adsabs/AstroCLIMB huggingface dataset:
Paper: A Pre-flyby View on the Origin of Asteroid Donaldjohanson, a Target of the NASA Lucy Mission
Authors: Simone Marchi, David Vokrouhlický, David Nesvorný, William F. Bottke, Josef Ďurech, Harold F. Levison
Figure caption: Best-fit solutions from a set of trial simulations sampling each time only one of the parameters p2 = (ρ, Γ, τ0) in our model: (i) fixed values ρ = 1.3 g cm−3 and τ0 = 1 Myr with five values of Γ listed in labels and color (left panel), (ii) fixed values Γ = 160 SI and τ0 = 1 Myr with five values of ρ listed in labels and color (middle panel), and (iii) fixed values ρ = 1.3 g cm−3 and Γ = 160 SI with five values of τ0 = 1 Myr listed in labels and color (right panel). The black symbols with uncertainty intervals show the data, namely distribution dNsym(C) (Equation (2)), with ∣C∣ ≤ Cfam values binned using ΔC = 1.5 × 10−6 au intervals for H ≤ 17.5 mag Erigone members with WISE dark albedo values. In each case the solution is statistically acceptable, indicating correlations between the parameters. In simulations (i) and (ii), the left and middle panels, the Erigone age T approximately scales with the tested parameter, i.e., T ∝ Γ and T ∝ ρ as expected from analytic formulae for da/dt (e.g., D. Vokrouhlický et al. 2015). In the last simulation (iii), the right panel, T depends on τ0 only weakly, but the χ2 value increases for larger τ0.
Paper: A Pre-flyby View on the Origin of Asteroid Donaldjohanson, a Target of the NASA Lucy Mission
Authors: Simone Marchi, David Vokrouhlický, David Nesvorný, William F. Bottke, Josef Ďurech, Harold F. Levison
Figure caption: Population context of asteroid DJ, a member of the C-type Erigone family (blue). Intriguingly, several other C-type families are also located in this region of the main belt, including New Polana and Eulalia, the likely source of spacecraft-visited asteroids (101955) Bennu and (162173) Ryugu, respectively (see text). These families are highlighted (in violet and yellow, respectively), while the remaining population of asteroids (mostly S-types) is shown using the light-gray symbols. The abscissa is the proper semimajor axis aP, and the ordinate is the proper eccentricity eP (top panel) and proper sine of inclination ﹩\sin {I}_{P}﹩ (bottom panel). Several orbital resonances are indicated (secular resonance ν6, Jupiter interior mean motion resonances J7/2 and J3/1, and Mars exterior mean motion resonances M1/2 and M5/9). Stars indicate the largest member of each family.
Paper: A Pre-flyby View on the Origin of Asteroid Donaldjohanson, a Target of the NASA Lucy Mission
Authors: Simone Marchi, David Vokrouhlický, David Nesvorný, William F. Bottke, Josef Ďurech, Harold F. Levison
Figure caption: Distribution of the geometric albedo values pV for 862 members in the Erigone family delimited by the dashed gray curves in the (aP, H) shown in Figure 2 (the ordinate is a number of asteroids in 0.005 wide albedo bins). The bulk of the family asteroids have dark albedo values with ﹩{p}_{V}\,\leqslant \,{p}_{V}^{\star }=0.125﹩ (red dashed line) confined in a narrow peak about the median ﹩\bar{{p}_{V}}=0.054﹩, followed by a tail subpopulation with pV values terminated by ﹩{p}_{V}^{\star }﹩ (see also J. R. Masiero et al. 2013). No clustering of pV values is seen above ﹩{p}_{V}^{\star }﹩ among a group of 34 bright objects, suggesting that they are interlopers in the family.
