adsabs/AstroCLIMB huggingface dataset:
Paper: Isolating the Gravitational Influence of Uranus’s Winds Requires Close Passages Inward of the Rings
Authors: Christopher R. Mankovich, Marzia Parisi, Damon F. Landau, Janosz W. Dewberry
Figure caption: Contributions to the odd gravity moments in the interior model from Figure 3. Each row assumes a different tropospheric wind profile. The first row assumes the profile Asym. 5, showing meridional slices of the odd part of the asymmetric wind profile (panel (a)) and the induced perturbation to mass density (panel (b)). Panels (c)–(f) show the integrands in Equation (A1) for J3, J5, J7, and J9, respectively, including the factor of ﹩{r}^{2}\sin \theta ﹩ from the spherical volume element, as well as an overall minus sign so positive values in the color map contribute to Jn in the positive sense. Panels (g)–(l) assume the profile Asym. 6, and panels (m)–(r) assume the Composite profile. Faint spokes mark 15∘ increments. All density perturbations (blue–yellow–red color maps) are in units of 10−5 g cm−3, and r is in units of 25,559 km.
Paper: NEOWISE Data and Thermophysical Modeling of 98943 Torifune (2001 CC21)
Authors: Edward L. (Ned) Wright, Joseph Masiero, Amy Mainzer
Figure caption: Correlation between the parameters of the ellipsoidal TPM model fit to the NEOWISE data. The maps and scatter diagrams show a random sample of 1000 models selected from the MCMC, while the histograms show the entire chain. The range for the scatter diagrams and histograms cover a “±2σ” range for each parameter that is actually given by (p16 + p84)/2 ± (p84 − p16), where p16 and p84 are the 16th and 84th percentile values of the parameter p. These ranges are shown in the upper right corner. However, the range is [0. . 1] for fc, (b/a)3, or (c/b)4. The maps show the rotation poles of the models in celestial coordinates. The points on the maps are colored to show how a given parameter correlates with the pole position, so a red dot on the map shows a model with a low value of the parameter.
Paper: NEOWISE Data and Thermophysical Modeling of 98943 Torifune (2001 CC21)
Authors: Edward L. (Ned) Wright, Joseph Masiero, Amy Mainzer
Figure caption: Spectral energy distributions for the Spitzer observation and the many epochs of NEOWISE observations predicted by the maximum posterior model found during the MCMC. The thermal inertia for this model is Γ1 = 2111 mks units. The rotation pole is at (α, δ) = (281°, 45°). The diameter of a sphere with the same volume is D = 2(abc)1/3 = 474 m.
Paper: NEOWISE Data and Thermophysical Modeling of 98943 Torifune (2001 CC21)
Authors: Edward L. (Ned) Wright, Joseph Masiero, Amy Mainzer
Figure caption: Orbit of 2001 CC21 relative to the Earth (blue dot) in a frame rotating to keep the Sun on the −y axis. The orange circle at y = −1 au indicates the Sun’s direction. The plot covers the period from MJD 57754 (2017 January 1) in the lower left to 60484 (2024 June 23). Lines indicating the current scan paths of the NEOWISE mission are shown. Tiny labels give the MJD for each observing epoch.
Paper: NEOWISE Data and Thermophysical Modeling of 98943 Torifune (2001 CC21)
Authors: Edward L. (Ned) Wright, Joseph Masiero, Amy Mainzer
Figure caption: Histogram of the cosine of the obliquity. The prior would be uniform in these coordinates. The black histogram shows the posterior distribution using the NEOWISE data alone. The gray histogram shows the posterior when using both the NEOWISE and the Spitzer data.
Paper: NEOWISE Data and Thermophysical Modeling of 98943 Torifune (2001 CC21)
Authors: Edward L. (Ned) Wright, Joseph Masiero, Amy Mainzer
Figure caption: Correlation between the parameters of the ellipsoidal TPM model fit to both the NEOWISE and Spitzer data. See Figure 2 for an explanation of the plot. The obliquity distribution has a median of 160° with a 16th–84th percentile range of 38°–168° The thermal inertia is much higher than the prior, with ﹩{\rm{\Gamma }}=292{4}_{-105 \% }^{+39 \% }﹩ mks.
