adsabs/AstroCLIMB huggingface dataset:
Paper: Lunar Crustal Magnetization Sourced via the Delivery of Iron-rich Ejecta from Basin-forming Impacts
Authors: R. I. Citron, L. L. Hood, S. T. Stewart
Figure caption: Dependence of ejecta patterns on impact angle for a 50 km diameter projectile. As in Figure A1 but with fixed D = 50 km, v = 16 km s−1, and with each column representing a different impact angle (θ = 30°, 45°, 60°).
Paper: Lunar Crustal Magnetization Sourced via the Delivery of Iron-rich Ejecta from Basin-forming Impacts
Authors: R. I. Citron, L. L. Hood, S. T. Stewart
Figure caption: Tracer temperature at ejection vs. ejection distance for three example simulations. In some cases, tracers that are ejected to farther distances are ejected at hotter temperatures (panels (a) and (b)); however, some simulations display no correlation between tracer ejection temperature and ejection distance (panel (c)).
Paper: Thermal-IR Observations of (152830) Dinkinesh during the Lucy Mission Flyby
Authors: Samuel L. Jackson, Joshua P. Emery, Benjamin Rozitis, Philip R. Christensen, John R. Spencer, Stefano Mottola, Victoria E. Hamilton, Carly J. A. Howett, Simone Marchi, Keith S. Noll, Harold F. Levison
Figure caption: (a) Scale factors fitted to each spectrum plotted with phase angle for the homogeneous model (red shaded region) and the heterogeneous model (blue shaded region). (b) Single-temperature blackbody temperatures fitted to the L’TES spectra (black crosses), the best-fit homogeneous surface ATPM spectra (red line), and the best-fit heterogeneous surface ATPM spectra (blue line). (c) Reduced χ2 statistic values for the single-temperature blackbody fits (black crosses), best-fit homogeneous surface ATPM spectra (red line), and best-fit heterogeneous surface ATPM spectra (blue line).
Paper: Thermal-IR Observations of (152830) Dinkinesh during the Lucy Mission Flyby
Authors: Samuel L. Jackson, Joshua P. Emery, Benjamin Rozitis, Philip R. Christensen, John R. Spencer, Stefano Mottola, Victoria E. Hamilton, Carly J. A. Howett, Simone Marchi, Keith S. Noll, Harold F. Levison
Figure caption: Grain size estimation for varying volume filling factors. Horizontal lines represent the thermal conductivities calculated from the nominal thermal inertia value for Dinkinesh of Γ = 91 J m−2 K−1 s−1/2. The curves describe the thermal conductivity model (assuming parameters for stony meteorites) as a function of regolith grain size. The intersection between the thermal conductivity model and the derived thermal conductivity provides the estimate of the grain size for that volume filling factor.
Paper: Thermal-IR Observations of (152830) Dinkinesh during the Lucy Mission Flyby
Authors: Samuel L. Jackson, Joshua P. Emery, Benjamin Rozitis, Philip R. Christensen, John R. Spencer, Stefano Mottola, Victoria E. Hamilton, Carly J. A. Howett, Simone Marchi, Keith S. Noll, Harold F. Levison
Figure caption: Example comparison of the simulated shape of Dinkinesh overlaid on a L’LORRI image, used to determine the time step/rotation angle of Dinkinesh corresponding to the L’TES observations taken simultaneously. Panels (A)–(C): decreasing opacity of the simulated shape at the best time step from left to right. Panels (D)–(F): the same as (A)–(C) but with a simulated temperature map for a thermal inertia of 90 J m−2 K−1 s−1/2.
