adsabs/AstroCLIMB huggingface dataset:
Paper: Establishing a Best Practice for SDTrimSP Simulations of Solar Wind Ion Sputtering
Authors: Liam S. Morrissey, Micah J. Schaible, Orenthal J. Tucker, Paul S. Szabo, Giovanni Bacon, Rosemary M. Killen, Daniel W. Savin
Figure caption: Simulations for vacancies/ion as a function of depth for (A) different incidence angle cases using 1 keV H+ impacts, (B) different H+ impact energy cases using a cosine distribution of incidence angles, and (C) different SW compositions using 1 keV amu−1 impacts with a cosine distribution of incidence angles. Vacancy counts were independent of O SBE (see text).
Paper: Establishing a Best Practice for SDTrimSP Simulations of Solar Wind Ion Sputtering
Authors: Liam S. Morrissey, Micah J. Schaible, Orenthal J. Tucker, Paul S. Szabo, Giovanni Bacon, Rosemary M. Killen, Daniel W. Savin
Figure caption: Anorthite elemental surface composition ratio as a function of fluence using O SBEs of (A) 1 eV, (B) 2.6 eV, and (C) 6.5 eV. Simulations were conducted using 1 keV H+ impacting at normal incidence. The jaggedness of the curves is due to the Monte Carlo nature of the simulations.
Paper: Establishing a Best Practice for SDTrimSP Simulations of Solar Wind Ion Sputtering
Authors: Liam S. Morrissey, Micah J. Schaible, Orenthal J. Tucker, Paul S. Szabo, Giovanni Bacon, Rosemary M. Killen, Daniel W. Savin
Figure caption: Energy distribution of sputtered O from anorthite as a function of emission energy for different simulation setups. Simulations were conducted using 1 keV H+ impacts. The jaggedness of the curves is due to the Monte Carlo nature of the simulations.
Paper: Examining Uranus’ ζ Ring in Voyager 2 Wide-angle Camera Observations: Quantifying the Ring’s Structure in 1986 and Its Modifications Prior to the Year 2007
Authors: M. M. Hedman, I. Regan, T. Becker, S. M. Brooks, I. de Pater, M. Showalter
Figure caption: Plot showing the available brightness profiles of the ζ ring, with lighter lines showing the uncertainties in each profile. Note that all the Voyager profiles are scaled by different factors to account for the varying phase angles assuming the brightness of the ring follows the three-component Henyey–Greenstein function shown in Figure 10, while the Keck observation is scaled by a factor consistent with the red color of many dusty rings.
Paper: Establishing a Best Practice for SDTrimSP Simulations of Solar Wind Ion Sputtering
Authors: Liam S. Morrissey, Micah J. Schaible, Orenthal J. Tucker, Paul S. Szabo, Giovanni Bacon, Rosemary M. Killen, Daniel W. Savin
Figure caption: Measured ion energy distribution of H+ in the slow solar wind (blue curve; Poppe et al. 2018), compared with the 1 keV approximation (black dashed line), and the mean of the measured ion energy distribution (red dotted line).
Paper: Examining Uranus’ ζ Ring in Voyager 2 Wide-angle Camera Observations: Quantifying the Ring’s Structure in 1986 and Its Modifications Prior to the Year 2007
Authors: M. M. Hedman, I. Regan, T. Becker, S. M. Brooks, I. de Pater, M. Showalter
Figure caption: Profiles of Saturn’s G and D rings derived from Cassini images at phase angles similar to the high-phase Voyager 2 images of the ζ ring. The top panel shows a profile derived from Figure 12 of Hedman et al. (2012), which was also obtained at a phase angle of around 146°. The vertical line marks the location where the Voyager 2 spacecraft passed through Saturn’s ring-plane. The bottom two panels show a background-subtracted profile of Saturn’s inner D ring derived from Cassini images derived from an image sequence containing 62 images obtained at phase angles between 145° and 149°. The two panels have different vertical scales to show better the signal at the location of the outermost ring-plane crossing during Cassini’s Grand Finale (marked with a dashed line). The profiles for the ζ and D ring are also compared with an exponential model fit. Note that data for both these rings are vertically shifted so that the exponential trend asymptotes to zero. The ζ ring profile is offset by 1 × 10−6 relative to the version shown in Figure 6, while the D ring profile is offset by 0.1 × 10−6.
