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Paper: JWST Reveals Varied Origins between Jupiter’s Irregular Satellites
Authors: Benjamin N. L. Sharkey, Andrew S. Rivkin, Richard J. Cartwright, Bryan J. Holler, Joshua P. Emery, Cristina Thomas
Figure caption: The 3 μm regions of Himalia family objects (with shifts for Lysithea and Himalia of ±0.05 for readability). Note that Lysithea displays a sharper band, overprinted by numerous subtle absorptions, while Elara and Himalia have more rounded features near 3 μm. Bottom: we averaged Himalia’s and Lysithea’s spectra into a new, combined spectrum that closely matches Elara, with the only exception being Elara’s lack of a 2.63 μm feature. The 3 μm band depth of the averaged Himalia/Lysithea absorption was multiplied by a factor of 1.07 to make comparison to the shape of Elara’s spectral features easier.
Paper: JWST Reveals Varied Origins between Jupiter’s Irregular Satellites
Authors: Benjamin N. L. Sharkey, Andrew S. Rivkin, Richard J. Cartwright, Bryan J. Holler, Joshua P. Emery, Cristina Thomas
Figure caption: The 3 μm band centers vs. band depths of Jovian Trojan and irregular satellites with available band analysis parameters, from this work and I. Wong et al. (2024). Himalia and Elara are excluded from this analysis owing to their overlapping features at 2.7 and 3.0 μm, which render a single band center ambiguous. Marker color corresponds to the object’s spectral slope from 0.7 to 2.4 μm collected in this work or from the literature (B. N. L. Sharkey et al. 2019; I. Wong et al. 2024). Marker size refers to the diameters as collected in Table 1.
Paper: Surface Binding Energies for Amorphous Plagioclase Feldspar Calculated Using Molecular Dynamics
Authors: Amanda Ricketts, Benjamin A. Clouter-Gergen, Anastasis Georgiou, Deborah Berhanu, Liam S. Morrissey
Figure caption: Radial distribution function (RDF) analyses performed in OVITO for the crystalline and amorphous albite and anorthite structures, showing the variation in atomic ordering between the two phases.
Paper: Powerful Lightning on Venus Constrained by Atmospheric NO
Authors: Tereza Constantinou, Oliver Shorttle, Paul B. Rimmer
Figure caption: Modeled NO mixing ratios in Venus’s atmosphere compared with observational constraints. (a) Comparison of atmospheric chemistry models. Our complete model (black dashed line) integrates the P. B. Rimmer et al. (2021) network with additional reactions from V. A. Krasnopolsky (2012) (Table 2). Other models shown include those from V. A. Krasnopolsky (2012; turquoise dashed), C. Bierson & X. Zhang (2020; orange dashed), L. Dai et al. (2024; blue dashed), and the original P. B. Rimmer et al. (2021) network without additions (pink dashed, primarily hidden under black dashed line). Gray shaded regions represent NO measurements from the TEXES spectrograph at NASA’s Infrared Telescope Facility (V. Krasnopolsky 2006) and upper limits derived from nondetections by VEx (A. Mahieux et al. 2024). All models exceed the upper limits in the cloud-top region (∼60–70 km), underscoring a persistent discrepancy between model predictions and observations. (b) Sensitivity of the complete network model to variations in the in-cloud eddy diffusion coefficient (100–1000 cm2 s−1). The nominal profile (black dashed) overpredicts NO abundances above the cloud layer, while reduced in-cloud mixing (colored lines) lowers NO to within the VEx upper limits. The eddy profiles used are plotted in Appendix Figure 5.
