adsabs/AstroCLIMB huggingface dataset:
Paper: Mixing of Condensable Constituents with H–He during the Formation and Evolution of Jupiter
Authors: David J. Stevenson, Peter Bodenheimer, Jack J. Lissauer, Gennaro D'Angelo
Figure caption: Temperature distribution at three different epochs of evolution: end of Phase IV (3.14 × 106 yr), end of Phase V (13.3 × 106 yr), and current age. The color bar renders the logarithm of the heavy-element mass fraction. Uniform-composition layers correspond to portions of the curves of uniform colors. Note that the temperatures T  c  at the inner edge of the outer core are comparable at t = 3.14 × 106 yr and t = 4.57 × 109 yr (see Table 1).
Paper: Mixing of Condensable Constituents with H–He during the Formation and Evolution of Jupiter
Authors: David J. Stevenson, Peter Bodenheimer, Jack J. Lissauer, Gennaro D'Angelo
Figure caption: Left: planet growth as a function of time, throughout formation. The curves represent total, heavy-element, and H–He mass, as indicated in the legend. The five filled circles indicate the end of Phases I–V, as labeled. Right: same quantities as in the left panel, but masses vs. time are illustrated on linear scales during Phases III and IV only. Filled and open circles indicate the end of the phases on each curve. The gas accretion is smooth across the transition between Phases II and III (M  XY  = M  Z ) and increases during Phase III. ﹩{\dot{M}}_{{XY}}﹩ declines as the planet mass increases during Phase IV.
Paper: Mixing of Condensable Constituents with H–He during the Formation and Evolution of Jupiter
Authors: David J. Stevenson, Peter Bodenheimer, Jack J. Lissauer, Gennaro D'Angelo
Figure caption: Planet radius, R  p , during the isolation phase and up to the current age, obtained from our standard model (as indicated). The planet’s volume contracts nearly 8 times during this period. The final radius differs by less than 2% from Jupiter’s radius, R J (open circle). Also plotted is the radius obtained from Run LowZ, with lower final M  Z , discussed in Section 3.5, and from one of the models of D’Angelo et al. (2021), in which heavy elements sediment to the core. Filled symbols mark the end of formation: circles for the end of Phase IV, and square for the end of Phase V.
Paper: Mixing of Condensable Constituents with H–He during the Formation and Evolution of Jupiter
Authors: David J. Stevenson, Peter Bodenheimer, Jack J. Lissauer, Gennaro D'Angelo
Figure caption: Planet’s structure and composition at t = 2.43 × 105 yr, right after the beginning of Phase II. The left panel shows density, pressure, mass fraction of heavy elements, and temperature, as indicated. The “inner core” extends to the left of the curves, as marked. The “core” is the innermost region defined by ﹩\mathrm{log}Z\gt -0.01﹩. The right panel shows the distributions of silicate, water, and H–He mass fractions.
Paper: Winter Weakening of Titan's Stratospheric Polar Vortices
Authors: J. Shultis, D. W. Waugh, A. D. Toigo, C. E. Newman, N. A. Teanby, J. Sharkey
Figure caption: Evolution of zonal-averaged PV (107 m2 s−1K kg−1) in black, static stability –g                   ﹩\tfrac{\partial \theta }{\partial p}﹩ (K m2/kg) in red, and absolute vorticity ζ  A  (s−1) in blue, throughout the year averaged over 80°–90°S on a 0.1 hPa surface.
Paper: Mixing of Condensable Constituents with H–He during the Formation and Evolution of Jupiter
Authors: David J. Stevenson, Peter Bodenheimer, Jack J. Lissauer, Gennaro D'Angelo
Figure caption: As in Figures 1 and 2, but the interior structure (left) and composition (right) refer to the current age, t = 4.57 × 109 yr.
Paper: Mixing of Condensable Constituents with H–He during the Formation and Evolution of Jupiter
Authors: David J. Stevenson, Peter Bodenheimer, Jack J. Lissauer, Gennaro D'Angelo
Figure caption: Planet’s structure and composition at the current age for Run LowZ. Compare with the standard model, illustrated in Figure 6 at the same epoch. The left panel shows the interior structure, while the right panel shows the distributions of mass fractions of light and heavy elements.