Paper: Setting the Stage for Uranian Seismology from Rings and Radial Velocities
Authors: Christopher R. Mankovich, A. James Friedson, Marzia Parisi, Stephen Markham, Janosz W. Dewberry, James Fuller, Matthew M. Hedman, Alex Akins, Mark D. Hofstadter
Figure caption: As in Figure 1, but emphasizing the range of models permitted by J2, J4, and ρ1. These representative models are used for detailed mode calculations. Top: interface models. Bottom: gradient models. Brunt–Väisälä frequency (dotted–dashed, read on the right axis) is plotted as a fraction of Uranus’s dynamical frequency (Equation (5)). Arrows mark the transition to the atmospheric polytrope.
Paper: Setting the Stage for Uranian Seismology from Rings and Radial Velocities
Authors: Christopher R. Mankovich, A. James Friedson, Marzia Parisi, Stephen Markham, Janosz W. Dewberry, James Fuller, Matthew M. Hedman, Alex Akins, Mark D. Hofstadter
Figure caption: Examples of the two types of interior structures considered in this study, one (top) fully adiabatic with a discontinuous core density enhancement and the other (bottom) with a gradual core density enhancement and superadiabaticity in the gradient region. Both models have moderate central density (9.3 and 7.9 g cm−3, respectively) among their parent samples. The insets in each panel emphasize the density and sound speed structure near the break between envelope and atmosphere polytropes.
Paper: Setting the Stage for Uranian Seismology from Rings and Radial Velocities
Authors: Christopher R. Mankovich, A. James Friedson, Marzia Parisi, Stephen Markham, Janosz W. Dewberry, James Fuller, Matthew M. Hedman, Alex Akins, Mark D. Hofstadter
Figure caption: Frequencies and eigenfunctions of the gravitational potential perturbation ﹩{\Phi }^{{\prime} }﹩ for interface and f-modes with similar frequencies, in a grid of models varying the core boundary between 0.5 (dark brown) and 0.7 RU (dark green). (a), (c) ℓ = m = 7 modes with strong eigenfunction overlap giving rise to mixed interface/f-mode character and an avoided frequency crossing. The higher-frequency mode (upper ﹩{\Phi }^{{\prime} }﹩ eigenfunction, offset vertically by +0.4) transitions from interface-dominated to f-dominated as the core boundary is increased. (b), (d) ℓ = m = 15 modes with little to no eigenfunction overlap; in this case, the interface modes (upper eigenfunctions) remain essentially decoupled from the f-modes (lower) and are unlikely to be observed. Arrows highlight the model yielding the smallest frequency separation, inducing weak mode mixing. The frequency axes (a, b) show the centroid (m = 0) mode frequencies as a function of core radius. Cross symbols represent the analytic approximation to the frequency of the interface mode (Equation (9)) and the dashed horizontal line gives the approximate frequency of the f-mode (Equation (8)).
Paper: Setting the Stage for Uranian Seismology from Rings and Radial Velocities
Authors: Christopher R. Mankovich, A. James Friedson, Marzia Parisi, Stephen Markham, Janosz W. Dewberry, James Fuller, Matthew M. Hedman, Alex Akins, Mark D. Hofstadter
Figure caption: OLR locations amid the rings for the best models obtained directly fitting either the ﹩{}_{2}^{2}﹩f-mode (in the rigid core model, open diamonds) or the ﹩{}_{2}^{2}﹩g1 mode (in the gradient model, filled circles) to an m = 2 OLR near the 6 ring. Modes with ℓ = m (black) are shown, as are modes with ℓ − m = 2 (blue), 4 (orange), 6 (green), and 8 (red). This latitudinal wavenumber ℓ − m generally increases toward the top left of the diagram. The dashed boxes highlight additional associations that would discriminate between the two models shown here (see text).
Paper: Setting the Stage for Uranian Seismology from Rings and Radial Velocities
Authors: Christopher R. Mankovich, A. James Friedson, Marzia Parisi, Stephen Markham, Janosz W. Dewberry, James Fuller, Matthew M. Hedman, Alex Akins, Mark D. Hofstadter
Figure caption: As in Figure 5, but for gradient models. Circles denote the f-modes. The modes concentrated at low m and orbital distances ≳42 × 103 km are n = 1 g-modes (triangles). Higher radial order (n > 1) g-modes are expected to produce weaker potentials; these and any g1 modes with ﹩\left|{\Phi }^{{\prime} }(r=R)\right|\lt 1{0}^{-5}\,GM/R﹩ are omitted here.