Paper: NEOWISE Data and Thermophysical Modeling of 98943 Torifune (2001 CC21)
Authors: Edward L. (Ned) Wright, Joseph Masiero, Amy Mainzer
Figure caption: The spectra of the ellipsoidal model with the highest posterior likelihood compared to the NEOWISE data.
Paper: Simultaneous Detection of the Size and Velocity of the Largest Ejecta Particles with Velocities Exceeding 1 km s−1
Authors: Akiko M. Nakamura, Keita Nomura, Sunao Hasegawa
Figure caption: Relationship between ejecta size, velocity, and ejection angle. (a) Relationships between ejecta size and ejection velocity: ﹩\left({V}_{{\rm{ej}},\,{\rm{\max }}}+{V}_{{\rm{ej}},\,{\rm{\min }}}\right)/2﹩. The error bars correspond to ﹩\left({V}_{{\rm{ej}},\,{\rm{\max }}}-{V}_{{\rm{ej}},\,{\rm{\min }}}\right)/2.﹩ The ejecta size is represented on the horizontal axis in terms of the equivalent sphere diameter. The error bars include a 10% measurement uncertainty in crater size, together with the estimated errors in velocity and the uncertainty of the scaling law. (b) ﹩{V}_{{\rm{ej}},\,{\rm{\min }}}﹩ versus ejecta size derived from Equation (6), where ﹩{V}_{{\rm{ej}}}={V}_{{\rm{ej}},\,{\rm{\min }}}﹩. The dashed and dotted curves are the extrapolations of an analytical model (Equation (9)) assuming that the tensile strengths are 10- and 100-fold the static tensile strength, respectively. (c) Relationship between ejection angle and velocity (﹩{V}_{{\rm{ej}},\,{\rm{\min }}}﹩). The dashed curve and square marks are from a previous study (D. E. Gault et al. 1963). (d) Relationship between ejecta size and velocity (﹩{V}_{{\rm{ej}},\,{\rm{\min }}}﹩). Previous results of impacts with oblique incidences of 30°, 45°, and 60° of basalt targets are shown by squares containing a plus sign, diagonal line, and a cross, respectively (A. Nakamura & A. Fujiwara 1991; A. Nakamura 1993).
Paper: Evaluating Lunar Crater Ejecta Maturation across Wavelengths
Authors: Angela M. Stickle, Anna C. Martin, Robyn M. Meier, Tyler M. Powell
Figure caption: Comparisons of average data values at the crater rim (circles) and one, two, and four crater radii from the crater rim (squares, diamonds, and triangles) for the three initial craters examined in this study. Table A1 includes the values for each dataset from 1-5 Rc. In general, the values at the crater rim follow expected trends, while farther out from the crater, more complexity is seen. (A) Diviner RA as a function of Clementine OMAT; higher OMAT values suggest younger craters. (B) Diviner RA as a function of Mini-RF CPR; younger craters tend to have blockier, rockier ejecta near the crater rim, which manifests as higher RA and CPR values. (C) CPR as a function of OMAT. (D)–(F) WAC color bands as a function of Diviner RA. (G)–(I) m − χ bands 1–3 as a function of OMAT. (J)–(L) WAC color bands as a function of OMAT.
Paper: Evaluating Lunar Crater Ejecta Maturation across Wavelengths
Authors: Angela M. Stickle, Anna C. Martin, Robyn M. Meier, Tyler M. Powell
Figure caption: Comparisons of average data values at the crater rim (blue triangles) and one and two crater radii from the crater rim (orange squares and yellow circles, respectively) for our expanded catalog of craters. All the datasets are plotted vs. OMAT. (A) Diviner RA vs. OMAT, (B) Diviner NST vs. OMAT, (C) Mini-RF CPR vs. OMAT, (D)–(F) Mini-RF m − χ bands vs. OMAT, (G)–(I) WAC UV RGB bands vs. OMAT. In general, expected behaviors from Figure 5 are seen for the expanded number of craters.