Paper: Powerful Lightning on Venus Constrained by Atmospheric NO
Authors: Tereza Constantinou, Oliver Shorttle, Paul B. Rimmer
Figure caption: Lightning energy and rate values consistent with the required lightning power for Venus. The best-fit curve (best agreement with observational constraints on atmospheric abundance of NO; orange line) is plotted as derived from our atmospheric photochemical-kinetic model, with in-cloud Kzz = 700 cm2 s−1. The broader possible power range, as determined from the minimum depletion flux from observational constraints and alternative in-cloud Kzz values, extends to higher energies and rates than the plotted range (yellow shaded area; Section 3). For reference, also plotted is the Earth’s average energy per lightning strike (C. R. Maggio et al. 2009) with the observed lightning rate (H. J. Christian et al. 2003) and the equivalent rate if the entire surface was only made up of land, without any oceans (G. Hodosán et al. 2016; lower and upper green circles on the left, respectively), and the average rate with the maximum energy per lightning strike (C. R. Maggio et al. 2009; right-most green circle). Also indicated are the global lightning flash rate of up to 320 s−1 inferred from whistler-mode waves (horizontal gray dotted line; R. A. Hart et al. 2022) and the minimum optical energy limit of 1.2 × 109 J from ground-based observations of optical flashes on Venus (vertical gray dotted line; V. Krasnopolsky 2006); neither are confirmed to be linked to lightning.
Paper: Powerful Lightning on Venus Constrained by Atmospheric NO
Authors: Tereza Constantinou, Oliver Shorttle, Paul B. Rimmer
Figure caption: Sensitivity of modeled NO mixing ratios to individual reactions in the chemical network. Profiles show the NO mixing ratio as a function of altitude when specific reactions (and their reverse reactions) are removed from the network to assess their impact. On the left are the complete profiles; on the right are the zoomed-in profiles of the cloud area where NO is depleted. The solid black line shows the baseline result with the full chemical network included. Gray shaded regions indicate observational constraints: NO measurements from the TEXES spectrograph (V. Krasnopolsky 2006) and upper limits from nondetections by VEx (A. Mahieux et al. 2024). The recombination reaction N + O ↔ NO was not removed; instead, its reaction rate was replaced with that of V. A. Krasnopolsky (2012) for comparison (the replacement rate coefficient is listed in Appendix Table 2).
Paper: Powerful Lightning on Venus Constrained by Atmospheric NO
Authors: Tereza Constantinou, Oliver Shorttle, Paul B. Rimmer
Figure caption: Vertical eddy diffusion profiles used as a function of altitude in Venus’s atmosphere. The nominal profile (turquoise) follows that of V. A. Krasnopolsky (2007) and P. B. Rimmer et al. (2021). Modified profiles vary the in-cloud eddy diffusion coefficient within the cloud layer (45–65 km altitude), adopting values of 100, 500, 700, and 1000 cm2 s−1 (blue, orange, green, and red, respectively). Below and above the cloud layer, all profiles follow the same nominal structure.
Paper: Powerful Lightning on Venus Constrained by Atmospheric NO
Authors: Tereza Constantinou, Oliver Shorttle, Paul B. Rimmer
Figure caption: Vertical profiles of the most abundant nitrogen-containing species as a function of altitude in our model. Left: nominal eddy diffusion profile used in P. B. Rimmer et al. (2021), which overestimates NO abundances relative to observational constraints. Right: modified eddy profile with reduced in-cloud diffusion (700 cm2 s−1), consistent with NO upper limits from VEx (A. Mahieux et al. 2024).
Paper: Powerful Lightning on Venus Constrained by Atmospheric NO
Authors: Tereza Constantinou, Oliver Shorttle, Paul B. Rimmer
Figure caption: Predicted vertical profiles of SO2, H2O, CO, OCS, O2, HCl, H2SO4, H2, SO, S3, S4, and H2S from three atmospheric chemistry models. The P. B. Rimmer et al. (2021) model is shown with a gray dashed line, the complete chemical network (P. B. Rimmer et al. 2021; updated with some NO reactions from V. A. Krasnopolsky 2012) with the nominal eddy profile is shown with a purple dashed line, and the complete network with a modified in-cloud (45–65 km) eddy diffusion coefficient of 700 cm2 s−1 is shown with a green dashed line. Observational constraints and upper limits for each species, compiled in P. B. Rimmer et al. (2021), are plotted in gray for comparison. The sulfuric acid profile includes both gaseous (H2SO4) and condensed (JH2SO4) phases.