Paper: Setting the Stage for Uranian Seismology from Rings and Radial Velocities
Authors: Christopher R. Mankovich, A. James Friedson, Marzia Parisi, Stephen Markham, Janosz W. Dewberry, James Fuller, Matthew M. Hedman, Alex Akins, Mark D. Hofstadter
Figure caption: Core radius vs. bulk rotation period in a sample fitting a high-degree mode (﹩{}_{9}^{9}﹩f) to the 6 ring (purple color map), compared to that fitting a low-degree mode (﹩{}_{2}^{2}﹩f) to the same ring (green color map; this is the same sample as the rigid core sample seen in Figures 7 and 8). The low-degree constraint would constrain Uranus’s core radius but not its rotation. The high-degree f-mode is more superficial and would be insensitive to core properties but would constrain Uranus’s rotation period.
Paper: Setting the Stage for Uranian Seismology from Rings and Radial Velocities
Authors: Christopher R. Mankovich, A. James Friedson, Marzia Parisi, Stephen Markham, Janosz W. Dewberry, James Fuller, Matthew M. Hedman, Alex Akins, Mark D. Hofstadter
Figure caption: OLR locations amid Uranus’s rings for ℓ = m modes in a series of interface-based models compatible with all available data. Colors map to the interior model as in Figure 2; see legend. F-modes with larger gravitational potentials at the planetary surface are rendered as larger points. Open symbols show f-mode OLRs for models with a perfectly rigid core. Larger rigid cores push the low-degree f-modes to lower frequencies and hence their OLRs to greater orbital distances. Crosses denote the interface modes, shown with uniform point size for clarity. The interface modes (crosses) in the model with the largest core (min ρc; blue points) are too low a frequency to resonate in the rings. In the model with the most compact core (max ρc; green points), the rigid and fluid core cases have indistinguishable spectra. Note that the ﹩{}_{2}^{2}﹩f-mode in the min ρc fluid core model (blue) nearly coincides with that in the max ρc model (green).
Paper: Setting the Stage for Uranian Seismology from Rings and Radial Velocities
Authors: Christopher R. Mankovich, A. James Friedson, Marzia Parisi, Stephen Markham, Janosz W. Dewberry, James Fuller, Matthew M. Hedman, Alex Akins, Mark D. Hofstadter
Figure caption: An ℓ = 2 propagation diagram for the gradient model with maximum gradient width. P-modes are oscillatory where their frequencies are greater than the Lamb frequency (thick dashed curve; see Equation (10)). G-modes are oscillatory where their frequencies are less than the Brunt–Väisälä frequency (thick solid curve; see Equation (1)). Horizontal lines are calculated m = 0 mode frequencies for the model. Dotted regions are evanescent zones where mode amplitudes decay with distance from their wave propagation region but are still generally nonzero. Integer labels give the p- or g-mode radial order. The gray shaded region at a low frequency indicates the inertial frequency range ω < 2ΩU in which the Coriolis force becomes an important restoring force and our approximations regarding rotation (Section 2.2) are no longer valid.
Paper: Setting the Stage for Uranian Seismology from Rings and Radial Velocities
Authors: Christopher R. Mankovich, A. James Friedson, Marzia Parisi, Stephen Markham, Janosz W. Dewberry, James Fuller, Matthew M. Hedman, Alex Akins, Mark D. Hofstadter
Figure caption: Low-degree zonal gravity moments for gradient-type models of Uranus. (Interface models yield a similar diagram.) The gray points show the part of the J2n arising from the rigidly rotating background structure. The colorful points show the total including the addition of ﹩\Delta {J}_{2n}^{{\rm{winds}}}﹩; these are colored according to their likelihood, with low to high likelihood running purple to green to yellow. The sample is fit to R. A. Jacobson (2014) gravity (1σ and 2σ ellipses in dashed white). Shown for comparison are the more recent R. G. French et al. (2024) measurements (1σ and 2σ ellipses in orange) and improved uncertainties anticipated by M. Parisi et al. (2024) for radio tracking of a future Uranus orbiter (narrow red 1σ ellipse; see text).