Paper: Evaluating Lunar Crater Ejecta Maturation across Wavelengths
Authors: Angela M. Stickle, Anna C. Martin, Robyn M. Meier, Tyler M. Powell
Figure caption: Examples of average radial profiles from a subset of the datasets. The three initial craters of study are represented by different colors: Byrgius A (yellow), Dufay B (green), and Golitsyn J (blue). The radial distances are normalized to crater radius (Rc). (A) Radial OMAT profiles from Clementine (dashed) and Kaguya (solid line) data, starting from the crater rim. Higher OMAT indicates less mature material and a younger age. (B) 415 nm WAC UV profiles, starting at the crater rim. (C) CF profiles showing the center wavelength of the CF as a function of distance from the crater rim. (D)–(F) Mini-RF m − χ profiles, normalized to mean lunar background values (i.e., where the curve flattens). (G)–(I) Nonnormalized m − χ profiles for Byrgius A (G), Dufay B (H), and Golitsyn J (I), showing profiles of each of the three scattering components.
Paper: Evaluating Lunar Crater Ejecta Maturation across Wavelengths
Authors: Angela M. Stickle, Anna C. Martin, Robyn M. Meier, Tyler M. Powell
Figure caption: Example of profile generation output for Byrgius A in the OMAT (Kaguya) dataset. (A) OMAT image and average (B) radial and (C) azimuthal profiles. The annuli in (A) and vertical dashed lines in (B) indicate one to five crater radii from the crater center.
Paper: NEOWISE Data and Thermophysical Modeling of 98943 Torifune (2001 CC21)
Authors: Edward L. (Ned) Wright, Joseph Masiero, Amy Mainzer
Figure caption: The posterior distribution of the equivalent volume sphere diameter from the ellipsoidal model applied to the NEOWISE data (black), with the 16th–84th percentile range indicated by a black horizontal error bar, the value derived from the polarimetric albedo (J. Geem et al. 2023) indicated by the blue error bar, the shape model of M. M. Popescu et al. (2025) scaled using the K. Arimatsu et al. (2024) occulation data shown as an orange error bar, and the S. Fornasier et al. (2024) NEATM result indicated by the red error bar. The magenta error bar shows the result of the TPM applied to the Fornasier et al. data. The gray histogram and error bar show the TPM applied to the Fornasier et al. data combined with the NEOWISE data. The M. Hirabayashi et al. (2021) value of 700 m would be at the right edge of the graph.
Paper: Snowball Bistability Vanishes at Moderate Orbital Eccentricity
Authors: Xuan Ji, 璇 纪, Dorian S. Abbot
Figure caption: Eccentricity versus annual-mean stellar flux for rocky exoplanets. Dots represent measured eccentricities, with vertical lines showing observational uncertainties; triangles denote planets for which only upper-limit constraints on eccentricity are available. Red symbols highlight planets whose upper eccentricity limits exceed 0.25, while black symbols represent the rest. The annual-mean stellar flux is computed using the mean eccentricity via ﹩S\propto {({a}^{2}\sqrt{1-{e}^{2}})}^{-1}﹩. Only potential rocky exoplanets with constrained eccentricity measurements are included in the sample. Seventy-two out of 216 rocky planets have eccentricity upper limits exceeding 0.25. The sample is drawn from the confirmed exoplanet catalog on the NASA Exoplanet Archive (NASA Exoplanet Archive 2019): for transiting planets, the criteria for selecting “rocky planets” follow X. Ji et al. (2025; filled symbols); for planets without radius measurements, those with planetary masses less than 6 Earth masses are shown (open symbols).
Paper: Snowball Bistability Vanishes at Moderate Orbital Eccentricity
Authors: Xuan Ji, 璇 纪, Dorian S. Abbot
Figure caption: Comparison between equatorial-ice thermodynamics model (top: panels (a)–(c) and GCM output at the equator (bottom: panels (d)–(f)) near the limiting case where the Snowball state ceases to exist (S/S0 = 0.87, e = 0.2), demonstrating qualitatively similar behavior. The panels show F(t) (Equation (3)) (a), (d), the ice thickness (b), (e), and the surface temperature (c), (f). F(t) > 0 between times t1 and t2, leading to melting. We define the integral of F(t) over this period as E1, an important quantity discussed in the text. Similarly, freezing occurs when F(t) < 0, and we define the integral of F(t) over this period as E2. The red and blue curves in panel (f) show the daily maximum and minimum temperature, while the thick purple line is the diurnal mean.