Paper: Powerful Lightning on Venus Constrained by Atmospheric NO
Authors: Tereza Constantinou, Oliver Shorttle, Paul B. Rimmer
Figure caption: The rates of the dominant chemical reactions producing (top panels; dashed lines) and destroying (bottom panels; solid lines) NO as a function of altitude for each eddy profile: the nominal (left panels) and the modified eddy profile with in-cloud coefficients of 700 cm2 s−1 that meet observational constraints (right panels). Rates represent instantaneous values at the final time step for each altitude and do not capture the complete chemical history.
Paper: Powerful Lightning on Venus Constrained by Atmospheric NO
Authors: Tereza Constantinou, Oliver Shorttle, Paul B. Rimmer
Figure caption: The rates of the dominant chemical reactions producing (top panels; dashed lines) and destroying (bottom panels; solid lines) N2 as a function of altitude for each eddy profile: the nominal (left panels) and the modified eddy profile with in-cloud coefficients of 700 cm2 s−1 that meet observational constraints (right panels). Rates represent instantaneous values at the final time step for each altitude and do not capture the complete chemical history.
Paper: Powerful Lightning on Venus Constrained by Atmospheric NO
Authors: Tereza Constantinou, Oliver Shorttle, Paul B. Rimmer
Figure caption: The rates of the chemical reactions that make up the net depletion mechanism for NO as a function of altitude for each eddy profile: the nominal (left panel) and the modified eddy profile with in-cloud coefficients of 700 cm2 s−1 that meet observational constraints (right panel). Rates represent instantaneous values at the final time step for each altitude and do not capture the complete chemical history.
Paper: A High-precision, Differentiable Code for Solar System Ephemerides
Authors: Ben Cassese, Malena Rice, Tiger Lu
Figure caption: A comparison of accumulated errors between jorbit and IAS15 for a simple scale-free r = 1, P = 2π circular orbit of a tracer particle around a unit mass. Both integrators were run forward to the specified number of outbound orbits, then reversed back to zero. The absolute difference between the start and finish positions gives a measure of the error accumulated purely due to the numerical method. Here we have plotted half this distance to show the degree of error expected for an integration of a given length. Note that jorbit stays well below its 10−10 target for many hundreds of dynamical times, meaning numerical imprecision should never be the limiting factor in an orbit fit to real data. Brouwer’s law, where error ∝t3/2, is included for reference. ✎
Paper: A High-precision, Differentiable Code for Solar System Ephemerides
Authors: Ben Cassese, Malena Rice, Tiger Lu
Figure caption: Actual TESS data of TIC 438412198 and jorbit’s postdiction simulation of the total flux of minor planets, centered on the flyby of asteroid (1055) Tynka. Note that transient asteroids can produce both apparent dips and apparent spikes in SAP light curves. The initial dimming occurs when (1055) Tynka approaches a cluster of pixels in the “background” aperture used to determine the sky background but before it reaches the pixels composing the extraction aperture. The exact morphology of each minor planet/TIC interaction depends on the relative placement of the background aperture and extraction aperture and the minor planet’s trajectory. ✎
Paper: A High-precision, Differentiable Code for Solar System Ephemerides
Authors: Ben Cassese, Malena Rice, Tiger Lu
Figure caption: Simulated observations of and jorbit’s prediction for the maximum-likelihood orbit of (274301) Wikipedia. To demonstrate jorbit’s ability to compute the likelihood of a set of parameters and the derivatives of that likelihood, we show the results of holding all other best-fit parameters fixed while varying the semimajor axis. The first and second derivatives were computed via automatic differentiation of the fully dynamical model (i.e., it was propagated through the IAS15-integrated, perturbers-included, GR-included N-body simulation), not through finite differencing or manual algebra. To guide the eye, the vertical line marks the semimajor axis of the fit, while the horizontal line marks zero derivative of the likelihood with respect to semimajor axis. ✎
Paper: A High-precision, Differentiable Code for Solar System Ephemerides
Authors: Ben Cassese, Malena Rice, Tiger Lu