Paper: Setting the Stage for Uranian Seismology from Rings and Radial Velocities
Authors: Christopher R. Mankovich, A. James Friedson, Marzia Parisi, Stephen Markham, Janosz W. Dewberry, James Fuller, Matthew M. Hedman, Alex Akins, Mark D. Hofstadter
Figure caption: Interior profiles constrained by a hypothetical ring seismology constraint (curves with color mapped to likelihood) compared to those of their parent sample unconstrained by seismology (gray curves). The top panel shows density profiles ρ(r) for interface models with a rigid (nonoscillating) core; the middle and bottom panels show ρ(r) and N(r), respectively, for models with a composition gradient. Models in gray are constrained solely by J2, J4, and ρ1; color-coded models additionally fit a single m = 2 ring seismology constraint as described in the text. Only a randomly chosen subset of the models—1024 per sample—are shown. The red dashed curves in the gradient case (lower panels) show the best profile yielded by an alternative sample that identifies the same resonance with the higher-order g-mode ﹩{}_{2}^{2}﹩g2 mode instead.
Paper: Setting the Stage for Uranian Seismology from Rings and Radial Velocities
Authors: Christopher R. Mankovich, A. James Friedson, Marzia Parisi, Stephen Markham, Janosz W. Dewberry, James Fuller, Matthew M. Hedman, Alex Akins, Mark D. Hofstadter
Figure caption: OLR locations for the modes highlighted in Figure 10. Point size scales with strength of the gravity perturbation at Uranus’s surface. At ℓ = 7 (circles), the deeply penetrating f-modes interact strongly with modes trapped on the core interface, giving rise to mixed modes that could be observed as a pair of distinct OLRs with the same m. At ℓ = 15 (squares), the f-modes are trapped so closely to the surface that f- and interface modes are effectively decoupled.
Paper: Informed Design of a Gravity Science Experiment for the Future Geophysical Investigation of the Uranian Moons
Authors: Valerio Filice, Gael Cascioli, Sébastien Le Maistre, Rose-Marie Baland, Antony Trinh, Erwan Mazarico, Sander Goossens
Figure caption: Ariel's rms gravity and error spectra expected from the GS experiment with the Decadal and Alternative Tour trajectories and nominal observation strategy (4 hr of tracking time centered on the C/A, Ka-band radiometric data, and optical data comprising four pictures per flyby with 10 landmarks per picture). The simulated gravity field (black dashed line) is computed in accordance with the methodology outlined in Appendix A.3.
Paper: Informed Design of a Gravity Science Experiment for the Future Geophysical Investigation of the Uranian Moons
Authors: Valerio Filice, Gael Cascioli, Sébastien Le Maistre, Rose-Marie Baland, Antony Trinh, Erwan Mazarico, Sander Goossens
Figure caption: Posterior distributions of Ariel's interior parameters, derived from a dedicated MCMC run (50 walkers, 100,000 steps). The uncertainty on the geodetic observables (MoI, k2, ε, and gs) was quantified using covariance analysis. This POD solution was characterized by the Alternative Tour, 4 hr of tracking time around C/A, radiometric (Ka band), and optical (four pictures per flyby, 10 landmarks per picture). The titles show the 15.87th and 84.13th percentiles of the posterior distributions, which correspond to the following uncertainties as defined in Section 2: ﹩{\sigma }_{{d}_{o}}=25.72\,{\rm{km}}﹩, ﹩{\sigma }_{{d}_{s}}=23.80\,{\rm{km}}﹩, and σrock/ice = 0.25. Green points show the truth values.
Paper: Informed Design of a Gravity Science Experiment for the Future Geophysical Investigation of the Uranian Moons
Authors: Valerio Filice, Gael Cascioli, Sébastien Le Maistre, Rose-Marie Baland, Antony Trinh, Erwan Mazarico, Sander Goossens
Figure caption: Orbital mean anomalies of the Uranian satellites at UOP C/A epochs. Circles are for flybys with closest distances less than three body radii, x otherwise.