Paper: Snowball Bistability Vanishes at Moderate Orbital Eccentricity
Authors: Xuan Ji, 璇 纪, Dorian S. Abbot
Figure caption: Maximum stellar flux allowing a Snowball state as a function of eccentricity. Red dots represent default GCM results, corresponding to the right boundary of the bistability region in Figure 2. The error bars indicate the range in annual-mean stellar flux spanned by the two simulations closest to this boundary. We also plot GCM sensitivity tests with the ice albedo increased by a factor of 1.04 (blue dots) and the obliquity increased to 23° (purple dots). The red line shows results from the ice-thermodynamic model with αi and Qadv tuned to default GCM results at low eccentricity. The blue and purple lines show results of the ice-thermodynamic model with parameters adjusted for the GCM sensitivity tests. The horizontal gray line shows the approximate critical stellar flux for the transition from Waterbelt to Snowball in the GCM, corresponding to the left boundary of the bistability region.
Paper: Snowball Bistability Vanishes at Moderate Orbital Eccentricity
Authors: Xuan Ji, 璇 纪, Dorian S. Abbot
Figure caption: Snowball bifurcation diagrams for different eccentricities with the GCM ExoCAM. Blue circles represent simulations initialized with global ice coverage, and red circles represent simulations initialized with no ice coverage. Seasonal variations in monthly mean values are shown by vertical bars but are smaller than the circles in many cases. The gray shaded region indicates the range of stellar flux where Snowball bistability exists. The panels on the left (a)–(f) show the global-mean ice fraction (Fice) as a function of annual-mean stellar flux. The panels on the right (g)–(l) show the global-mean surface temperature as a function of annual-mean stellar flux.
Paper: Snowball Bistability Vanishes at Moderate Orbital Eccentricity
Authors: Xuan Ji, 璇 纪, Dorian S. Abbot
Figure caption: The maximum eccentricity at which a Snowball bifurcation can exist is shown as a function of the variation in infrared emission to space at the water freezing temperature, ΔA, and top-of-atmosphere (TOA) albedo over ice, αi, in the ice-thermodynamic model.
Paper: Snowball Bistability Vanishes at Moderate Orbital Eccentricity
Authors: Xuan Ji, 璇 纪, Dorian S. Abbot
Figure caption: GCM bifurcation diagram for Earth-like obliquity cases. The format follows Figure 2, where red markers represent Warm Start simulations and blue markers represent Cold Start simulations. Solid lines indicate simulations with Earth-like obliquity (23°), while dotted lines show corresponding zero-obliquity cases for comparison. From top to bottom, eccentricity increases.
Paper: Snowball Bistability Vanishes at Moderate Orbital Eccentricity
Authors: Xuan Ji, 璇 纪, Dorian S. Abbot
Figure caption: Prediction of maximum CO2 forcing allowing a Snowball state as a function of eccentricity using the ice-thermodynamic model. We explore the effect of changing CO2 concentrations by adjusting the parameter A in the linearized OLR parameterization, where lower CO2 levels correspond to larger A values due to weaker greenhouse effects.
Paper: Snowball Bistability Vanishes at Moderate Orbital Eccentricity
Authors: Xuan Ji, 璇 纪, Dorian S. Abbot
Figure caption: GCM bifurcation diagram with e = 0.1, with the ice surface albedo increased by 4%, from 0.67 to 0.7. Thick solid lines indicate simulations with the ice surface albedo adjusted, while dashed lines show the default case.
Paper: Snowball Bistability Vanishes at Moderate Orbital Eccentricity
Authors: Xuan Ji, 璇 纪, Dorian S. Abbot
Figure caption: GCM bifurcation diagram with e = 0.1 for mixed-layer depth (MLD) values of to 1 and 100 m in addition to the default value of 50 m.
Paper: Evidence of Possible Spectral Variability in the Patroclus–Menoetius Binary System
Authors: Ian Wong, William M. Grundy, Joshua P. Emery, Richard P. Binzel, Oriel A. Humes, Simone Marchi, Pippa M. Molyneux, Keith S. Noll
Figure caption: Viewing geometries at the start times of the GMOS observations, centered in the stationary frame of Patroclus. The sky-projected disks of Patroclus and Menoetius are approximated by circles with radii of 49 and 45 km, respectively. The hatched circles indicate the shadow of Patroclus or Menoetius. The direction of Menoetius’s instantaneous relative motion is indicated by the black arrows. The “N” and “E” directions denote increasing decl. and R.A., respectively. The rotational poles of the two tidally locked components point downward in these plots.
