outlines of the hot spots visible within (a) are overlain a composite of Galileo SSI color imaging from 1999 July (21ISCOLOR_01) and clear-filter imaging from 1999 October (24ISSTEREO01) in the right image (b). The outline for Lei-Kung A surrounds a dark-red lineament.
Paper: Hot Spot Detections and Volcanic Changes on Io during the Juno Epoch: Orbits PJ5 to PJ55
Authors: Jason E. Perry, Ashley Gerard Davies, David A. Williams, David M. Nelson
Figure caption: Close-up (a) of the region around Seth Patera observed by Juno/JIRAM in its M-band filter during orbit 55 (2023 October 15). Composite of six JIRAM frames with pixel scales ranging from 3.7 to 4.5 km. A log stretch was used to accentuate fainter thermal structures while preserving details within bright areas within the Seth flow field. This same composite is overlain on a Galileo SSI mosaic (21ISCOLOR_01; 1999 July) in the right image (b). Thin, filament-like streaks above the hot spots in the JIRAM data are a camera artifact.
Paper: Hot Spot Detections and Volcanic Changes on Io during the Juno Epoch: Orbits PJ5 to PJ55
Authors: Jason E. Perry, Ashley Gerard Davies, David A. Williams, David M. Nelson
Figure caption: (a) JIRAM 4.8 μm composite from 2023 October showing the multiple hot spots at Volund and North Volund and the single hot spot at Zamama. This same composite is overlain on a JunoCam observation from orbit 55 (55C00028) in the right image (b).
Paper: Hot Spot Detections and Volcanic Changes on Io during the Juno Epoch: Orbits PJ5 to PJ55
Authors: Jason E. Perry, Ashley Gerard Davies, David A. Williams, David M. Nelson
Figure caption: Surface changes observed at Volund and North Volund between Galileo SSI (a; 1999 October) and JunoCam (b; 2023 October), showing significant changes in the flow field since Galileo. The original Galileo data have a pixel scale of 1.45 km, while the JunoCam image has a pixel scale of 8.4 km.
Paper: Hot Spot Detections and Volcanic Changes on Io during the Juno Epoch: Orbits PJ5 to PJ55
Authors: Jason E. Perry, Ashley Gerard Davies, David A. Williams, David M. Nelson
Figure caption: Observations of Amaterasu Patera in visible light, L band (3.5 μm), and M band (4.8 μm) from Voyager, Galileo, and Juno. Despite its history of vigorous thermal emission episodes reported over the last 20 yr (e.g., C. Cantrall et al. 2018), its visible-light appearance has remained constant over the last 45 yr. The floor appears uniformly dark, although subtle variations, like a darkening trend from east to west and a debris flow on the eastern margin, are observed in the Juno/JunoCam image from orbit 57. Pixel scales of the images shown here vary: 1.2 km pixel–1 for the Voyager 1/ISS observation, 6.7 km for Galileo/SSI, and 2.2–25.5 km for Juno/JunoCam. Near-infrared observations from Juno/JIRAM from orbit 51 (2023 May) during a major brightening show the majority of the thermal emission emanates from the center of the patera, with thermal emission decreasing toward the margins, the opposite of the pattern reported using the same data in A. Mura et al. (2024b). Pixel scale is 13.1 km. Near-infrared observations from Juno/JIRAM from orbit 55 (2023 October) show a similar pattern in the M-band data, while the L-band data show more spatial variation, with the eastern and western ends of the patera brighter than the rest of the floor. A debris flow along the straight northeastern margin interrupts thermal emission in this region, as seen in the L-band data from orbit 55. Dark spots in the center of the floor in the L-band data are likely due to noise. Pixel scale of the orbit 55 JIRAM data is 6.9 km.
Paper: Hot Spot Detections and Volcanic Changes on Io during the Juno Epoch: Orbits PJ5 to PJ55
Authors: Jason E. Perry, Ashley Gerard Davies, David A. Williams, David M. Nelson
Figure caption: Comparison of hot spot detections in JIRAM data from orbits PJ41 to PJ49 inclusive, reflecting the preponderance of observations of the northern hemisphere. Perry et al. detections (this publication) are separated into four classes. Class 1 contains detections in both L and M bands where the emission angle e is <70°. Class 2 is where detections are in one band and e <70°. Class 3 contains dual-band detections where e >70°. Class 4 contains single band detections where e >70°.
Paper: Hot Spot Detections and Volcanic Changes on Io during the Juno Epoch: Orbits PJ5 to PJ55
Authors: Jason E. Perry, Ashley Gerard Davies, David A. Williams, David M. Nelson
Figure caption: A before (a) and after (b) example of the residual flat field applied to images with exposure times of less than 2 ms. The image used in this example is JIR_IMG_RDR_2023288T064806_V01 and shows Lei-Kung K on the left and Chors Patera on the right. Removal of this vertical striping improves the ability to interpret subtle variations in brightness, for example the brightness variations across the floor of Chors Patera.