Paper: Informed Design of a Gravity Science Experiment for the Future Geophysical Investigation of the Uranian Moons
Authors: Valerio Filice, Gael Cascioli, Sébastien Le Maistre, Rose-Marie Baland, Antony Trinh, Erwan Mazarico, Sander Goossens
Figure caption: UOP ground tracks (±30 minutes around C/A) with respect to the Uranian satellites. Ariel's flybys are shown in Figure 6. Colors show the altitude with respect to the moons’ surface, whereas the crosses show the point of C/A. Only flybys with a C/A distance less than three body radii are shown.
Paper: Informed Design of a Gravity Science Experiment for the Future Geophysical Investigation of the Uranian Moons
Authors: Valerio Filice, Gael Cascioli, Sébastien Le Maistre, Rose-Marie Baland, Antony Trinh, Erwan Mazarico, Sander Goossens
Figure caption: Correlation matrices of the POD solutions using the decadal and alternative tours for the parameter set Q + ε + k2 + gs. The measurement settings are characterized by the following: Ka band and 4 hr tracking time, four pictures per flyby, with 10 landmarks per picture. The hydrostatic constraint is not applied to the presented cases.
Paper: THUNDER: A Titan Orbiter Mission Concept for the New Frontiers Program Designed at the JPL Planetary Science Summer School
Authors: Cassandra Seltzer, Rudi Lien, Brandon T. Radzom, Ella Mullikin, Kimberly Bott, Gwendolyn Brouwer, David G. Burtt, Chloe Gentgen, Jewel Abbate, Victor Gandarillas, Austin P. Green, Tristen Head, Jonathon R. Hill, Jennifer N. Larson, Nicholas J. Montiel, M. Regina A. Moreno, Nicholas L. Wagner, Piyumi Wijesekara, James Tuttle Keane, Alfred E. Nash, Jennifer Scully
Figure caption: CAD models of THUNDER’s (a) external and (b) internal components, as well as THUNDER’s (c) stowed and (d) deployed) configurations.
Paper: THUNDER: A Titan Orbiter Mission Concept for the New Frontiers Program Designed at the JPL Planetary Science Summer School
Authors: Cassandra Seltzer, Rudi Lien, Brandon T. Radzom, Ella Mullikin, Kimberly Bott, Gwendolyn Brouwer, David G. Burtt, Chloe Gentgen, Jewel Abbate, Victor Gandarillas, Austin P. Green, Tristen Head, Jonathon R. Hill, Jennifer N. Larson, Nicholas J. Montiel, M. Regina A. Moreno, Nicholas L. Wagner, Piyumi Wijesekara, James Tuttle Keane, Alfred E. Nash, Jennifer Scully
Figure caption: Diagram of a nominal science orbit.
Paper: Beyond Point Masses. IV. Trans-Neptunian Object Altjira Is Likely a Hierarchical Triple Discovered through Non-Keplerian Motion
Authors: Maia A Nelsen, Darin Ragozzine, Benjamin C. N. Proudfoot, William G. Giforos, Will Grundy
Figure caption: Corner plot for the binary quadrupole–point-mass non-Keplerian Altjira orbit fit. Along the tops of the columns are the marginal posterior distribution for each parameter, which can be used to determine the best fit and uncertainty for Gaussian distributions. The contour plots shows the 1σ, 2σ, and 3σ levels of the joint posterior distributions between every pair of given parameters. Of particular interest is the J 2 R 2 posterior, which strongly disfavors the Keplerian model (J 2 R 2 = 0). Also note that the C 22 R 2 parameter is constrained by the prior C 22 R 2 ≤ J 2 R 2/2 but is not constrained by the data, as expected. All angles are measured relative to the the J2000 ecliptic plane on JD 2454300.0 (2007 July 18, 12:00 UT).