Paper: Evidence of Possible Spectral Variability in the Patroclus–Menoetius Binary System
Authors: Ian Wong, William M. Grundy, Joshua P. Emery, Richard P. Binzel, Oriel A. Humes, Simone Marchi, Pippa M. Molyneux, Keith S. Noll
Figure caption: Reflectance spectra of the PM binary from the two visits (blue = 2024 September 2; magenta = 2024 October 4). The best-fit spectral slopes are overplotted in green and yellow, respectively. Both spectra are normalized to unity at 550 nm. The uncertainties are inflated so that the reduced χ2 statistic of the linear fit is 1.
Paper: SpinTrace: A Python Library to Study the Physical Properties of Small Bodies Using Survey-based Photometry
Authors: F. L. Rommel, E. Fernández-Valenzuela, A. C. Souza-Feliciano, B. E. Morgado, B. Proudfoot
Figure caption: Reduced magnitude on the r-SDSS filter as a function of the phase angle before (light green circles) and after (all other colored circles) correcting for rotational modulation for Haumea (upper) and Hektor (bottom). The color gradient depicts the astrometry offsets between the object’s predicted and observed positions (O − C). The red line represents the fitted linear phase function to obtain the absolute magnitude (Hr) and the linear phase coefficient (βr) shown in Table 1.
Paper: SpinTrace: A Python Library to Study the Physical Properties of Small Bodies Using Survey-based Photometry
Authors: F. L. Rommel, E. Fernández-Valenzuela, A. C. Souza-Feliciano, B. E. Morgado, B. Proudfoot
Figure caption: Lomb–Scargle periodogram for Haumea’s combined relative magnitudes in red. Gray lines represent the periodogram obtained from the observational window test. Panel (A) shows the entire frequency range, panels (B) and (C) zoom in on the highest peak region, marked by the blue shaded regions in panels (A) and (B), respectively. The black dotted lines in panel (C) delimit the assumed 3σ uncertainty for the rotational period obtained in this work.
Paper: SpinTrace: A Python Library to Study the Physical Properties of Small Bodies Using Survey-based Photometry
Authors: F. L. Rommel, E. Fernández-Valenzuela, A. C. Souza-Feliciano, B. E. Morgado, B. Proudfoot
Figure caption: Haumea’s RM folded with a rotation period of 3.915342 hr represented as blue dots (JD0 = 2458202.5695942747). The black line represents the rotational light-curve model, and red points are the residuals.
Paper: SpinTrace: A Python Library to Study the Physical Properties of Small Bodies Using Survey-based Photometry
Authors: F. L. Rommel, E. Fernández-Valenzuela, A. C. Souza-Feliciano, B. E. Morgado, B. Proudfoot
Figure caption: Hektor’s RM folded by the best period of 6.92025 hr. The top panel shows the folded data, and the bottom panel shows the residuals. The black line represents the initial light-curve model.
Paper: SpinTrace: A Python Library to Study the Physical Properties of Small Bodies Using Survey-based Photometry
Authors: F. L. Rommel, E. Fernández-Valenzuela, A. C. Souza-Feliciano, B. E. Morgado, B. Proudfoot
Figure caption: Periodogram obtained from the periodic search between 300 and 2400 hr in the Haumea’s data residuals (red). In gray is the periodogram obtained from the observational window test. The dashed dark blue line in panel (A) represents the result from the shuffle test. The blue shaded area is centered on the highest peak. Panel (B) zooms in on the blue shaded area from Panel (A). Vertical dotted lines delimit the uncertainty of the derived period of 588 ± 9 hr (3σ).