Paper: Examining Uranus’ ζ Ring in Voyager 2 Wide-angle Camera Observations: Quantifying the Ring’s Structure in 1986 and Its Modifications Prior to the Year 2007
Authors: M. M. Hedman, I. Regan, T. Becker, S. M. Brooks, I. de Pater, M. Showalter
Figure caption: Phase curves showing the peak brightness of the ζ ring and other diffuse rings as a function of observed phase angle. The ζ ring data are compared with data from Jupiter’s Main ring (Throop et al. 2004), Saturn’s G ring (Hedman & Stark 2015), and Uranus’ ν ring (Showalter & Lissauer 2006). The curve through the G ring data corresponds to the best-fit three-component Henyey–Greenstein function from Hedman & Stark (2015), and the dotted curve shows the same theoretical phase function scaled by a factor of 5.5 to best fit the three ζ ring data points.
Paper: Examining Uranus’ ζ Ring in Voyager 2 Wide-angle Camera Observations: Quantifying the Ring’s Structure in 1986 and Its Modifications Prior to the Year 2007
Authors: M. M. Hedman, I. Regan, T. Becker, S. M. Brooks, I. de Pater, M. Showalter
Figure caption: Maps of the inner ring system derived from the high-phase Voyager 2 observations. Each map shows the brightness vs. ring-plane radius and inertial longitude, and the green dotted line indicates the projected location of the planet’s limb. The limb position varies with longitude because the system was observed at a ring opening angle of around 55°, so the spherical planet is projected into an oval shape on the ring-plane. Note the images have all been stretched to show better the regions beyond the planet’s dark limb (the ring actually extends all the way around the planet, see Figure 1). The ζ ring is the bright band centered around 37,500 km in all the maps. There is no obvious ring material interior to the ζ ring in these images.
Paper: Examining Uranus’ ζ Ring in Voyager 2 Wide-angle Camera Observations: Quantifying the Ring’s Structure in 1986 and Its Modifications Prior to the Year 2007
Authors: M. M. Hedman, I. Regan, T. Becker, S. M. Brooks, I. de Pater, M. Showalter
Figure caption: Plots of Q scat f as a function of particle size s computed from Mie theory assuming a wavelength of 0.46 μm for three phase angles relevant to the Voyager 2 Uranus observations and for three different optical constants. These curves were computed using the IDL code mie_single and the phase functions from that code were divided by four to ensure proper normalization. These parameters have also been smoothed to account for the finite bandpass of the camera. Note that the optical constants in the top panel correspond to those of pure water ice at optical wavelengths, while those in the bottom panel are for amorphous carbon. The middle panel uses intermediate optical constants between these two extremes.
Paper: Examining Uranus’ ζ Ring in Voyager 2 Wide-angle Camera Observations: Quantifying the Ring’s Structure in 1986 and Its Modifications Prior to the Year 2007
Authors: M. M. Hedman, I. Regan, T. Becker, S. M. Brooks, I. de Pater, M. Showalter
Figure caption: Example images from the high-phase observations of Uranus containing the ζ ring. The left panels show individual images from each of the three image sets. The only visible object in each of these images is the narrow lit crescent of Uranus (compare to Figure 1). The middle panels show the average image used to remove background stray light patterns. In these images Uranus itself falls near the top of the frame, but there are also faint crescents in the center of these images. These are artifacts corresponding to bright regions of earlier images. The right panel shows the left panels after subtracting the background image. Note the greatly reduced stray light patterns over most of the image. The ζ ring is still too faint to be seen in most of these individual images.