Figure caption: Example performance of the “DoubleDouble” precision integrator. Note that we can tune the order of the integrator based on the number of substeps, and we can achieve relative position errors near roughly 10−32, about 16 orders of magnitude below the best precision available to double-precision operations. Were we using single-precision operations, like those available on most GPUs, the DoubleDouble operations would level out at 10−16. The single-orbit errors from REBOUND’s implementation of IAS15 and jorbit, both of which use seven substeps, are shown as horizontal lines since both use adaptive, rather than fixed, time steps. ✎
Paper: A High-precision, Differentiable Code for Solar System Ephemerides
Authors: Ben Cassese, Malena Rice, Tiger Lu
Figure caption: Top: the difference in predicted sky positions for 100 randomly sampled objects as calculated by JPL Horizons and jorbit. Bottom: the same data on a log scale alongside the difference in sky positions of the same objects at the same times, as viewed from Kitt Peak and Palomar Mountain and predicted by Horizons. After 10 yr of integration, the median disagreement between Horizons and jorbit was 0.13 mas, while the median effect of the parallax between the observatories was 209 mas. ✎
Paper: Topographic Relaxation of Complex Impact Craters in a Clathrate Crust on Titan
Authors: Gwendolyn Brouwer, Lauren Schurmeier, Sarah Fagents, Veronica Bray, Catherine Neish, Emily Costello
Figure caption: Simulated crater topography of the 85 and 100 km diameter craters and four different clathrate layer thicknesses. From top to bottom, the clathrate layer thickness increases. Line colors correspond to initial crater shape, with a simplified bowl-shaped crater shown in purple, a flat-floored crater shown in black, and a central pit shape shown in teal. Dotted lines correspond to original, prerelaxation crater shapes, and solid lines correspond to the crater shape after 1 billion yr. Gray transparent boxes represent the depth range, measured from the background terrain (terrain depth) to the lowest point on the crater floor, including their positive and negative errors, of similar-sized craters on Titan: Soi (D = 85 km), Selk (D = 84 km), Sinlap (D = 88 km), Hano (D = 105 km), and Afekan (D = 115 km) (J. E. Hedgepeth et al. 2020).
Paper: Topographic Relaxation of Complex Impact Craters in a Clathrate Crust on Titan
Authors: Gwendolyn Brouwer, Lauren Schurmeier, Sarah Fagents, Veronica Bray, Catherine Neish, Emily Costello
Figure caption: Crater shapes before and after 1 billion yr of topographic relaxation for a 40 km diameter crater and two different clathrate layer thicknesses. Note that we omit the 15 and 20 km thick clathrate layers from this plot, given that they do not relax significantly. Each column corresponds to a different central feature: central peak crater (left) and central pit crater (right). From top to bottom, the clathrate layer thickness increases (ice shell temperature decreases from top to bottom). Line colors correspond to initial crater shape, with a simplified bowl-shaped crater shown in purple, a flat-floored crater shown in black, and a central peak or pit shape shown in teal. Dotted lines correspond to the original, prerelaxation crater shapes, and solid lines correspond to the crater shape after 1 billion yr. Gray transparent boxes represent the depth range, measured from the background terrain (terrain depth) to the lowest point on the crater floor, including their positive and negative errors, of similar-sized craters on Titan: Ihi (D = 41 km) and Ksa (D = 45 km) (J. E. Hedgepeth et al. 2020). Note that the crater floor widths of the central peak craters ((a) and (b)) are narrower than the central pit craters ((c) and (d)). Thus, the flat-floored simulations corresponding to the central peak craters relax less than those of the central pit craters. Initial floor widths and other crater dimensions are reported in Table 1.
Paper: Topographic Relaxation of Complex Impact Craters in a Clathrate Crust on Titan
Authors: Gwendolyn Brouwer, Lauren Schurmeier, Sarah Fagents, Veronica Bray, Catherine Neish, Emily Costello
Figure caption: Cassini SAR images of Titan’s impact craters overlaid on Cassini ISS images. (a) Forseti, (b) Afekan, (c) Hano, (d) Sinlap, (e) Soi, (f) Selk, (g) Ksa, (h) Ihi. North is to the top of each image. White lines in (c), (e), and (f) show the location of the elevation profiles in Figure 3.