Paper: Mixing of Condensable Constituents with H–He during the Formation and Evolution of Jupiter
Authors: David J. Stevenson, Peter Bodenheimer, Jack J. Lissauer, Gennaro D'Angelo
Figure caption: Integrated mass of heavy elements in the planet interior, at the current age, for the standard model and the Run LowZ, with lower M  Z , and color rendering of ﹩\mathrm{log}Z﹩.
Paper: The Gravitational Imprint of an Interior–Orbital Resonance in Jupiter–Io
Authors: Benjamin Idini, David J. Stevenson
Figure caption: Jupiter interior models with a dilute core defined as a gradient in the enrichment of heavy elements. Shown are (left) a wide dilute core with a smooth compositional gradient similar to that proposed in Debras & Chabrier (2019), (middle) a narrow dilute core with a sharp compositional gradient similar to that proposed in Militzer et al. (2022), and (right) a compact dilute core with a sharp compositional gradient constrained to a central region, similar to a traditional core. The density profile is normalized by a central density ρ  c  equal to 5.8, 4.6, and 23.1 g cm−3, respectively. The enrichment of heavy elements Z corresponds to the mass fraction of elements heavier than H and He. The Brunt–Väisälä (B-V) frequency is normalized by Jupiter’s dynamical frequency ﹩{\omega }_{\mathrm{dyn}}^{2}={ \mathcal G }{M}_{{\rm{J}}}/{R}_{{\rm{J}}}^{3}﹩.
Paper: The Gravitational Imprint of an Interior–Orbital Resonance in Jupiter–Io
Authors: Benjamin Idini, David J. Stevenson
Figure caption: Fractional correction to the hydrostatic Love number k 42 as a function of tidal frequency and dissipation Q 4. The dilute core model (Figure 2(b)) produces a g 1 mode in resonance with the tidal frequency ω ≈ −1.5Ω, a forcing frequency close to Io’s tidal frequency, ω Io ≈ −1.53Ω.
Paper: The Gravitational Imprint of an Interior–Orbital Resonance in Jupiter–Io
Authors: Benjamin Idini, David J. Stevenson
Figure caption: Pictographic orbital migration and dilute core evolution required to explain Juno’s k 42 using a core–orbital resonance. The dilute core forms with a g–mode frequency lower than the satellite tidal frequency. Initially out of resonance, the satellite migrates outward at an almost negligible rate. After some uncertain time, the dilute core evolves into a locked interior–orbital resonance, increasing the rate of satellite orbital migration.
Paper: The Diverse Shapes of Dwarf Planet and Large KBO Phase Curves Observed from New Horizons
Authors: Anne J. Verbiscer, Paul Helfenstein, Simon B. Porter, Susan D. Benecchi, J. J. Kavelaars, Tod R. Lauer, Jinghan Peng, Silvia Protopapa, John R. Spencer, S. Alan Stern, Harold A. Weaver, Marc W. Buie, Bonnie J. Buratti, Catherine B. Olkin, Joel Parker, Kelsi N. Singer, Leslie A. Young
Figure caption: Phase integral q  V  vs. visible geometric albedo p  V  for objects in the solar system that have been observed at phase angles large enough to evaluate their phase integrals. Filled circles are KBOs; open circles are comets; open triangles are satellites; filled triangles are asteroids and Ceres. Objects with hypervolatile surface compositions are shown in red; objects on which water ice has been detected are shown in blue; objects with unknown or nonvolatile surface compositions are shown in black. L and T denote leading and trailing hemispheres, respectively. Filled squares represent the Moon and Mercury. Generally, observations at α > 70° are required to estimate phase integrals (Verbiscer & Veverka 1988). Panel (a) contains all objects; however, to facilitate the identification and location of objects with p  V  < 0.5, panel (b) corresponds to the area within the box defined by the dashed lines in panel (a). Panel (c) corresponds to the area within the box defined by the dashed lines in panel (b) (i.e., those objects with p  V  < 0.15 and q  V  < 0.4). The solid line is the proposed Brucker et al. (2009) linear relationship between q  V  and p  V ; see text for discussion. Data points are shown for Triton (Hillier et al. 1990); Nereid (Thomas et al. 1991); Europa, Ganymede, Callisto (Domingue & Verbiscer 1997); Mimas, Enceladus, Tethys, Dione, Rhea (Verbiscer et al. 2007); Iapetus (Blackburn et al. 2010); Phoebe (Simonelli et al. 1999; Miller et al. 2011); Phobos (Simonelli et al. 1998); Deimos (Thomas et al. 1996); Miranda, Ariel, Umbriel, Titania, Oberon, Puck (Karkoschka 2001); Pluto, Charon (Verbiscer et al. 2019a); Mercury (Warell & Bergfors 2008); the Moon (Helfenstein & Veverka 1987); Ceres (Ciarniello et al. 2017); Vesta (Li et al. 2013); Eros (Li et al. 2004); Ida, Dactyl, Gaspra (Helfenstein et al. 1996); Mathilde (Clark et al. 1999); Lutetia (Masoumzadeh et al. 2015); Steins (Spjuth et al. 2012); Annefrank (Hillier et al. 2011); Itokawa (Tatsumi et al. 2018); Bennu (Takir et al. 2015); Ryugu (Ishiguro et al. 2014); C and S asteroids (Helfenstein & Veverka 1989); Borrelly (R band), Hartley 2, Tempel 1, Wild 2 (Li et al. 2013); 67P (Ciarniello et al. 2015); and Arrokoth (Stern et al. 2019).
