adsabs/AstroCLIMB huggingface dataset:
Paper: Methane-saturated Layers Limit the Observability of Impact Craters on Titan
Authors: Shigeru Wakita , Brandon C. Johnson, Jason M. Soderblom, Jahnavi Shah, and Catherine D. Neish
Figure caption: Melting temperature curve as a function of pressure. The pink solid line represents the melting temperature curve of methane clathrate in this study (see Section 2). The melting temperature of water ice is shown as a blue dashed line as a reference. The points depict experimental data (Sloan et al. 2007, and references therein). The green dashed–dotted line is given by the equation in Levi et al. (2014).
Paper: Methane-saturated Layers Limit the Observability of Impact Craters on Titan
Authors: Shigeru Wakita , Brandon C. Johnson, Jason M. Soderblom, Jahnavi Shah, and Catherine D. Neish
Figure caption: Yield strength of methane clathrate as a function of temperature. The symbols depict experimental data (Durham et al. 2003) colored by the confining pressure (MPa). Lines represent our strength model with a confining pressure of 100 (solid line) and 50 (dotted line) MPa.
Paper: Methane-saturated Layers Limit the Observability of Impact Craters on Titan
Authors: Shigeru Wakita , Brandon C. Johnson, Jason M. Soderblom, Jahnavi Shah, and Catherine D. Neish
Figure caption: Surface profiles 60 s after the impact of a 5 km diameter impactor on different targets. The blue dashed line depicts a water-ice basement, and the pink solid line depicts a methane-clathrate basement.
Paper: Methane-saturated Layers Limit the Observability of Impact Craters on Titan
Authors: Shigeru Wakita , Brandon C. Johnson, Jason M. Soderblom, Jahnavi Shah, and Catherine D. Neish
Figure caption: Surface profiles 2400 s after the impact of a 5 km diameter impactor on different targets: (a) water-ice basement, (b) 5 km methane-clathrate layer over a water-ice basement, (c) 10 km methane-clathrate layer over a water-ice basement, and (d) methane-clathrate basement. The shaded region depicts the 300 m (three cells) from the original target surface (six cells in total height).
Paper: Methane-saturated Layers Limit the Observability of Impact Craters on Titan
Authors: Shigeru Wakita , Brandon C. Johnson, Jason M. Soderblom, Jahnavi Shah, and Catherine D. Neish
Figure caption: The 2D radial profiles of the target composition, with water ice in blue and methane clathrate in pink, 2400 s after the impact of a 5 km diameter impactor on different targets: (a) water-ice basement, (b) 5 km methane-clathrate layer over a water-ice basement, (c) 10 km methane-clathrate layer over a water-ice basement, and (d) methane-clathrate basement. Black solid lines depict the surface profile of case (d) (same as the solid line in Figure 4).
Paper: Methane-saturated Layers Limit the Observability of Impact Craters on Titan
Authors: Shigeru Wakita , Brandon C. Johnson, Jason M. Soderblom, Jahnavi Shah, and Catherine D. Neish
Figure caption: Time series for the impact of a Dimp = 5 km impactor on a target composed of a 1 km methane-saturated layer over a methane-clathrate basement. Blue illustrates water ice (impactor), pink is methane clathrate, and yellow is the methane-saturated layer.
Paper: Methane-saturated Layers Limit the Observability of Impact Craters on Titan
Authors: Shigeru Wakita , Brandon C. Johnson, Jason M. Soderblom, Jahnavi Shah, and Catherine D. Neish
Figure caption: Same viewing geometry as Figure 6 but for the case of a 1.5 km methane-saturated layer over a methane-clathrate basement with Dimp = 5 km.
Paper: Methane-saturated Layers Limit the Observability of Impact Craters on Titan
Authors: Shigeru Wakita , Brandon C. Johnson, Jason M. Soderblom, Jahnavi Shah, and Catherine D. Neish
Figure caption: Same viewing geometry as Figure 6 but for the case of a 2 km methane-saturated layer over a methane-clathrate basement with Dimp = 5 km.