Paper: Examining Uranus’ ζ Ring in Voyager 2 Wide-angle Camera Observations: Quantifying the Ring’s Structure in 1986 and Its Modifications Prior to the Year 2007
Authors: M. M. Hedman, I. Regan, T. Becker, S. M. Brooks, I. de Pater, M. Showalter
Figure caption: Constraints on the absolute brightness of the ζring’s inner flank based on the observed brightness differences between locations just beyond Uranus’ dark limb and the dark side of Uranus itself. Each point in this plot gives the difference in the average μ I/F values between regions 500 and 1500 km on either side of the predicted position of the planet’s limb for a 10° wide longitude bin, with positive values indicating the ring region is brighter than the dark side of Uranus. The horizontal location of each point corresponds to the mean radial position of the selected region outside the limb, and the error bars correspond to 1 standard deviation uncertainties. Note the nonzero differences probably primarily reflect residual instrumental backgrounds rather than real astronomical signals.
Paper: Examining Uranus’ ζ Ring in Voyager 2 Wide-angle Camera Observations: Quantifying the Ring’s Structure in 1986 and Its Modifications Prior to the Year 2007
Authors: M. M. Hedman, I. Regan, T. Becker, S. M. Brooks, I. de Pater, M. Showalter
Figure caption: Radial brightness profile of the ζ ring derived from the high-phase Voyager 2 images. Gray diamonds show the profiles from individual columns in the combined map that are beyond Uranus’ limb. The solid line is the average of all data beyond the planet’s limb. Note the profile has been arbitrarily offset to have an average of zero between 28,000 and 32,000 km. The brightness fluctuations interior to 32,000 km are likely due to instrumental artifacts.
Paper: Examining Uranus’ ζ Ring in Voyager 2 Wide-angle Camera Observations: Quantifying the Ring’s Structure in 1986 and Its Modifications Prior to the Year 2007
Authors: M. M. Hedman, I. Regan, T. Becker, S. M. Brooks, I. de Pater, M. Showalter
Figure caption: Evidence for the ζ ring in the low-resolution, low-phase Voyager images. The points come from the background-subtracted, coadded radial brightness profiles with 500 km radial sampling and covering 10° in inertial longitude. The line shows the average of all these profiles. While the S/N is rather low, there is a weak peak centered around 37,500 km with an amplitude around 3 × 10−6, consistent with the moderate-phase profile shown in Figure 2.
Paper: Examining Uranus’ ζ Ring in Voyager 2 Wide-angle Camera Observations: Quantifying the Ring’s Structure in 1986 and Its Modifications Prior to the Year 2007
Authors: M. M. Hedman, I. Regan, T. Becker, S. M. Brooks, I. de Pater, M. Showalter
Figure caption: Two of the low-phase Voyager 2 images that might contain a weak signal from the ζ ring. In both images, Uranus itself is positioned at one corner of the field of view, and the dense main rings can be seen extending toward the center of the frame. The right image contains after-images of the planet’s bright disk in all four corners from previous exposures. The ζ ring would fall between the visible rings and the planet, and is not clearly visible in either of these individual images.
Paper: New Insights into Variations in Enceladus Plume Particle Launch Velocities from Cassini-VIMS Spectral Data
Authors: H. Sharma, M. M. Hedman, S. Vahidinia
Figure caption: The plume’s equivalent width at Z = 0.5 (altitude z = 85 km) as a function of orbital phase for the three dates and four different wavelength values. The plume’s maximum brightness around the orbital phase of 180° is consistent at all wavelengths. Additionally, note that the brightness of the plume was higher on August 2 than it was on 2017 June 18 or August 28 at all wavelengths.