Paper: The Diverse Shapes of Dwarf Planet and Large KBO Phase Curves Observed from New Horizons
Authors: Anne J. Verbiscer, Paul Helfenstein, Simon B. Porter, Susan D. Benecchi, J. J. Kavelaars, Tod R. Lauer, Jinghan Peng, Silvia Protopapa, John R. Spencer, S. Alan Stern, Harold A. Weaver, Marc W. Buie, Bonnie J. Buratti, Catherine B. Olkin, Joel Parker, Kelsi N. Singer, Leslie A. Young
Figure caption: Placement of Pluto and Triton parameters from previous work (Table A1) in Figures 9 and 10(a). As in those figures, open circles represent volatile-rich surfaces, diamonds represent nonvolatile surfaces or those otherwise of undetermined volatile content, and filled circles represent H2O-rich surfaces. (a) Plot of h  S  vs. SPPF b shows that there is no unique correlation between the regolith porosity predicted from SHOE and the regolith grain surface roughness, indicated by the SPPF b parameter. From this work, the diagram indicates that the SPPFs of bright, volatile-rich bodies have narrower lobes than those of the darker nonvolatile and H2O-rich bodies. However, for both Pluto and Triton, previous work found SPPFs with broad lobes, in the range of those for darker objects. (b) SHOE amplitude parameter B  oS  vs. the SPPF effective asymmetry parameter g eff for DPs and large KBOs. In most cases, the SHOE is most prominent for regoliths containing nearly opaque grains (B  oS  > 0.8) that project dark shadows. Forward-scattering grains diminish projected shadows, consistent with our solutions for Triton, Pluto, and Quaoar. Previous solutions for Pluto and Triton have the low-amplitude SHOE of bright icy particles, but they imply more strongly backscattering regolith grains. (c) Relationship between the SPPF effective asymmetry parameter g eff vs. ﹩{\tilde{\omega }}_{o}﹩ suggests a trend from dominantly backscattering low-albedo particles to dominantly forward-scattering high-albedo grains. Solutions for volatile-rich surfaces from this work consistently have grains that are highest in both single-scattering albedo and forward scattering. Nonvolatile surface particles have low single-scattering albedos and range from moderately backscattering to nearly isotropic, with symmetric forward- and backscattering lobes. The directional scattering behavior of H2O-rich surfaces tends to lie in between that of the hypervolatile and nonvolatile surfaces. Previous results deviate from this trend—although they have high albedos, they have asymmetry factors that are most similar to those of the darkest surfaces with the most opaque grains.