Paper: Methane-saturated Layers Limit the Observability of Impact Craters on Titan
Authors: Shigeru Wakita , Brandon C. Johnson, Jason M. Soderblom, Jahnavi Shah, and Catherine D. Neish
Figure caption: The 2D radial profiles of the target composition for Dimp = 5 km impactors on a methane-saturated layer. Methane clathrate is shown in pink, methane-saturated ice in yellow, and water ice (impactor) in blue. Black solid lines depict the surface profile without the methane-saturated layer (i.e., into a pure methane-clathrate basement). The thickness of the methane-saturated layer is (a) 1, (b) 1.5, and (c) 2 km. An arrow in panel (a) indicates the edge of the wall (see text).
Paper: Methane-saturated Layers Limit the Observability of Impact Craters on Titan
Authors: Shigeru Wakita , Brandon C. Johnson, Jason M. Soderblom, Jahnavi Shah, and Catherine D. Neish
Figure caption: Same viewing as Figure 9 but for the case of Dimp = 3 km. The thickness of the methane-saturated layer is (a) 0.5, (b) 1.5, and (c) 2 km.
Paper: Methane-saturated Layers Limit the Observability of Impact Craters on Titan
Authors: Shigeru Wakita , Brandon C. Johnson, Jason M. Soderblom, Jahnavi Shah, and Catherine D. Neish
Figure caption: Same viewing as Figure 9 but for the case of Dimp = 2 km. The thickness of the methane-saturated layer is (a) 0.5, (b) 1, and (c) 1.5 km.
Paper: Methane-saturated Layers Limit the Observability of Impact Craters on Titan
Authors: Shigeru Wakita , Brandon C. Johnson, Jason M. Soderblom, Jahnavi Shah, and Catherine D. Neish
Figure caption: Crater depth as a function of crater diameter. Color indicates the thickness of the methane-saturated layer. Each symbol represents a different topographic expression of the crater: circles for an obvious cavity with rim, squares for an obvious cavity without rim, triangles for depression, and crosses for a flat surface (see also Table 2). The vertical error bar corresponds to the uncertainty of six cells.
Paper: Magnetospheric Ion Bombardment of Europa’s Surface
Authors: T. A. Nordheim, L. H. Regoli, C. D. K. Harris, C. Paranicas, K. P. Hand, and X. Jia
Figure caption: Magnetic fields for the three multifluid MHD simulation cases listed in Table 1, where case 1 represents Europa near Jupiter’s magnetic equator, and cases 2 and 3 represent the moon at increasingly higher southern magnetic latitudes. The results are plotted in the EPhiO coordinate system, and the distance units are in Europa radii. We show the perpendicular component of the magnetic field in each plane in color contours and the parallel components of the magnetic field in streamlines projected onto each plane. We omit the streamlines in the XY plane, where BX and BY vary negligibly.
Paper: Magnetospheric Ion Bombardment of Europa’s Surface
Authors: T. A. Nordheim, L. H. Regoli, C. D. K. Harris, C. Paranicas, K. P. Hand, and X. Jia
Figure caption: Electric fields for the three multifluid MHD simulation cases listed in Table 1, where case 1 represents Europa near Jupiter’s magnetic equator, and cases 2 and 3 represent the moon at increasingly higher southern magnetic latitudes. The results are plotted in the EPhiO coordinate system, and the distance units are in Europa radii. The electric field is calculated as E = −u × B, where u is the charge-averaged velocity of the thermal ion fluids in the MHD model.
Paper: Magnetospheric Ion Bombardment of Europa’s Surface
Authors: T. A. Nordheim, L. H. Regoli, C. D. K. Harris, C. Paranicas, K. P. Hand, and X. Jia
Figure caption: Trajectories of 100 keV magnetospheric ions (H+ in blue, O++ in red, and S+++ in yellow) within the electromagnetic fields from case 1, where Europa was near Jupiter’s magnetic equator. Here magnetic field draping at the trailing (upstream) hemisphere can be seen to strongly affect the particle trajectories near Europa. The results are plotted in the EPhiO coordinate system, and the distance units are in Europa radii.