Paper: Thermal-IR Observations of (152830) Dinkinesh during the Lucy Mission Flyby
Authors: Samuel L. Jackson, Joshua P. Emery, Benjamin Rozitis, Philip R. Christensen, John R. Spencer, Stefano Mottola, Victoria E. Hamilton, Carly J. A. Howett, Simone Marchi, Keith S. Noll, Harold F. Levison
Figure caption: χ2 contour plane for thermal inertia vs. roughness. The color bar indicates the reduced χ2 value across the 10 spectra. The black circle denotes the minimum χ2 solution. The dotted contour denotes accepted 3σ solutions within Δχ2 = 14.2 of the minimum χ2. The black cross denotes the mean of the accepted 3σ solutions (i.e., the final parameter estimates).
Paper: Thermal-IR Observations of (152830) Dinkinesh during the Lucy Mission Flyby
Authors: Samuel L. Jackson, Joshua P. Emery, Benjamin Rozitis, Philip R. Christensen, John R. Spencer, Stefano Mottola, Victoria E. Hamilton, Carly J. A. Howett, Simone Marchi, Keith S. Noll, Harold F. Levison
Figure caption: Thermal inertia values derived from the individual L’TES spectra varying with phase angle. Tentative, but not significant, evidence of surface heterogeneity is present in these data. (a) All measurements. (b) Y-axis rescaled to exclude the two initial values and show a trend in the eight remaining values.
Paper: Thermal-IR Observations of (152830) Dinkinesh during the Lucy Mission Flyby
Authors: Samuel L. Jackson, Joshua P. Emery, Benjamin Rozitis, Philip R. Christensen, John R. Spencer, Stefano Mottola, Victoria E. Hamilton, Carly J. A. Howett, Simone Marchi, Keith S. Noll, Harold F. Levison
Figure caption: L’TES data binned into 10 spectra (crosses), ATPM homogeneous surface model fits and corresponding uncertainty region (blue lines and shaded areas), and the single-temperature blackbody fit to the data (red lines).
Paper: Thermal-IR Observations of (152830) Dinkinesh during the Lucy Mission Flyby
Authors: Samuel L. Jackson, Joshua P. Emery, Benjamin Rozitis, Philip R. Christensen, John R. Spencer, Stefano Mottola, Victoria E. Hamilton, Carly J. A. Howett, Simone Marchi, Keith S. Noll, Harold F. Levison
Figure caption: Grain sizes for a variety of solar system objects as a function of gravitational acceleration from B. Gundlach & J. Blum (2013), excluding objects observed with IRAS (which were systematically offset). The black lines are the mathematical models fit to the non-IRAS data by B. Gundlach & J. Blum (2013). Dinkinesh does not overlap with the fits to the rest of the asteroids, along with the C-type binary (175706) 1996 FG3 and the M-type asteroid (33342) 1998 WT24.
Paper: Thermal-IR Observations of (152830) Dinkinesh during the Lucy Mission Flyby
Authors: Samuel L. Jackson, Joshua P. Emery, Benjamin Rozitis, Philip R. Christensen, John R. Spencer, Stefano Mottola, Victoria E. Hamilton, Carly J. A. Howett, Simone Marchi, Keith S. Noll, Harold F. Levison
Figure caption: Calibrated spectral radiance at 423 cm−1 for each of the collected L’TES spectra (P. R. Christensen et al. 2024c). A clear peak is seen during the close approach of Dinkinesh.
Paper: Dust Production Rates in Jupiter-family Comets. II. Trends and Population Insights from ATLAS Photometry of 116 JFCs
Authors: A. Fraser Gillan, Alan Fitzsimmons, Larry Denneau, Robert J. Siverd, Ken W. Smith, John L. Tonry, David R. Young
Figure caption: Comparison between our measurements of A(0°)fρ for 67P in 2021–2022, values calculated from the magnitudes reported by D. Gardener et al. (2022), and values for the 2014/15 apparition calculated from the average rPS1 light curve also reported by D. Gardener et al. (2022). As both those data sets reported magnitudes in the PS1 system, we have converted our A(0°)fρ to that system as explained in the text. The apparent discontinuity at perihelion in the 2014–2015 values is due to the change in perihelion distance between the two apparitions.