Paper: The Diverse Shapes of Dwarf Planet and Large KBO Phase Curves Observed from New Horizons
Authors: Anne J. Verbiscer, Paul Helfenstein, Simon B. Porter, Susan D. Benecchi, J. J. Kavelaars, Tod R. Lauer, Jinghan Peng, Silvia Protopapa, John R. Spencer, S. Alan Stern, Harold A. Weaver, Marc W. Buie, Bonnie J. Buratti, Catherine B. Olkin, Joel Parker, Kelsi N. Singer, Leslie A. Young
Figure caption: Relationships among texture-dependent parameters of the Hapke model (﹩\bar{\theta }﹩, h  S , and SPPF b). Open circles represent hypervolatile-rich surfaces, diamonds represent nonvolatile surfaces or those otherwise of undetermined volatile content, and filled circles represent H2O-rich surfaces. (a) Plot of h  S  vs. SPPF b shows that there is no unique correlation between the regolith porosity predicted from SHOE and the regolith grain surface roughness, indicated by the b parameter of the average SPPF. (b) Nominal corrected “actual” mean roughness slope angle values of ﹩\bar{\theta }﹩ are plotted from Table 17 against the SPPF b parameter. Objects with roughness angles greater than 45° have been excluded. Vertical error bars have been omitted owing to the degeneracy of the albedo and scattering asymmetry correction at the estimated uncertainty limits in the uncorrected values of ﹩{\bar{\theta }}_{p}﹩ or otherwise on bodies for which ﹩{\bar{\theta }}_{p}﹩ was fixed at a constant value during fits of the Hapke model to the phase curves. The dashed line represents an (unweighted) fit to the nominal data points, ﹩\bar{\theta }=-33.06b+33.63﹩, and suggests that macroscopically smoother surfaces correlate with regolith grains that have smoother, more regular shapes.
Paper: The Diverse Shapes of Dwarf Planet and Large KBO Phase Curves Observed from New Horizons
Authors: Anne J. Verbiscer, Paul Helfenstein, Simon B. Porter, Susan D. Benecchi, J. J. Kavelaars, Tod R. Lauer, Jinghan Peng, Silvia Protopapa, John R. Spencer, S. Alan Stern, Harold A. Weaver, Marc W. Buie, Bonnie J. Buratti, Catherine B. Olkin, Joel Parker, Kelsi N. Singer, Leslie A. Young
Figure caption: Comparison of retrieved global-average SPPFs for Pluto (top row) and Triton (bottom row) from this study and previous work listed in Table A1. Plots on the left show ﹩{\tilde{\omega }}_{o}P(\alpha )﹩ vs. α curves predicted by the best-fit Hapke model fits from this study and from previous work. Data points are the whole-disk phase curve observations that have been inverted to corresponding values of ﹩{\tilde{\omega }}_{o}P(\alpha )﹩ using the method of Helfenstein & Shepard (2011). The solid black ﹩{\tilde{\omega }}_{o}P(\alpha )﹩ curves are the haze models from previous work. Plots on the right are McGuire & Hapke (1995) hockey stick plots (with thick and thin solid curves as described in the caption to Figure 8) that compare the SPPF b and c values from this study to the corresponding values from Table A1 in the context of corresponding regolith grain properties. Note that the error bars for the Hillier et al. (2021) Pluto data are smaller than the data point symbols. The cyan squares are the results of stepwise grid searches of parameter space around the best-fit solution in this work; they are the b and c values from all valid model solutions found within the nominal error envelope of the Hapke model solutions presented herein. See text for discussion.
Paper: Spatial Distribution and Thermal Diversity of Surface Volatile Cold Traps at the Lunar Poles
Authors: Margaret E. Landis, Paul O. Hayne, Jean-Pierre Williams, Benjamin T. Greenhagen, David A. Paige
Figure caption: Maximum bolometric temperatures for the north (left) and south (right) poles derived in this study and used to determine surface thermal stability regions for volatiles, displayed in polar azimuthal equidistant projection. Each latitude ring is 5°.
Paper: Orbits and Occultation Opportunities of 15 TNOs Observed by New Horizons
Authors: Simon B. Porter, John R. Spencer, Anne Verbiscer, Susan Benecchi, H. A. Weaver, Hsing Wen Lin, J. J. Kavelaars, Wesley C. Fraser, David W. Gerdes, Marc W. Buie, Kelsi N. Singer, Joel W. Parker, S. Alan Stern
Figure caption: Best US domestic occultation opportunities for 2021–2022. The red region represents the nominal shadow path based on the size of the object, and the yellow region adds 1σ uncertainty. Note that the 1σ uncertainty for 2004 LW31 goes off of the disk of the Earth.