Paper: Magnetospheric Ion Bombardment of Europa’s Surface
Authors: T. A. Nordheim, L. H. Regoli, C. D. K. Harris, C. Paranicas, K. P. Hand, and X. Jia
Figure caption: Ion access maps for H+, O++, and S+++ traced for an idealized case where the background Jovian magnetic field is uniform, and there are no local electromagnetic perturbations due to Europa. The color bar indicates the local accessibility, in percentage, for an ion of a given species and energy. In other words, for a given ion, 100% indicates complete access, whereas 50% means that only half of the incoming ions at that energy would be able to reach that region of the surface. The results are shown in a simple cylindrical map projection in a geographic west longitude coordinate system, where the trailing hemisphere (270° W) is upstream and the leading hemisphere (90° W) is downstream relative to thermal corotating plasma from Jupiter’s magnetosphere.
Paper: Magnetospheric Ion Bombardment of Europa’s Surface
Authors: T. A. Nordheim, L. H. Regoli, C. D. K. Harris, C. Paranicas, K. P. Hand, and X. Jia
Figure caption: Ion access maps for H+, O++, and S+++ traced within electromagnetic fields from the case 1 multifluid MHD simulation (Table 1). The color bar indicates the local accessibility, in percentage, for an ion of a given species and energy. In other words, for a given ion, 100% indicates complete access, whereas 50% means that only half of the incoming ions at that energy would be able to reach that region of the surface. The results are shown in a simple cylindrical map projection in a geographic west longitude coordinate system, where the trailing hemisphere (270° W) is upstream and the leading hemisphere (90° W) is downstream relative to thermal corotating plasma from Jupiter’s magnetosphere.
Paper: Magnetospheric Ion Bombardment of Europa’s Surface
Authors: T. A. Nordheim, L. H. Regoli, C. D. K. Harris, C. Paranicas, K. P. Hand, and X. Jia
Figure caption: Ion access maps for H+, O++, and S+++ traced within electromagnetic fields from the case 2 multifluid MHD simulation (Table 1). The color bar indicates the local accessibility (in %) for an ion of a given species and energy. The results are shown in a simple cylindrical map projection in a geographic west longitude coordinate system, where the trailing hemisphere (270° W) is upstream and the leading hemisphere (90° W) is downstream relative to thermal corotating plasma from Jupiter’s magnetosphere.
Paper: Magnetospheric Ion Bombardment of Europa’s Surface
Authors: T. A. Nordheim, L. H. Regoli, C. D. K. Harris, C. Paranicas, K. P. Hand, and X. Jia
Figure caption: Ion access maps for H+, O++, and S+++ traced within electromagnetic fields from the case 3 multifluid MHD simulation (Table 1). The color bar indicates the local accessibility (in %) for an ion of a given species and energy. The results are shown in a simple cylindrical map projection in a geographic west longitude coordinate system, where the trailing hemisphere (270° W) is upstream and the leading hemisphere (90° W) is downstream relative to thermal corotating plasma from Jupiter’s magnetosphere.
Paper: Magnetospheric Ion Bombardment of Europa’s Surface
Authors: T. A. Nordheim, L. H. Regoli, C. D. K. Harris, C. Paranicas, K. P. Hand, and X. Jia
Figure caption: Ion access maps for H+ and S+++ traced within electromagnetic fields from the case 3 multifluid MHD simulation (Table 1) without (left) and with (right) ocean-induced magnetic fields included. The color bar indicates the local accessibility (in %) for an ion of a given species and energy. The results for O++ (not shown) are almost identical to those for S+++. The results are shown in a simple cylindrical map projection in a geographic west longitude coordinate system, where the trailing hemisphere (270° W) is upstream and the leading hemisphere (90° W) is downstream relative to thermal corotating plasma from Jupiter’s magnetosphere.