Paper: Orbital Capture of Ejecta into Periodic Orbits around Binary Asteroid (65803) Didymos
Authors: Xiaoyu Fu, Flavia Saveriano, Stefania Soldini, Fabio Ferrari, Derek C. Richardson, Masatoshi Hirabayashi, Alessandro Rossi, Eugene G. Fahnestock, Tony L. Farnham, Arnold Gucsik, Stravro L. Ivanovski, Martin Jutzi, Akos Kereszturi, Jian-Yang Li, Francesco Marzari, Colby C. Merrill, Fernando Moreno, Sabina D. Raducan, Juan Luis Rizos, Gonzalo Tancredi, Josep M. Trigo-Rodriguez, Kleomenis Tsiganis, Stephan Ulamec, Yang Yu, Yun Zhang, Nancy Chabot, Andrew Rivkin, Adriano Campo Bagatin, Patrick Michel
Figure caption: Acceleration environment in the vicinity of the Didymos binary system. The x-axis indicates the radial distance along the line extending from the Didymos barycenter toward the Dimorphos barycenter. The ranges between minimum and maximum accelerations caused by the gravitation of homogeneous spherical Didymos and Dimorphos, third-body gravitational perturbation from the Sun, and SRP on spherical ejecta of varying radii are presented. These ranges are calculated over a time frame spanning from the DART impact on 2022 September 26 to 60 days postimpact. During the investigated period, the Sun–Didymos distance remains relatively stable, with a maximum variation of 3.16%. Therefore, the minimum and maximum perturbing accelerations from the Sun are on the same order of magnitude, leading to an almost invisible blue shaded area in the figure.
Paper: Orbital Capture of Ejecta into Periodic Orbits around Binary Asteroid (65803) Didymos
Authors: Xiaoyu Fu, Flavia Saveriano, Stefania Soldini, Fabio Ferrari, Derek C. Richardson, Masatoshi Hirabayashi, Alessandro Rossi, Eugene G. Fahnestock, Tony L. Farnham, Arnold Gucsik, Stravro L. Ivanovski, Martin Jutzi, Akos Kereszturi, Jian-Yang Li, Francesco Marzari, Colby C. Merrill, Fernando Moreno, Sabina D. Raducan, Juan Luis Rizos, Gonzalo Tancredi, Josep M. Trigo-Rodriguez, Kleomenis Tsiganis, Stephan Ulamec, Yang Yu, Yun Zhang, Nancy Chabot, Andrew Rivkin, Adriano Campo Bagatin, Patrick Michel
Figure caption: Didymos-centered synodic frame of the augmented BCRFB model for the Sun–Didymos–Dimorphos system. In this reference frame, the barycenters of the Sun (denoted by S) and Didymos (denoted by D1) remain stationary, while Dimorphos (denoted by D2) rotates clockwise about the origin. Furthermore, both Didymos and Dimorphos are approximated as polyhedrons and rotate clockwise about their respective major principal axes.
Paper: Orbital Capture of Ejecta into Periodic Orbits around Binary Asteroid (65803) Didymos
Authors: Xiaoyu Fu, Flavia Saveriano, Stefania Soldini, Fabio Ferrari, Derek C. Richardson, Masatoshi Hirabayashi, Alessandro Rossi, Eugene G. Fahnestock, Tony L. Farnham, Arnold Gucsik, Stravro L. Ivanovski, Martin Jutzi, Akos Kereszturi, Jian-Yang Li, Francesco Marzari, Colby C. Merrill, Fernando Moreno, Sabina D. Raducan, Juan Luis Rizos, Gonzalo Tancredi, Josep M. Trigo-Rodriguez, Kleomenis Tsiganis, Stephan Ulamec, Yang Yu, Yun Zhang, Nancy Chabot, Andrew Rivkin, Adriano Campo Bagatin, Patrick Michel
Figure caption: Illustration of the augmented BCRFB model. In this model, the motion of a mass particle m4 is governed by the SRP perturbation and the gravitational fields of three primary masses m1, m2, and m3, with their masses satisfying the relationship m1 ≫ m2 ≫ m3. Additionally, m2 and m3 are in circular motion about their barycenter with a mutual separation of d2, while m1 and m2–m3 orbit their common center of mass with a radius d1.