Paper: Orbits and Occultation Opportunities of 15 TNOs Observed by New Horizons
Authors: Simon B. Porter, John R. Spencer, Anne Verbiscer, Susan Benecchi, H. A. Weaver, Hsing Wen Lin, J. J. Kavelaars, Wesley C. Fraser, David W. Gerdes, Marc W. Buie, Kelsi N. Singer, Joel W. Parker, S. Alan Stern
Figure caption: Best US domestic occultation opportunities for 2023–2029. The red region represents the nominal shadow path based on the size of the object, and the yellow region adds 1σ uncertainty.
Paper: Orbits and Occultation Opportunities of 15 TNOs Observed by New Horizons
Authors: Simon B. Porter, John R. Spencer, Anne Verbiscer, Susan Benecchi, H. A. Weaver, Hsing Wen Lin, J. J. Kavelaars, Wesley C. Fraser, David W. Gerdes, Marc W. Buie, Kelsi N. Singer, Joel W. Parker, S. Alan Stern
Figure caption: Best international occultation opportunities for 2011 HF103, 2011 HJ103, 2011 HK103, and 2011 HZ102. The red region represents the nominal shadow path based on the size of the object, and the yellow region adds 1σ uncertainty.
Paper: An Open-source Bayesian Atmospheric Radiative Transfer (BART) Code. II. The TRANSIT Radiative Transfer Module and Retrieval of HAT-P-11b
Authors: Patricio E. Cubillos, Joseph Harrington, Jasmina Blecic, Michael D. Himes, Patricio M. Rojo, Thomas J. Loredo, Nate B. Lust, Ryan C. Challener, Austin J. Foster, Madison M. Stemm, Andrew S. D. Foster, Sarah D. Blumenthal
Figure caption: Top: HAT-P-11b transmission spectra. The black points with error bars denote the HST and Spitzer IRAC data and their 1σ uncertainties reported by Chachan et al. (2019). The gray points with error bars denote the data reported by Fraine et al. (2014). The pink and blue curves show the BART best-fitting spectrum to the Chachan et al. (2019) data sets (with and without considering the Spitzer observations, respectively). The gray curves at the bottom show the Spitzer transmission filters. Bottom: pairwise and marginal posterior probability distribution to the Chachan et al. (2019) data set (the pink shaded areas show the retrieval posteriors of the HST and Spitzer data, whereas the blue contours show that of the HST data alone). The red and blue solid vertical lines denote the posterior’s median for the retrieval with and without considering the Spitzer observations, respectively. We omitted plotting the credible interval boundaries to avoid cluttering (their values are available in Table 2).
Paper: An Open-source Bayesian Atmospheric Radiative Transfer (BART) Code. II. The TRANSIT Radiative Transfer Module and Retrieval of HAT-P-11b
Authors: Patricio E. Cubillos, Joseph Harrington, Jasmina Blecic, Michael D. Himes, Patricio M. Rojo, Thomas J. Loredo, Nate B. Lust, Ryan C. Challener, Austin J. Foster, Madison M. Stemm, Andrew S. D. Foster, Sarah D. Blumenthal
Figure caption: Top: HAT-P-11b transmission spectra. The black points with error bars denote the HST WFC3/G141 and Spitzer IRAC data and their 1σ uncertainties reported by Fraine et al. (2014). The gray points with error bars denote the data reported by Chachan et al. (2019). The green curve shows the BART best-fitting spectrum to the Fraine et al. (2014) data set. The HST points were adjusted downward according to the retrieved offset. The gray curves at the bottom show the Spitzer transmission filters. Bottom: pairwise and marginal posterior probability distribution to the Fraine et al. (2014) data set. The solid and dashed vertical lines denote the posterior’s median and boundaries of the 68% credible interval, respectively (Table 2).
Paper: An Open-source Bayesian Atmospheric Radiative Transfer (BART) Code. II. The TRANSIT Radiative Transfer Module and Retrieval of HAT-P-11b
Authors: Patricio E. Cubillos, Joseph Harrington, Jasmina Blecic, Michael D. Himes, Patricio M. Rojo, Thomas J. Loredo, Nate B. Lust, Ryan C. Challener, Austin J. Foster, Madison M. Stemm, Andrew S. D. Foster, Sarah D. Blumenthal
Figure caption: Normalized, systematics-corrected Spitzer HAT-P-11b transit light curves (black points) with the best-fitting models (colored solid curves). The error bars denote the 1σ uncertainties. For clarity, we binned the data points and vertically shifted the curves.