Paper: Hot Spot Detections and Volcanic Changes on Io during the Juno Epoch: Orbits PJ5 to PJ55
Authors: Jason E. Perry, Ashley Gerard Davies, David A. Williams, David M. Nelson
Figure caption: Temperatures derived by A. Mura et al. (2024a) from a selection of detections during orbits PJ41 to PJ49.
Paper: Hot Spot Detections and Volcanic Changes on Io during the Juno Epoch: Orbits PJ5 to PJ55
Authors: Jason E. Perry, Ashley Gerard Davies, David A. Williams, David M. Nelson
Figure caption: Derived temperatures from a subset of detections to match the parameters of A. Mura et al. (2024a).
Paper: Fully Coherent Model of Dynamics around Binary Asteroids: Application to Didymos and the DART Impact
Authors: Alex J. Meyer, Daniel J. Scheeres
Figure caption: Scatter plots of the time-averaged (a) inclination as a function of eccentricity and (b) semimajor axis as a function of eccentricity for the debris simulations. The duration of each ejecta particle as a function of particle radius (c) and the time-averaged eccentricity as a function of particle radius (d).
Paper: Fully Coherent Model of Dynamics around Binary Asteroids: Application to Didymos and the DART Impact
Authors: Alex J. Meyer, Daniel J. Scheeres
Figure caption: The eccentricities of Dimorphos and the spacecraft trajectory over time. We see that fluctuations in the binary mutual orbit eccentricity also manifest as a strong perturbation on the spacecraft, eventually pushing the spacecraft onto an unstable orbit, resulting in an impact onto the primary.
Paper: Fully Coherent Model of Dynamics around Binary Asteroids: Application to Didymos and the DART Impact
Authors: Alex J. Meyer, Daniel J. Scheeres
Figure caption: Plots of examples for (a) direct interior, (b) retrograde interior, (c) direct exterior, (d) retrograde exterior, (e) circumsecondary, and (f) L4 point orbits. Only the interior orbits remain stable in the perturbed system.
Paper: Fully Coherent Model of Dynamics around Binary Asteroids: Application to Didymos and the DART Impact
Authors: Alex J. Meyer, Daniel J. Scheeres
Figure caption: Diagram of the dynamical system, showing the binary asteroid, Sun, and particle, along with the relevant vectors.
Paper: Fully Coherent Model of Dynamics around Binary Asteroids: Application to Didymos and the DART Impact
Authors: Alex J. Meyer, Daniel J. Scheeres
Figure caption: Scatter plot of the duration of each ejecta particle as a function of its initial velocity relative to Dimorphos. We group the simulations into four categories depending on their ultimate fate.
Paper: Fully Coherent Model of Dynamics around Binary Asteroids: Application to Didymos and the DART Impact
Authors: Alex J. Meyer, Daniel J. Scheeres
Figure caption: The stroboscopic orbit period (top) and separation distance (bottom) of the Didymos mutual orbit over 1 yr postimpact.
Paper: Fully Coherent Model of Dynamics around Binary Asteroids: Application to Didymos and the DART Impact
Authors: Alex J. Meyer, Daniel J. Scheeres
Figure caption: The orbit roll (top), pitch (middle), and yaw (bottom) of Dimorphos relative to the rotating Hill frame over 1 yr.
Paper: Fully Coherent Model of Dynamics around Binary Asteroids: Application to Didymos and the DART Impact
Authors: Alex J. Meyer, Daniel J. Scheeres
Figure caption: Terminator orbits shown in the rotating Sun frame, showing (a) stable and (b) unstable cases. The unstable orbit is in a 2:1 resonance with Dimorphos.
Paper: The Spin Zone: Synchronously and Asynchronously Rotating Land Planets Have Spectral Differences in Transmission
Authors: Nicholas Scarsdale, C. E. Harman, Thomas J. Fauchez
Figure caption: The spectrum of each simulation in our explored parameter space. Each has the same composition (N2-dominated, trace CO2 and H2O; Table 2). Each box shows the synchronous and 1 day rotator cases for different instellation values, which are printed in the legend. Up to 1.66 S⊕, the transit spectra are distinguishable. In warmer cases, the differences disappear.
Paper: The Spin Zone: Synchronously and Asynchronously Rotating Land Planets Have Spectral Differences in Transmission
Authors: Nicholas Scarsdale, C. E. Harman, Thomas J. Fauchez
Figure caption: Convergence diagnostics for our simulations. (a) The pressure–temperature profiles of each simulation at the substellar point (or longitude = 0 for the 1 day rotators). The region where the HITRAN line list is inadequate is highlighted in red. (b) The average surface temperature at each time point of our synchronously rotating models, shown for each irradiation step. (c) The energy balance of each simulation. A value of 0 would indicate a perfectly equilibrated simulation. The hottest synchronous rotators display nonzero net fluxes. But values lower than ∼0.75 W m−2 are sufficient to be considered converged (although see Section 2.2).