Paper: Magnetospheric Ion Bombardment of Europa’s Surface
Authors: T. A. Nordheim, L. H. Regoli, C. D. K. Harris, C. Paranicas, K. P. Hand, and X. Jia
Figure caption: Average ion access maps for H+, O++, and S+++ appropriate for the study of surface weathering at Europa over longer timescales (e.g., exceeding one orbit of Europa around Jupiter). The color bar indicates the local accessibility (in %) for an ion of a given species and energy. The results are shown in a simple cylindrical map projection in a geographic west longitude coordinate system, where the trailing hemisphere (270° W) is upstream and the leading hemisphere (90° W) is downstream relative to thermal corotating plasma from Jupiter’s magnetosphere.
Paper: Magnetospheric Ion Bombardment of Europa’s Surface
Authors: T. A. Nordheim, L. H. Regoli, C. D. K. Harris, C. Paranicas, K. P. Hand, and X. Jia
Figure caption: Representative ion flux profiles for Europa. These profiles represent the upstream unperturbed ion flux environment well away from the Europa interaction region. The thermal component (dashed–dotted lines) was calculated using a convecting Maxwellian distribution and plasma properties from Bagenal et al. (2015) and Delamere et al. (2005). For the energetic proton, O++, and S+++ fluxes (solid lines), we have used the modified kappa distributions from Mauk et al. (2004) based on observations made by the Galileo EPD instrument during the E4 flyby (“E4_ENC”).
Paper: Magnetospheric Ion Bombardment of Europa’s Surface
Authors: T. A. Nordheim, L. H. Regoli, C. D. K. Harris, C. Paranicas, K. P. Hand, and X. Jia
Figure caption: Ion flux maps for the surface of Europa calculated using the average access maps shown in Figure 9, as well as the flux spectra shown in Figure 10. Fluxes are in units of ions/cm2-s. The results are shown in a simple cylindrical map projection in a geographic west longitude coordinate system, where the trailing hemisphere (270° W) is upstream and the leading hemisphere (90° W) is downstream relative to thermal corotating plasma from Jupiter’s magnetosphere. Note that for 1 and 10 keV, the flux is calculated using the sum of the thermal (O+, S++) and energetic (O++, S+++) parts of the distributions, and therefore the precipitating flux includes a mix of the two charge states. See Appendix B for results at additional energies.
Paper: Magnetospheric Ion Bombardment of Europa’s Surface
Authors: T. A. Nordheim, L. H. Regoli, C. D. K. Harris, C. Paranicas, K. P. Hand, and X. Jia
Figure caption: Plots of half-bounce equatorial displacement (top) and period (bottom) for H+, O++, and S+++ magnetospheric ions at Europa’s minimum L-shell (L=9.4) calculated using the equations from Roederer (1967).
Paper: Magnetospheric Ion Bombardment of Europa’s Surface
Authors: T. A. Nordheim, L. H. Regoli, C. D. K. Harris, C. Paranicas, K. P. Hand, and X. Jia
Figure caption: Energy Change of back-traced magnetospheric Ions for Case 1. Shown are back-traced trajectories of H+, O++, and S+++ ions with an initial kinetic energy of 100 keV and an equatorial pitch angle of 45 degrees°. This demonstrates that the change in kinetic energy due to the locally perturbed electromagnetic fields near Europa is at the ~percent level and therefore negligible.
Paper: Magnetospheric Ion Bombardment of Europa’s Surface
Authors: T. A. Nordheim, L. H. Regoli, C. D. K. Harris, C. Paranicas, K. P. Hand, and X. Jia
Figure caption: Flux of magnetospheric protons at the surface of Europa calculated using the average access maps shown in Figure 9, as well as the flux spectra shown in Figure 10. These flux maps are identical to those shown in Figure 11, but include additional energies (100 eV and 100 MeV). Fluxes are in units of ions/cm2-s. The results are shown in a simple cylindrical map projection in a geographic west longitude coordinate system, where the trailing hemisphere (270°W)is upstream and the leading hemisphere (90°W) is downstream relative to thermal corotating plasma from Jupiter’s magnetosphere. Note that for 100 eV, 1 keV, and 10 keV, the flux is calculated using the sum of the thermal (O+, S++) and energetic (O++, S+++) parts of the distributions, and therefore the precipitating flux includes a mix of the two charge states.