Paper: SpinTrace: A Python Library to Study the Physical Properties of Small Bodies Using Survey-based Photometry
Authors: F. L. Rommel, E. Fernández-Valenzuela, A. C. Souza-Feliciano, B. E. Morgado, B. Proudfoot
Figure caption: Lomb–Scargle periodogram obtained from the analysis of Hektor’s data, exploring periodicity values between 4 and 12 hr. The dashed dark blue line in panels (A) and (B) represents the result from the shuffle test. Panel (B) provides a zoom of this region from panel (A), and panel (C) further enlarges the same area from panel (B). The vertical dotted lines in panel (C) correspond to the uncertainty of the derived period, P = 6.92025 ± 0.0008 hr (3σ).
Paper: SpinTrace: A Python Library to Study the Physical Properties of Small Bodies Using Survey-based Photometry
Authors: F. L. Rommel, E. Fernández-Valenzuela, A. C. Souza-Feliciano, B. E. Morgado, B. Proudfoot
Figure caption: Flowchart showing the classes inside the SPINTRACE Python tool, along with a short description of their functionalities.
Paper: Isolating the Gravitational Influence of Uranus’s Winds Requires Close Passages Inward of the Rings
Authors: Christopher R. Mankovich, Marzia Parisi, Damon F. Landau, Janosz W. Dewberry
Figure caption: Gravity moments calculated by applying each of the four wind models displayed in Figure 1 to the same interior model. The same wind radial decay function is enforced in all cases, with winds extending to a depth d = 940 km, close to the median value obtained assuming the Even wind fit. The thick red lines denote the ±3σ detection limits for T1, T2, and T3; dashed purple shows those of T4 and T5 (see Table 2). The gray and black lines at n = 2 and 4 labeled J14 and F24 give the R. A. Jacobson (2014) and R. G. French et al. (2024) 3σ uncertainties on the measured moments J2 and J4.
Paper: Isolating the Gravitational Influence of Uranus’s Winds Requires Close Passages Inward of the Rings
Authors: Christopher R. Mankovich, Marzia Parisi, Damon F. Landau, Janosz W. Dewberry
Figure caption: Different datasets tracking Uranus’s tropospheric features yield a range of permitted zonal wind profiles. Panel (a) gives wind speed as a function of planetographic latitude for the even fit (black) and three asymmetric fits (colors). Panel (b) examines north–south asymmetry, giving the angular velocity difference (degrees west per hour) relative to the even fit for each of the three odd fits. Data and fits are from E. Karkoschka (2015) and L. A. Sromovsky et al. (2015); see Table 1.
Paper: Isolating the Gravitational Influence of Uranus’s Winds Requires Close Passages Inward of the Rings
Authors: Christopher R. Mankovich, Marzia Parisi, Damon F. Landau, Janosz W. Dewberry
Figure caption: The wind-induced even zonal moments J2n as a function of wind depth and bulk rotation. Rotation period is mapped to colors running from 16 hr (dark blue) to 18 hr (bright yellow). Panel (a) shows the posterior histogram of wind depth. Panels (b)–(e) plot the even gravity moments from n = 2 through n = 10. For comparison, gray points show the distribution of full gravity moments (rigid body plus winds). The rigid-body components are negligible for J8 and J10 such that the gray points fall behind the colorful points in panels (d) and (e). The range in panel (b) shows the ±3σ range of the observational J4 constraint.
Paper: Isolating the Gravitational Influence of Uranus’s Winds Requires Close Passages Inward of the Rings
Authors: Christopher R. Mankovich, Marzia Parisi, Damon F. Landau, Janosz W. Dewberry
Figure caption: Close passages of Uranus for each of the five trajectories listed in Table 2. The rings are shown extending from 7000 to 25,590 km altitude above the 1 bar surface, spanning the innermost extent of the ζ ring estimated by I. de Pater et al. (2006; but see discussion in Section 4) through the ϵ ring. The viewing inclination is 10∘ below the ring plane.
Paper: SpinTrace: A Python Library to Study the Physical Properties of Small Bodies Using Survey-based Photometry
Authors: F. L. Rommel, E. Fernández-Valenzuela, A. C. Souza-Feliciano, B. E. Morgado, B. Proudfoot
Figure caption: Per subsample periodogram (top) and folded light curves (bottom) with colors representing individual subsamples. Vertical dashed lines in the upper plot show the 3σ limits of 0.0008 hr obtained for Hektor’s rotational period. The rotational light-curve models and amplitudes are shown in the bottom plot, with amplitude values presented in the legend.