Paper: Orbital Capture of Ejecta into Periodic Orbits around Binary Asteroid (65803) Didymos
Authors: Xiaoyu Fu, Flavia Saveriano, Stefania Soldini, Fabio Ferrari, Derek C. Richardson, Masatoshi Hirabayashi, Alessandro Rossi, Eugene G. Fahnestock, Tony L. Farnham, Arnold Gucsik, Stravro L. Ivanovski, Martin Jutzi, Akos Kereszturi, Jian-Yang Li, Francesco Marzari, Colby C. Merrill, Fernando Moreno, Sabina D. Raducan, Juan Luis Rizos, Gonzalo Tancredi, Josep M. Trigo-Rodriguez, Kleomenis Tsiganis, Stephan Ulamec, Yang Yu, Yun Zhang, Nancy Chabot, Andrew Rivkin, Adriano Campo Bagatin, Patrick Michel
Figure caption: The variation of the x-coordinates of the collinear EPs in the augmented Sun–Didymos and Dimorphos system with respect to the SRP acceleration magnitude ∣∣aSRP∣∣. The locations of EPs are represented in the synodic frame centered on the secondary, which coincides with the origin of this frame.
Paper: Orbital Capture of Ejecta into Periodic Orbits around Binary Asteroid (65803) Didymos
Authors: Xiaoyu Fu, Flavia Saveriano, Stefania Soldini, Fabio Ferrari, Derek C. Richardson, Masatoshi Hirabayashi, Alessandro Rossi, Eugene G. Fahnestock, Tony L. Farnham, Arnold Gucsik, Stravro L. Ivanovski, Martin Jutzi, Akos Kereszturi, Jian-Yang Li, Francesco Marzari, Colby C. Merrill, Fernando Moreno, Sabina D. Raducan, Juan Luis Rizos, Gonzalo Tancredi, Josep M. Trigo-Rodriguez, Kleomenis Tsiganis, Stephan Ulamec, Yang Yu, Yun Zhang, Nancy Chabot, Andrew Rivkin, Adriano Campo Bagatin, Patrick Michel
Figure caption: An example of a backward-propagated ejecta trajectory along the stable manifold of a terminator orbit eventually impacting the surface of Dimorphos. (a) Trajectory in the Didymos-centered synodic frame. (b) Trajectory in the Dimorphos-centered body-fixed frame.
Paper: Orbital Capture of Ejecta into Periodic Orbits around Binary Asteroid (65803) Didymos
Authors: Xiaoyu Fu, Flavia Saveriano, Stefania Soldini, Fabio Ferrari, Derek C. Richardson, Masatoshi Hirabayashi, Alessandro Rossi, Eugene G. Fahnestock, Tony L. Farnham, Arnold Gucsik, Stravro L. Ivanovski, Martin Jutzi, Akos Kereszturi, Jian-Yang Li, Francesco Marzari, Colby C. Merrill, Fernando Moreno, Sabina D. Raducan, Juan Luis Rizos, Gonzalo Tancredi, Josep M. Trigo-Rodriguez, Kleomenis Tsiganis, Stephan Ulamec, Yang Yu, Yun Zhang, Nancy Chabot, Andrew Rivkin, Adriano Campo Bagatin, Patrick Michel
Figure caption: An example of a backward-propagated ejecta trajectory along the stable manifold of a terminator orbit eventually impacting the surface of Didymos. (a) Trajectory in the Didymos-centered synodic frame. (b) Trajectory in the Didymos-centered body-fixed frame.