Paper: New Insights into Variations in Enceladus Plume Particle Launch Velocities from Cassini-VIMS Spectral Data
Authors: H. Sharma, M. M. Hedman, S. Vahidinia
Figure caption: The integrated brightness of the plume (equivalent width) as a function of the parameter Z (=﹩{[z/({r}_{{\rm{E}}}+z)]}^{1/2}﹩, where r E = 250 km is the radius of Enceladus and z is the plume’s altitude) and launch velocity v (calculated using Equation (1)). The equivalent widths for the three different dates 2017 June 18, August 2, and August 28 are plotted (in blue, green, and red, respectively) at similar orbital phase value of ≃200° and four different wavelengths. The equivalent width is fit to a linear function of Z. Note that the brightness of the plume is higher for the observation on August 2 (in green) than for the observations on the other dates.
Paper: New Insights into Variations in Enceladus Plume Particle Launch Velocities from Cassini-VIMS Spectral Data
Authors: H. Sharma, M. M. Hedman, S. Vahidinia
Figure caption: Example Enceladus plume spectra, showing the plume’s equivalent width (in km; see Section 2.2) vs. wavelength (in μm) at similar orbital phases for all three orbits. An orbital phase close to 200° is chosen, as the signal is strongest closer to the plume maxima at apoapsis. The points show the equivalent widths for individual spectral channels (after removing outliers before 2.5 μm and after 3.3 μm), and the line plot with error bars shows the data after averaging each spectrum over eight wavelength channels.
Paper: New Insights into Variations in Enceladus Plume Particle Launch Velocities from Cassini-VIMS Spectral Data
Authors: H. Sharma, M. M. Hedman, S. Vahidinia
Figure caption: The difference in the plume’s equivalent width at different wavelengths and at Z = 0.5 (altitude z = 85 km) as a function of orbital phase, grouped by the Orbit no./Date. Note that on August 2 the brightness variations are nearly identical at all wavelengths; spectral trends in the plume’s brightness can be seen in both the June 18 and August 28 data at orbital phases below 180°.
Paper: New Insights into Variations in Enceladus Plume Particle Launch Velocities from Cassini-VIMS Spectral Data
Authors: H. Sharma, M. M. Hedman, S. Vahidinia
Figure caption: Typical launch velocity (in m s−1) for three different orbits derived using Equation (3) as a function of orbital phase. Note that the typical launch velocity is higher on August 28 than on June 18 or August 2 at lower wavelengths of 1.2 μm. The typical launch velocity also generally increases with orbital phase. Note also that the variations in the typical launch velocity with wavelength are relatively small.
Paper: New Insights into Variations in Enceladus Plume Particle Launch Velocities from Cassini-VIMS Spectral Data
Authors: H. Sharma, M. M. Hedman, S. Vahidinia
Figure caption: The spatial geometry of the reprojected VIMS cubes. On the left is a sample image of Enceladus and its plume at a wavelength of 1.03 μm derived from a single reprojected cube (CM_1876456410_1) obtained at an orbital phase of 200° during Orbit no. 279 on June 18. On the right is the geometry of the reprojected VIMS cubes. The reprojected data plane is defined using Cartesian coordinates [x, y], with Enceladus at the center at [0, 0], and the negative y-axis is aligned with the moon’s spin axis. The left vertical axis and the horizontal axis show the [x, y] coordinates for the cube. For the right vertical axis of the figure the y coordinate has been converted into altitude above Enceladus’s south pole (z = −(250 + y) in km). The outlined regions on either side correspond to the region used to calculate background signal levels.
Paper: New Insights into Variations in Enceladus Plume Particle Launch Velocities from Cassini-VIMS Spectral Data
Authors: H. Sharma, M. M. Hedman, S. Vahidinia
Figure caption: The plume’s equivalent width at Z = 0.5 (altitude z = 85 km, same as Figure 5) as a function of orbital phase, grouped by the Orbit no./Date instead of wavelength. Note that on August 2 the brightness variations are nearly identical at all wavelengths; spectral trends in the plume’s brightness can be seen in both the June 18 and August 28 data at orbital phases below 180°.