Paper: Beyond Point Masses. IV. Trans-Neptunian Object Altjira Is Likely a Hierarchical Triple Discovered through Non-Keplerian Motion
Authors: Maia A Nelsen, Darin Ragozzine, Benjamin C. N. Proudfoot, William G. Giforos, Will Grundy
Figure caption: Astrometric residuals for observations shown in Table 2 for the binary quadrupole–point-mass fit. Points are colored as a function of time to illustrate that the residuals show no major time dependence. These residuals are consistent with Gaussian noise (p-value assuming a χ 2 distribution of 8.6%).
Paper: A Pre-flyby View on the Origin of Asteroid Donaldjohanson, a Target of the NASA Lucy Mission
Authors: Simone Marchi, David Vokrouhlický, David Nesvorný, William F. Bottke, Josef Ďurech, Harold F. Levison
Figure caption: Left panel: segment of Erigone family projected onto the plane defined by the proper semimajor axis aP (abscissa) and absolute magnitude H (ordinate; H < 17.5 mag zone shown). The black symbols are Erigone members observed by WISE constrained by two conditions: (i) pV ≤ 0.125, and (ii) with ∣C∣ ≤ ∣C⋆∣ = 1.7 × 10−5 au (gray lines). The light-gray V-shaped zone is defined by ∣C∣ ≤ 5.2 × 10−6 au, and it corresponds to the region in which the initial fragments from the family-forming event would land assuming an isotropic velocity field and ejection velocity v5 = 24 m s−1 for D = 5 km asteroids (see Equation (5) in D. Vokrouhlický et al. 2006b). The color-highlighted asteroids with known spin state, sidereal rotation period, and pole orientations consist of DJ and objects listed in Table 1: the prograde- and retrograde-rotating cases are red and blue, respectively. The color intervals connect their current position to their past state T = 155 Myr ago using a simplified steady migration by the Yarkovsky effect fixing the present-day rotation state, bulk density ρ = 1.5 g cm−3, and surface thermal inertia Γ = 135 SI (in the DJ case we assumed zero obliquity, but any value  ≤20∘ would lead to about the same conclusions). As expected, the prograde- and retrograde-rotating objects have aP > ac and aP < ac, respectively, and their initial positions are in (or near) the initial velocity dispersal zone. Right panel: distribution of rotation rate values (abscissa; in rotations per day) for Erigone family members (except for (163) Erigone; gray histogram). The same for the subsample of asteroids with resolved rotation pole orientation in Table 1 is highlighted in red. The distribution is not compatible with that of the collisionally relaxed population, characterized by the Maxwellian function; rather, it bears similarity to the YORP-relaxed sample (see P. Pravec et al. 2008, for comparison). The vertical dashed line is the approximate rotation fission limit for low-density and low material cohesion asteroids.
Paper: Ariel’s Medial Grooves: Spreading Centers on a Candidate Ocean World
Authors: Chloe B. Beddingfield, Richard J. Cartwright, Lauren M. Jozwiak, Tom A. Nordheim, G. Wes Patterson
Figure caption: Geologic map and Voyager 2 ISS images of Ariel. The base figure is a digitized and modified version of the geologic map presented in S. Croft & L. Soderblom (1991). Locations of the three known medial grooves are shown in red. See S. Croft & L. Soderblom (1991) for detailed descriptions of mapped units and geologic features. The top blue-bordered Voyager 2 ISS image covers the three medial grooves identified on Ariel (arrows) and where they disappear beyond the terminator (c2684539, V. I. S. Team 1988, 995 m pixel−1). The bottom yellow-bordered ISS image covers three offset fracture systems including Kra Chasma (arrows; c2684535, V. I. S. Team 1988, 999 m pixel−1). While CO and CO2 exhibit stronger spectral features over Ariel's trialing hemisphere, observations by JWST and ground-based facilities are disk integrated, and we cannot discern finer detail on the distribution of these constituents, even at the regional scale. Understanding the spatial relationship between geologic features like medial grooves and carbon oxides is not possible at this time and requires high spatial resolution spectral data collected during close flybys by a Uranus orbiter.