Paper: Magnetospheric Ion Bombardment of Europa’s Surface
Authors: T. A. Nordheim, L. H. Regoli, C. D. K. Harris, C. Paranicas, K. P. Hand, and X. Jia
Figure caption: Flux of magnetospheric oxygen ions at the surface of Europa calculated using the average access maps shown in Figure 9, as well as the flux spectra shown in Figure 10. These flux maps are identical to those shown in Figure 11, but include additional energies (100 eV and 100 MeV). Fluxes are in units of ions/cm2-s. The results are shown in a simple cylindrical map projection in a geographic west longitude coordinate system, where the trailing hemisphere (270°W)is upstream and the leading hemisphere (90°W) is downstream relative to thermal corotating plasma from Jupiter’s magnetosphere. Note that for 100 eV, 1 keV, and 10 keV, the flux is calculated using the sum of the thermal (O+, S++) and energetic (O++, S+++) parts of the distributions, and therefore the precipitating flux includes a mix of the two charge states.
Paper: Magnetospheric Ion Bombardment of Europa’s Surface
Authors: T. A. Nordheim, L. H. Regoli, C. D. K. Harris, C. Paranicas, K. P. Hand, and X. Jia
Figure caption: Flux of magnetospheric sulfur ions at the surface of Europa calculated using the average access maps shown in Figure 9, as well as the flux spectra shown in Figure 10. These flux maps are identical to those shown in Figure 11, but include additional energies (100 eV and 100 MeV). Fluxes are in units of ions/cm2-s. The results are shown in a simple cylindrical map projection in a geographic west longitude coordinate system, where the trailing hemisphere (270°W)is upstream and the leading hemisphere (90°W) is downstream relative to thermal corotating plasma from Jupiter’s magnetosphere. Note that for 100 eV, 1 keV, and 10 keV, the flux is calculated using the sum of the thermal (O+, S++) and energetic (O++, S+++) parts of the distributions, and therefore the precipitating flux includes a mix of the two charge states.
Paper: Magnetospheric Ion Bombardment of Europa’s Surface
Authors: T. A. Nordheim, L. H. Regoli, C. D. K. Harris, C. Paranicas, K. P. Hand, and X. Jia
Figure caption: Comparison of time-averaged ion access patterns for different charge states.
Paper: Empirical Photochemical Modeling of Saturn’s Ionization Balance Including Grain Charging
Authors: E. Vigren, J. Dreyer, A. I. Eriksson, F. L. Johansson, M. Morooka, and J.-E. Wahlund
Figure caption: Model results (solid lines) generated by the provided model input (dashed lines and numbers within the text box). In this case, the model has been used for conditions encountered near 2200 km above Saturn’s 1 bar level during the inbound part of orbit 292. The [M]/[R] ratio varies over the range 0–∼2.
Paper: Empirical Photochemical Modeling of Saturn’s Ionization Balance Including Grain Charging
Authors: E. Vigren, J. Dreyer, A. I. Eriksson, F. L. Johansson, M. Morooka, and J.-E. Wahlund
Figure caption: Model results (solid lines) generated by the provided model input (dashed lines and numbers within the text box). In this case, the model has been used for conditions encountered near 1700 km above Saturn’s 1 bar level during the inbound part of orbit 292. The [M]/[R] ratio varies over the range 0–∼0.02.