Paper: Jupiter’s Early Luminosity May Have Driven off Io’s Initial Water Inventory
Authors: Carver J. Bierson, Jonathan J. Fortney, Kevin T. Trinh, Mikhail A. Kreslavsky
Figure caption: The mass-loss rates are highly temperature dependent. Times prior to 1 Myr are shaded gray as these luminosity values are higher than what is expected after the proto-Jovian disk dissipates. These early times are shown for their value in understanding the general model behavior. (a) Luminosity of Jupiter in units of solar luminosity from Fortney et al. (2011). (b) Equilibrium temperatures calculated using Equation (1). Solid lines include greenhouse heating while dashed curves assume an optically thin atmosphere. (c) Mass of the potential primordial ice shell divided by the instantaneous mass-loss rate. The solid black line is a 1:1 line. Where the satellite values lie below the black line all the ice could be lost. For Jovian luminosity values between 1 and 3 Myr, Io could lose its water inventory (with greenhouse heating) but Europa and Ganymede would not.
Paper: Jupiter’s Early Luminosity May Have Driven off Io’s Initial Water Inventory
Authors: Carver J. Bierson, Jonathan J. Fortney, Kevin T. Trinh, Mikhail A. Kreslavsky
Figure caption: Jupiter’s early luminosity can cause significant mass loss from Io and Europa while preserving an ice-rich Ganymede if the start time is 0.5 Myr and they maintain optically thin atmospheres. If the atmospheres experience a runaway greenhouse Io could not retain any ice until after 3 Myr (L  J  < 6 × 10−6 L ☉). Plotted is the total (integrated) mass lost as a function of the start time of the integration. Times prior to 1 Myr are shaded gray as these luminosity values are higher than what is expected after the proto-Jovian disk dissipates (Fortney et al. 2011).
Paper: Jupiter’s Early Luminosity May Have Driven off Io’s Initial Water Inventory
Authors: Carver J. Bierson, Jonathan J. Fortney, Kevin T. Trinh, Mikhail A. Kreslavsky
Figure caption: Summary of the possible role of Jupiter’s radiation in the evolution of the Galilean satellites. (a) The satellites accrete in the proto-Jovian disk. Io and Europa’s initial water inventory may or may not be lost during this stage by processes suggested in previous work (Ronnet et al. 2017; Bierson & Nimmo 2020). (b) After the disk dissipates, radiation heating from Jupiter could potentially cause the removal of Io and Europa’s remaining water inventory. (c) Tidal heating causes Io’s silicates to dehydrate while Jupiter is still luminous and thus this water inventory is lost. (d) Europa does not dehydrate until after Jupiter has dimmed resulting in the present ocean.
Paper: Jupiter’s Early Luminosity May Have Driven off Io’s Initial Water Inventory
Authors: Carver J. Bierson, Jonathan J. Fortney, Kevin T. Trinh, Mikhail A. Kreslavsky
Figure caption: Example of the outgoing energy flux due to mass loss and radiate cooling according to Equation (1) for Io. Above about 350 K the energy from mass loss dominates over radiative cooling. Also shown are values for the modern solar flux and Jupiter’s flux at three different times. Note that these incoming fluxes do not include the impact of albedo or greenhouse heating.
Paper: Jupiter’s Early Luminosity May Have Driven off Io’s Initial Water Inventory
Authors: Carver J. Bierson, Jonathan J. Fortney, Kevin T. Trinh, Mikhail A. Kreslavsky
Figure caption: Same as Figure 3 but using the luminosity of D’Angelo et al. (2021). The key result of this work, that Io’s water inventory can be lost for times less than ∼3 Myr, still holds for this luminosity model.
Paper: Jupiter’s Early Luminosity May Have Driven off Io’s Initial Water Inventory
Authors: Carver J. Bierson, Jonathan J. Fortney, Kevin T. Trinh, Mikhail A. Kreslavsky
Figure caption: Same as Figure 2 but using the luminosity of D’Angelo et al. (2021). The high initial luminosity is enough to produce rapid volatile loss from Io but not the other satellites, as shown by panel (c).