Paper: Plume Activity on Europa: Current Knowledge and Search Strategy for Europa Clipper
Authors: Lorenz Roth, Erin Leonard, Kelly Miller, Matt Hedman, Lynnae C. Quick, Tracy M. Becker, Shawn Brooks, Corey Cochrane, Ashley Gerard Davies, Carolyn M. Ernst, Cyril Grima, Candice J. Hansen, Carly Howett, Sean Hsu, Xianzhe Jia, Adrienn Luspay-Kuti, Margaret Kivelson, Fabian Klenner, Alfred McEwen, William B. McKinnon, Robert T. Pappalardo, Frank Postberg, Julie Rathbun, Kurt D. Retherford, Kirk Scanlan, K. Marshall Seaton, John R. Spencer, J. Hunter Waite, Paul Withers, Danielle Wyrick, Mikhail Yu. Zolotov
Figure caption: Coordinates of locations of inferred plumes from different studies (pink with error bars indicating the uncertainty) overlaid on a simplified version of the global geological map of Europa (E. J. Leonard et al. 2024). Uncertainties for the coordinates were estimated considering mapping detected features in spatially resolved images to surface coordinates (L. Roth et al. 2014b; W. B. Sparks et al. 2016), the size of the observing slit at the equator (L. Paganini et al. 2020), or the range of parameters tested (H. Arnold et al. 2019). Location and shape of the plume inferred in X. Jia et al. (2018) appear tightly constrained (including a required tilt of the plume axis from the normal), and thus the location has no uncertainty here.
Paper: Plume Activity on Europa: Current Knowledge and Search Strategy for Europa Clipper
Authors: Lorenz Roth, Erin Leonard, Kelly Miller, Matt Hedman, Lynnae C. Quick, Tracy M. Becker, Shawn Brooks, Corey Cochrane, Ashley Gerard Davies, Carolyn M. Ernst, Cyril Grima, Candice J. Hansen, Carly Howett, Sean Hsu, Xianzhe Jia, Adrienn Luspay-Kuti, Margaret Kivelson, Fabian Klenner, Alfred McEwen, William B. McKinnon, Robert T. Pappalardo, Frank Postberg, Julie Rathbun, Kurt D. Retherford, Kirk Scanlan, K. Marshall Seaton, John R. Spencer, J. Hunter Waite, Paul Withers, Danielle Wyrick, Mikhail Yu. Zolotov
Figure caption: Schematic of a cross section through the icy shell of Europa showing hypothesized processes that might generate a plume, cryovolcanic surface features, and other morphology indicative of current activity. The ice shell is shown as consisting of a cold, brittle shell over a warmer, more deformable ductile layer, above a global briny ocean. The ice shell is subject to stresses that may first form and then possibly open and close cracks and any conduits. The latter could provide indirect pathways for water into the ice shell. These strong tidal stresses contribute to the formation of cycloids, ridges, and extensional bands. The effects of diapirism within the ice shell may penetrate to the surface, leading to extrusion and resurfacing. Diapirism and shell fracturing can lead to the formation of liquid reservoirs within the brittle ice. Stresses in such reservoirs as the water or brine freezes might lead to the opening of conduits to the surface, the generation of a plume, the formation of domes, or the emplacement of “cryolavas” or smooth plains; all these phenomena present the possibility of plume activity to different extents. Figure from I. J. Daubar et al. (2024).