Paper: An Open-source Bayesian Atmospheric Radiative Transfer (BART) Code. II. The TRANSIT Radiative Transfer Module and Retrieval of HAT-P-11b
Authors: Patricio E. Cubillos, Joseph Harrington, Jasmina Blecic, Michael D. Himes, Patricio M. Rojo, Thomas J. Loredo, Nate B. Lust, Ryan C. Challener, Austin J. Foster, Madison M. Stemm, Andrew S. D. Foster, Sarah D. Blumenthal
Figure caption: Fit residuals’ rms (black curve with 1σ uncertainties) vs. bin size for the second visit at 3.6 μm. The red curve shows the expected rms for Gaussian (uncorrelated) noise. The green dashed vertical line marks the transit duration time.
Paper: An Open-source Bayesian Atmospheric Radiative Transfer (BART) Code. II. The TRANSIT Radiative Transfer Module and Retrieval of HAT-P-11b
Authors: Patricio E. Cubillos, Joseph Harrington, Jasmina Blecic, Michael D. Himes, Patricio M. Rojo, Thomas J. Loredo, Nate B. Lust, Ryan C. Challener, Austin J. Foster, Madison M. Stemm, Andrew S. D. Foster, Sarah D. Blumenthal
Figure caption: Near-infrared titanium- and vanadium-oxide opacity spectra. TRANSIT calculated the opacities at a temperature of 2200 K and a pressure of 10.13 bars (10 atm). Our models are consistent with Figures 4 and 5 of Sharp & Burrows (2007).
Paper: The Gravitational Imprint of an Interior–Orbital Resonance in Jupiter–Io
Authors: Benjamin Idini, David J. Stevenson
Figure caption: The ﹩{}_{4}^{2}{g}_{1}﹩ mode frequency of several dilute core models. The vertical lines represent the tidal frequency ∣ω∣ of Io, Europa, Ganymede, and Callisto (left to right).
Paper: The Gravitational Imprint of an Interior–Orbital Resonance in Jupiter–Io
Authors: Benjamin Idini, David J. Stevenson
Figure caption: Same as Figure 4 but for the ﹩{}_{2}^{2}{g}_{1}﹩ mode frequency. The open rectangles show the higher-frequency ﹩{}_{4}^{2}{g}_{1}﹩ mode of the same dilute core models.
Paper: Dynamical Regimes of Polar Vortices on Terrestrial Planets with a Seasonal Cycle
Authors: Ilai Guendelman, Darryn W. Waugh, Yohai Kaspi
Figure caption: Top row: seasonal variations of the zonal mean zonal wind (at a height of σ = 0.5) around southern hemisphere winter for ω = 4, γ = 30°, and Ω = 0.5. As in Figure 2, the x-axis represents the fraction of the year. The fractions confined between the colored vertical lines represent the time average period for the respective columns below it: black (left column) for early winter (late fall), blue for midwinter, and red for late winter (early spring). Second row: vertical structure of the zonal mean zonal wind (ms−1). Third row: vertical structure of the mass streamfunction (1012 kg s−1). Fourth row: vertical structure of the temperature (K). Fifth row: vertical structure of the eddy momentum flux convergence (ms−2).
Paper: Dynamical Regimes of Polar Vortices on Terrestrial Planets with a Seasonal Cycle
Authors: Ilai Guendelman, Darryn W. Waugh, Yohai Kaspi
Figure caption: Absolute value PV (solid) and zonal mean zonal wind (dashed) meridional structure in the winter hemisphere for different parameter values for a temporal mean of days 180–240 and σ = 0.5. Each line is normalized by its maximum value. (a) Black is for Ω = 1, blue is for Ω = 1/4, and red is for Ω = 1/16; other parameters are constant, with ω = 1 and γ = 30°. (b) Black is for γ = 20°, blue is for γ = 50°, and red is for γ = 80°; other parameters are constant, with ω = 1 and Ω = 1. (c) Black is for ω = 1, blue is for ω = 4, and red is for ω = 1/4; other parameters are constant, with Ω = 1 and γ = 30°.