Paper: Topographic Relaxation of Complex Impact Craters in a Clathrate Crust on Titan
Authors: Gwendolyn Brouwer, Lauren Schurmeier, Sarah Fagents, Veronica Bray, Catherine Neish, Emily Costello
Figure caption: Topography profiles of Titan’s impact craters that have SARTopo coverage through their centers; (a) Soi, (b) Selk, and (c) Hano. Arrows on topographic profiles indicate the location of the crater rims. White lines crossing craters in Figure 2 correspond to the location of profiles.
Paper: Topographic Relaxation of Complex Impact Craters in a Clathrate Crust on Titan
Authors: Gwendolyn Brouwer, Lauren Schurmeier, Sarah Fagents, Veronica Bray, Catherine Neish, Emily Costello
Figure caption: Stereo topography of (a) Ihi, (b) Ksa, and (c) Soi overlain on SAR and ISS imagery. White lines correspond to topographic profiles plotted in Figure 11. Stereo images courtesy of Randy Kirk.
Paper: Topographic Relaxation of Complex Impact Craters in a Clathrate Crust on Titan
Authors: Gwendolyn Brouwer, Lauren Schurmeier, Sarah Fagents, Veronica Bray, Catherine Neish, Emily Costello
Figure caption: Crater rim depth vs. diameter of Ganymede’s fresh craters from P. M. Schenk (2002) and the nine craters on Titan that have topographic coverage. The maroon line shows the current observed trend line of Ganymede’s large complex craters, and the teal line shows the extrapolated trend of small complex craters (L. R. Schurmeier et al. 2024). Rim depth is the distance from the top of the rim to the crater floor. Titan rim depths and diameters are from J. E. Hedgepeth et al. (2020).
Paper: Topographic Relaxation of Complex Impact Craters in a Clathrate Crust on Titan
Authors: Gwendolyn Brouwer, Lauren Schurmeier, Sarah Fagents, Veronica Bray, Catherine Neish, Emily Costello
Figure caption: Dimensions of a central pit crater. D is the crater diameter, Hr is the rim height, d is the crater depth, Hpr is the pit-rim height, Dpr is the pit-rim width, Dp is the pit width, and dp is the pit depth.
Paper: JWST Reveals Varied Origins between Jupiter’s Irregular Satellites
Authors: Benjamin N. L. Sharkey, Andrew S. Rivkin, Richard J. Cartwright, Bryan J. Holler, Joshua P. Emery, Cristina Thomas
Figure caption: Left: processed relative reflectances for all observed targets in JWST GO 4028, labeled according to groupings identified in the text. Right: continuum-divided reflectances using a polynomial of order 2–4 fit on either side of major absorption bands. Objects are normalized to have reflectance equal to 1 at 2.5 μm and displayed with offsets for ease of comparison. Targets are arranged according to spectral characteristics, not orbital groupings. Major band complexes near 3.0 μm differentiate between the different material categories. The steep red slopes of Carme, Sinope, and Themisto (Group 1) are similar to D-type asteroids or “red”-type Jovian Trojans. Ananke (Group 2) shows a broad feature at similar wavelengths to Lysithea and Pasiphae but with a very different, rounded shape. Lysithea and Pasiphae (Group 3) show deep features centered on 3.0 μm similar to less red Jovian Trojans. Himalia and Elara (Group 4) display a clear 2.7 μm feature, detected previously on aqueously altered inner solar system materials but never identified in the Jovian system.