Paper: Plume Activity on Europa: Current Knowledge and Search Strategy for Europa Clipper
Authors: Lorenz Roth, Erin Leonard, Kelly Miller, Matt Hedman, Lynnae C. Quick, Tracy M. Becker, Shawn Brooks, Corey Cochrane, Ashley Gerard Davies, Carolyn M. Ernst, Cyril Grima, Candice J. Hansen, Carly Howett, Sean Hsu, Xianzhe Jia, Adrienn Luspay-Kuti, Margaret Kivelson, Fabian Klenner, Alfred McEwen, William B. McKinnon, Robert T. Pappalardo, Frank Postberg, Julie Rathbun, Kurt D. Retherford, Kirk Scanlan, K. Marshall Seaton, John R. Spencer, J. Hunter Waite, Paul Withers, Danielle Wyrick, Mikhail Yu. Zolotov
Figure caption: (a) Modeled identification of plume gas and atmospheric gas in absorption during Europa-UVS occultation. (b) Europa-UVS mapping of H Lyα plume auroral emissions as modeled after L. Roth et al. (2014b) using the push broom observing mode with airglow port and high spatial resolution port. (c) New Horizons image of optical auroral emission from Tvashtar plume near Io’s north pole (J. R. Spencer et al. 2007).
Paper: Plume Activity on Europa: Current Knowledge and Search Strategy for Europa Clipper
Authors: Lorenz Roth, Erin Leonard, Kelly Miller, Matt Hedman, Lynnae C. Quick, Tracy M. Becker, Shawn Brooks, Corey Cochrane, Ashley Gerard Davies, Carolyn M. Ernst, Cyril Grima, Candice J. Hansen, Carly Howett, Sean Hsu, Xianzhe Jia, Adrienn Luspay-Kuti, Margaret Kivelson, Fabian Klenner, Alfred McEwen, William B. McKinnon, Robert T. Pappalardo, Frank Postberg, Julie Rathbun, Kurt D. Retherford, Kirk Scanlan, K. Marshall Seaton, John R. Spencer, J. Hunter Waite, Paul Withers, Danielle Wyrick, Mikhail Yu. Zolotov
Figure caption: Left: simultaneous spectral HST images of localized emissions from H (at 1215.6 nm) and O (at 130.4 nm) near the south pole interpreted to originate from dissociative excitation of locally sourced H2O vapor by electrons (adapted from L. Roth et al. 2014b). Right: HST UV filter image of Europa in transit of Jupiter with small dark features outside the yellow circle (white arrows) interpreted to originate from absorption by a substance in erupting plumes (W. B. Sparks et al. 2016). Note that the orbital phase of Europa differs by 90° between these images (the two on the left and the right one) and features appearing on the limb are not mapped to the same locations (see also Figure 4 for the corresponding locations).
Paper: Plume Activity on Europa: Current Knowledge and Search Strategy for Europa Clipper
Authors: Lorenz Roth, Erin Leonard, Kelly Miller, Matt Hedman, Lynnae C. Quick, Tracy M. Becker, Shawn Brooks, Corey Cochrane, Ashley Gerard Davies, Carolyn M. Ernst, Cyril Grima, Candice J. Hansen, Carly Howett, Sean Hsu, Xianzhe Jia, Adrienn Luspay-Kuti, Margaret Kivelson, Fabian Klenner, Alfred McEwen, William B. McKinnon, Robert T. Pappalardo, Frank Postberg, Julie Rathbun, Kurt D. Retherford, Kirk Scanlan, K. Marshall Seaton, John R. Spencer, J. Hunter Waite, Paul Withers, Danielle Wyrick, Mikhail Yu. Zolotov
Figure caption: Planned trajectory (21F31_v6) for the Europa Clipper Tour Phase. Each line is the ground track of the spacecraft colored by altitude (up to 2000 km) and labeled by Jovian orbit number and Europa flyby number (e.g., 72E46 is the 72nd Jupiter orbit and the 46th Europa flyby). Crosses show the subspacecraft location for each flyby at closest approach. For more information (such as panels and numbers) on this figure, see details in R. T. Pappalardo et al. (2024).