Paper: High-resolution Search for Kuiper Belt Object Binaries from New Horizons
Authors: H.A. Weaver, S.B. Porter, and J.R. Spencer
Figure caption: R.A. and decl. drift rates are displayed for the 125 images taken during the observations of OS393 for REQID 131ss. The pointing drifts within a dead band of ±250 μrad (±52″) centered on the commanded target ephemeris location. Hydrazine thrusters fire to maintain the pointing within the dead band; the times of thruster firings are associated with abrupt changes in either the R.A. or decl. drift rates in this plot. The mean total plane-of-sky drift rate for this set of observations was 27.34 ± 4.51 μrad s−1(5.64 ± 0.93 arcsec s−1), which is typical for New Horizons observations.
Paper: High-resolution Search for Kuiper Belt Object Binaries from New Horizons
Authors: H.A. Weaver, S.B. Porter, and J.R. Spencer
Figure caption: Window selection details for one set (REQID = 131ss) of observations of OS393. The background image is taken from the Palomar Digital Sky Survey (red filter, second generation reduction); celestial north points straight down and celestial east points to the right. The orange box is the LORRI FOV with XLORRI (the direction of increasing CCD columns) pointing to the right and YLORRI (the direction of increasing CCD rows) pointing up. The magenta box is the requested window (i.e., the window specified by the command arguments listed in magenta just above the orange box). The dashed magenta box (with light yellow background highlighting) is the magenta box reduced by the size of the pointing dead band (500 μrad = 104″) in each dimension. We generally sized the image windows to capture both the KBO and at least one star with V ≤ 13 within the dashed magenta box. The red dot gives the LORRI boresight location, which is where the pointing control system commanded OS393 to be placed. The red box shows the size of the pointing dead band centered on the LORRI boresight. The red X shows the predicted OS393 location using the ephemeris used in planning the observations, which is offset from the boresight by the absolute pointing error derived using astrometry from 4 × 4 images taken near the time of the 1 × 1 observations. The cyan X shows the predicted OS393 location using the new ephemeris generated based on the location of OS393 in the 4 × 4 images. The cyan box is the pointing dead band centered on that location. The V magnitudes from APASS for stars in the UCAC4 catalog are indicated in cyan.
Paper: High-resolution Search for Kuiper Belt Object Binaries from New Horizons
Authors: H.A. Weaver, S.B. Porter, and J.R. Spencer
Figure caption: Composite images of HK103 from two different epochs (2018 August 17 above the red line and 2018 August 19 below the red line) are displayed. For each epoch, the top row shows 512 × 512 frames containing the windowed portions of the full 1024 × 1024 LORRI 1 × 1 images, and the bottom row shows 64 × 64 frames centered on either the KBO (circled in red in the top row) or a nearby star of comparable brightness (circled in blue in the top row). Composite images produced by coaligning the images on the ephemeris locations of HK103 are displayed in the first three columns: 125 images are combined for the first two columns and 250 images are combined for the third column. The REQIDs are displayed in the upper left of each frame. Composite images created by coaligning on stars for all 250 images are displayed in the fourth column. All images are displayed using a linear stretch ranging from −1 to 1 DN, except for the top two images in the fourth column, which use a stretch from −2 to 4 DN to avoid saturating the circled star. Celestial north points down and east points to the right in all images.
Paper: High-resolution Search for Kuiper Belt Object Binaries from New Horizons
Authors: H.A. Weaver, S.B. Porter, and J.R. Spencer
Figure caption: Single- and double-PSF fits to the double-sampled LORRI images of HK103. The pair of panels on the left-hand side shows the two observations from the first epoch (REQIDs 123u and 123v), and the pair of panels on the right-hand side shows the two observations from the second epoch (REQIDs 123w and 123x). For the three frames within each observation epoch, the leftmost image shows the WCS-driven shift stack of the 125 images, the middle image shows the residuals after subtracting a best-fit single PSF, and the rightmost images show the residuals after subtracting the best-fit double PSFs. The red dots show the locations of the center of each PSF fit. The same linear stretch is used for each image. Since the residuals in the double-PSF solution look similar to those in the single-PSF solution, and the locations of the object locations in the double-PSF solution varies over the image, HK103 does not appear to be a binary.