Paper: JWST Reveals Varied Origins between Jupiter’s Irregular Satellites
Authors: Benjamin N. L. Sharkey, Andrew S. Rivkin, Richard J. Cartwright, Bryan J. Holler, Joshua P. Emery, Cristina Thomas
Figure caption: Top: estimated thermal flux (data points) and resulting NEATM best-fit thermal model (blue curve) for irregular satellite Lysithea. Fits were performed by varying target albedo and beaming parameter to reproduce the cut-on wavelength where measurable thermal emission begins (typically near 4.0 μm, related to the observed surface’s temperature), as well as the shape and magnitude of the thermal fluxes at longer wavelengths. Finalized reflectance spectra are created by subtraction of the blue curve from the processed, flux-calibrated spectra. Bottom: thermal flux residuals from best-fit NEATM model.
Paper: JWST Reveals Varied Origins between Jupiter’s Irregular Satellites
Authors: Benjamin N. L. Sharkey, Andrew S. Rivkin, Richard J. Cartwright, Bryan J. Holler, Joshua P. Emery, Cristina Thomas
Figure caption: Continuum-divided reflectance of the 4.15–4.40 μm region of Himalia and Elara. They are compared with previous observations of Jovian Trojan Eurybates, which was reprocessed using the same reduction pipeline. The two irregular satellites show features near 4.27 μm that are shifted +∼0.01 μm compared to Eurybates. The features on Himalia, Elara, and Eurybates are similar to but measurably distinct from the CO2 bands observed on Europa and Callisto, which display minima at 4.25 and 4.27 μm.
Paper: JWST Reveals Varied Origins between Jupiter’s Irregular Satellites
Authors: Benjamin N. L. Sharkey, Andrew S. Rivkin, Richard J. Cartwright, Bryan J. Holler, Joshua P. Emery, Cristina Thomas
Figure caption: Himalia compared with other small solar system bodies that show the 3.05 μm. While Himalia shows major spectral features similar to Ceres (H. Kurokawa et al. 2020) at 2.7 and 3.05 μm, the differing relative strengths of these bands suggest novel materials on Himalia that have not been cataloged on any other bodies at present. Faint features from 3.3 to 3.6 μm seen on 67P (A. Raponi et al. 2020) are more similar to Himalia than corresponding deep and broad features on Ceres.
Paper: JWST Reveals Varied Origins between Jupiter’s Irregular Satellites
Authors: Benjamin N. L. Sharkey, Andrew S. Rivkin, Richard J. Cartwright, Bryan J. Holler, Joshua P. Emery, Cristina Thomas
Figure caption: Comparison of the 3 μm band complex on Lysithea (prograde, Himalia group) and Pasiphae (retrograde, Pasiphae group). The centers and depths of these features are highly similar. Lysithea includes an additional narrow absorption near 2.63 μm, and Pasiphae includes a narrow absorption at 3.01 μm that may also be present on Lysithea.
Paper: JWST Reveals Varied Origins between Jupiter’s Irregular Satellites
Authors: Benjamin N. L. Sharkey, Andrew S. Rivkin, Richard J. Cartwright, Bryan J. Holler, Joshua P. Emery, Cristina Thomas
Figure caption: Irregular satellite orbital inclinations and semimajor axes (normalized to Jupiter’s Hill radius). Family groupings are given as indicated. The prograde population is dominated in mass and number by the Himalia family. The retrograde population is categorized into three orbital families, with the more widely dispersed Pasiphae and Ananke families and the more tightly grouped Carme family. This work studies the Himalia, Carme, Pasiphae, and Ananke families, as well as the isolated satellite Themisto. Orbital parameters are from JPL Horizons.
Paper: Surface Binding Energies for Amorphous Plagioclase Feldspar Calculated Using Molecular Dynamics
Authors: Amanda Ricketts, Benjamin A. Clouter-Gergen, Anastasis Georgiou, Deborah Berhanu, Liam S. Morrissey
Figure caption: Albite (A) and anorthite (B) MD substrate surfaces.
Paper: Surface Binding Energies for Amorphous Plagioclase Feldspar Calculated Using Molecular Dynamics
Authors: Amanda Ricketts, Benjamin A. Clouter-Gergen, Anastasis Georgiou, Deborah Berhanu, Liam S. Morrissey
Figure caption: Albite (A) and anorthite (B) surface atoms only.