Paper: Plume Activity on Europa: Current Knowledge and Search Strategy for Europa Clipper
Authors: Lorenz Roth, Erin Leonard, Kelly Miller, Matt Hedman, Lynnae C. Quick, Tracy M. Becker, Shawn Brooks, Corey Cochrane, Ashley Gerard Davies, Carolyn M. Ernst, Cyril Grima, Candice J. Hansen, Carly Howett, Sean Hsu, Xianzhe Jia, Adrienn Luspay-Kuti, Margaret Kivelson, Fabian Klenner, Alfred McEwen, William B. McKinnon, Robert T. Pappalardo, Frank Postberg, Julie Rathbun, Kurt D. Retherford, Kirk Scanlan, K. Marshall Seaton, John R. Spencer, J. Hunter Waite, Paul Withers, Danielle Wyrick, Mikhail Yu. Zolotov
Figure caption: Global coverage of Europa in longitude and local time for a possible tour for Europa Clipper (figure from P. R. Christensen et al. 2024). Local time is measured in degrees of rotation, starting at midnight. Global data are assumed to be obtained during joint scans obtained at roughly 30,000 km range on approach and departure for each flyby. Each diamond represents the subspacecraft point during the approach (suffix “A”) or departure (suffix “D”) leg of the named orbit, and the diagonal line shows longitude and local time away from the subspacecraft point, out to 60° emission angle. Arbitrary colors are used to distinguish different orbits. Orange and purple background indicates the desired “day” and “night” local times for thermal inertia determination, respectively, as specified in the E-THEMIS requirements.
Paper: Plume Activity on Europa: Current Knowledge and Search Strategy for Europa Clipper
Authors: Lorenz Roth, Erin Leonard, Kelly Miller, Matt Hedman, Lynnae C. Quick, Tracy M. Becker, Shawn Brooks, Corey Cochrane, Ashley Gerard Davies, Carolyn M. Ernst, Cyril Grima, Candice J. Hansen, Carly Howett, Sean Hsu, Xianzhe Jia, Adrienn Luspay-Kuti, Margaret Kivelson, Fabian Klenner, Alfred McEwen, William B. McKinnon, Robert T. Pappalardo, Frank Postberg, Julie Rathbun, Kurt D. Retherford, Kirk Scanlan, K. Marshall Seaton, John R. Spencer, J. Hunter Waite, Paul Withers, Danielle Wyrick, Mikhail Yu. Zolotov
Figure caption: Left: two theoretical MISE spectra of a plume on Europa, computed assuming that the plume particles are composed of pure water ice and that the particles’ size and launch velocity distributions are similar to those of the Enceladus plume (D. Blaney et al. 2024). The spectrum of the plume’s upper reaches is bluer than that of the base because larger particles are launched at lower speeds (J. Schmidt et al. 2008; F. Postberg et al. 2011). Right: detection of thermal anomalies by MISE (D. Blaney et al. 2024). The solid lines represent a pixel-filling thermal anomaly. The dashed lines represent a 10% pixel fill fraction. The acceptable SNR is 10. Coadding of bands further increases instrument sensitivity.
Paper: Plume Activity on Europa: Current Knowledge and Search Strategy for Europa Clipper
Authors: Lorenz Roth, Erin Leonard, Kelly Miller, Matt Hedman, Lynnae C. Quick, Tracy M. Becker, Shawn Brooks, Corey Cochrane, Ashley Gerard Davies, Carolyn M. Ernst, Cyril Grima, Candice J. Hansen, Carly Howett, Sean Hsu, Xianzhe Jia, Adrienn Luspay-Kuti, Margaret Kivelson, Fabian Klenner, Alfred McEwen, William B. McKinnon, Robert T. Pappalardo, Frank Postberg, Julie Rathbun, Kurt D. Retherford, Kirk Scanlan, K. Marshall Seaton, John R. Spencer, J. Hunter Waite, Paul Withers, Danielle Wyrick, Mikhail Yu. Zolotov
Figure caption: Voyager 1 image of plumes on Io’s limb (left) and terminator from a distance of 4.5 × 106 km. Similarly, EIS will be able to detect plumes erupting on Europa’s limb and terminator.