Paper: The Spin Zone: Synchronously and Asynchronously Rotating Land Planets Have Spectral Differences in Transmission
Authors: Nicholas Scarsdale, C. E. Harman, Thomas J. Fauchez
Figure caption: The terminator cloud properties of our simulations as a function of latitude. The left and right sides correspond to the morning and evening terminators, respectively. (a) and (b) The fractional cloud cover of each cell for the synchronous (a) and 1 day (b) rotators. (c) and (d) The height of the cloud top for the synchronous (c) and 1 day (d) rotators in millibars. Higher-pressure (lower-altitude) clouds are radially further from the center.
Paper: The Spin Zone: Synchronously and Asynchronously Rotating Land Planets Have Spectral Differences in Transmission
Authors: Nicholas Scarsdale, C. E. Harman, Thomas J. Fauchez
Figure caption: The mean pressure–humidity profile for each simulation. Envelopes span the minimum and maximum specific humidity at each pressure level. Unlike in other figures, the color scheme is the same for the synchronous and 1 day cases to enable easier comparison between instellations, and the two synchronization states are indicated by line style (solid lines for synchronous, dashed lines for 1 day).The transition to nearly subsaturated atmospheres occurs at lower irradiation for the synchronous rotators than the 1 day rotators.
Paper: The Spin Zone: Synchronously and Asynchronously Rotating Land Planets Have Spectral Differences in Transmission
Authors: Nicholas Scarsdale, C. E. Harman, Thomas J. Fauchez
Figure caption: Diagnostic maps of the representative 0.8 S⊕ and 1.25 S⊕ simulation instances, with both synchronization states shown. (a)–(d): ground temperature. Synchronous rotators are dominated by dayside-to-nightside variation and 1 day rotators by latitudinal variation. (e)–(h): relative humidity at 500 mbar. (i)–(l): cloud cover. The cooler simulations are much cloudier. (m)–(p): cloud-top height in millibars. Note that the left and right halves of the plot use different color bars.
Paper: The Spin Zone: Synchronously and Asynchronously Rotating Land Planets Have Spectral Differences in Transmission
Authors: Nicholas Scarsdale, C. E. Harman, Thomas J. Fauchez
Figure caption: Slices through the four coolest simulation atmospheres at 100 mbar. Top: synchronous rotators. Bottom: 1 day rotators.
Paper: Spectroscopic Mapping of Callisto with HST/STIS and Implications for its Surface Composition
Authors: M. Ryleigh Davis, Samantha K. Trumbo, Michael E. Brown, Mathew Belyakov
Figure caption: Example HST spectra from 200 to 1000 nm of a few representative regions on Callisto. The location of each spectrum is indicated by a numbered circle on the map (a) with a corresponding color to the plotted spectrum (b). Each spectrum is calculated by averaging the UV and visible pixels that intersect a circle with a radius of 2° about the point of interest, and combining the resulting UV and visible spectra. Spectra are normalized to unity at 1000 nm and offset by increments of 0.15 for clarity. These spectra are generally smoothly varying, and uncertainties can be estimated from the scatter in the data. Panels (c)–(h) show many of the individual spectral features discussed in this paper, with band centers indicated by the vertical dashed gray lines. Colors indicate the corresponding spectrum from panel (b) used to highlight each individual spectral feature. Polynomial continuum fits are shown with black dashed lines, and continuum-divided features are included above each spectrum. In panel (f), the Asgard spectrum (5, blue) is included to highlight the difference between a typical Callisto spectrum that does not have a 275 nm absorption edge and one that does (3, yellow). The large ringed basins Valhalla, Asgard, Utgard, and Adlinda are outlined with black dashed lines and labeled on the map in panel (a) along with the bright young impact craters Heimdall and Lofn and their ejecta. The base map is the high-resolution USGS global mosaic created from Voyager and Galileo images (USGS Astrogeology Science Center 2013).
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: Range of Hapke model parameter values for the different morphological units in the study areas. The top row presents the results for area I, the center row is area II, and the bottom row is area III. The left column displays single-scattering albedo values, the center column displays surface roughness values, and the right column displays single-particle scattering function amplitude values. The area II data are divided into groups. Light blue represents parameter values from the top, lower data quality, portion of the image (see Figures 7– 9). Dark blue represents parameter values from the bottom, higher data quality, portion of the image (see Figures 7– 9). The bars have been offset to note the overlap.
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: The MLC cluster unit maps for study areas I (top), II (center), and III (bottom). The first column shows gray-scale reflectance images of each area, the central column shows the MLC cluster unit maps with morphologic boundaries shown in white, and the right column is a transparent overlay of the MLC cluster unit maps on top of the reflectance images. Area II has been divided into two portions (top with lower data quality, bottom with higher data quality). The center column shows no overlap in coverage, and the right column has the overlap shown in gray scale. Each of these portions was examined independently. For the central and right columns: blue = basin floor MLC cluster, orange = flow MLC cluster, magenta = hollow MLC cluster, green = halo MLC cluster. Refer to Table 3 for details on the parameter value ranges for each cluster unit.