Paper: Jupiter’s Early Luminosity May Have Driven off Io’s Initial Water Inventory
Authors: Carver J. Bierson, Jonathan J. Fortney, Kevin T. Trinh, Mikhail A. Kreslavsky
Figure caption: Comparison of Jupiter’s luminosity from the models of Fortney et al. (2011) and D’Angelo et al. (2021).
Paper: The Timeline of Early Lunar Bombardment Constrained by the Evolving Distributions of Differently Aged Melt
Authors: Tiantian Liu, Greg Michael, Kai Wünnemann
Figure caption: Integrated melt age distribution at Apollo sampling sites. (a) U–Pb datings of Apollo 12, 14, 15, 16, 17 samples (Vanderliek et al. 2021), where the black curve is the first-order spline interpolation of the gray histogram. The italic number indicates the number of datings. Panels (b1) and (c1) are the model-derived melt age distributions while considering the basin list of Orgel et al. (2018) and the addition of newly detected pre-Nectarian basins (Conrad et al. 2018), respectively. The considered basins in panel (c1) are 12 more than in panel (b1). The error bars indicate the standard deviation of 10 times Monte Carlo simulations. Their age distribution of basin-sourced melt with an age >4.1 Ga (indicated by the green zones in panels (b1) and (c1)) is shown in panels (b2) and (c2), respectively.
Paper: The Timeline of Early Lunar Bombardment Constrained by the Evolving Distributions of Differently Aged Melt
Authors: Tiantian Liu, Greg Michael, Kai Wünnemann
Figure caption: Abundance of pre-Nectarian melt relative to all the materials in the top 5 m when considering the basin list of Orgel et al. (2018; top panel) and an addition of newly detected pre-Nectarian basins (Conrad et al. 2018; bottom panel). Abundances below 0.01 are shown in gray, and those above 0.10 are shown in dark red. The red crosses point out the location of so-far-accomplished sample return missions (Chang’e-5, Apollo, and Luna). The black curves outline the boundary of maria where the surface has been filled with volcanic materials.
Paper: The Timeline of Early Lunar Bombardment Constrained by the Evolving Distributions of Differently Aged Melt
Authors: Tiantian Liu, Greg Michael, Kai Wünnemann
Figure caption: Distribution of basin D and D  t , where the known D  t  (black circles) is derived from Miljković et al. (2016) and Wieczorek & Phillips (1999). The unknown D  t  (red circles) is estimated based on a liner fit of the known D and D  t  (black circles).
Paper: The Timeline of Early Lunar Bombardment Constrained by the Evolving Distributions of Differently Aged Melt
Authors: Tiantian Liu, Greg Michael, Kai Wünnemann
Figure caption: Age distribution of basin and nonbasin impact melt at the Apollo sampling sites in the top 5 m.
Paper: The Timeline of Early Lunar Bombardment Constrained by the Evolving Distributions of Differently Aged Melt
Authors: Tiantian Liu, Greg Michael, Kai Wünnemann
Figure caption: Cumulative number of generated craters considering impact rate function of tail-end, sawtooth, and terminal cataclysm.
Paper: Thermal Properties of the Leading Hemisphere of Callisto Inferred from ALMA Observations
Authors: Maria Camarca, Katherine de Kleer, Bryan Butler, Alex B. Akins, Alexander Thelen, Imke de Pater, Mark A. Gurwell, Arielle Moullet
Figure caption: (Left) Calibrated ALMA Band 7 (0.87 mm/343 GHz) image of Callisto’s leading hemisphere. (Right) Result of subtracting a sample Lambertian disk from the left panel to highlight the difference in T  b  across the disk. In both images, the ellipse in the lower left corner represents the FWHM of the synthesized ALMA beam. The latitude/longitude grid is spaced at 30° increments, and the 0° longitude line is marked with dashes. Callisto’s north pole is aligned with the image axis. Notably, the Valhalla impact crater appears slightly colder than other disk regions viewed at similar incident and emission angles. The data behind Figure 1 (left) are available in Tar: FITS files format.(The data used to create this figure are available.)