adsabs/AstroCLIMB huggingface dataset:
Paper: Gravity Investigation of Saturn’s Inner System with the Innovative Skimmer Concept
Authors: Marzia Parisi, Mar Vaquero, Matthew M. Hedman, and Matthew S. Tiscareno
Figure caption: Trajectory design for Scenario 1 (left) and Scenario 2 (right). Panels (a) and (b) show the view of the ring overflights (in blue) from the orbital pole, for a total of 21 and 32 passes, respectively, grazing different regions of Saturn’s rings. The orbits of the innermost moons are also displayed. The reference frame is Saturn’s mean equator. Panels (c) and (d) show the orbital altitude of the spacecraft with respect to the ring plane throughout the duration of the track, referenced to the beginning of pass for each ring overflight. The beginning and end of each pass mark the time period for which the spacecraft position is inside the F ring. The altitude is negative in panel (c) because the passes occur below the ring plane, while it is positive in panel (d) as passes occur above the ring plane.
Paper: Gravity Investigation of Saturn’s Inner System with the Innovative Skimmer Concept
Authors: Marzia Parisi, Mar Vaquero, Matthew M. Hedman, and Matthew S. Tiscareno
Figure caption: Example of simulated range-rate residuals from a tracking pass of the spacecraft by NASA’s Deep Space Network antennas at 60 s integration time. The ring overflight (dashed lines) is visible from the Goldstone complex for about 8 hr around closest approach to Saturn. The (one-way) noise rms is 0.010 mm s−1.
Paper: Gravity Investigation of Saturn’s Inner System with the Innovative Skimmer Concept
Authors: Marzia Parisi, Mar Vaquero, Matthew M. Hedman, and Matthew S. Tiscareno
Figure caption: The range-rate residuals in Figure 3 are perturbed in this plot by changing the mass of one of the ring regions. The signatures during the ring overflight and the noise rms of the perturbed data (0.131 mm s−1) are larger than the noise rms of flat residuals.
Paper: Gravity Investigation of Saturn’s Inner System with the Innovative Skimmer Concept
Authors: Marzia Parisi, Mar Vaquero, Matthew M. Hedman, and Matthew S. Tiscareno
Figure caption: Results of the gravity experiment simulations for Scenario 1, in terms of the mass of the C (a), B (b), A (c), and F (d) rings. The plots show the uncertainties (3σ) considering a purely zonal field for Saturn (solid lines), or considering longitudinal/temporal variations of the gravity field absorbed by constant accelerations around closest approach (dashed lines). The uncertainties are a function of the number of passes and generally improve with mission duration. The black dotted lines or gray shaded areas show the range of nominal values (NV) for the masses of the different rings (Tiscareno et al. 2007; Hedman & Nicholson 2014, 2016), except the F ring, for which there is no reliable mass estimate.
Paper: Gravity Investigation of Saturn’s Inner System with the Innovative Skimmer Concept
Authors: Marzia Parisi, Mar Vaquero, Matthew M. Hedman, and Matthew S. Tiscareno
Figure caption: Simulated values (solid lines) and retrieved 3σ uncertainties (dashed line) for the outbound and inbound mass concentrations placed in the F ring.
Paper: Gravity Investigation of Saturn’s Inner System with the Innovative Skimmer Concept
Authors: Marzia Parisi, Mar Vaquero, Matthew M. Hedman, and Matthew S. Tiscareno
Figure caption:  Time series of random accelerations for one of the ring passes of Scenario 1 (#2). The timeframe is 2 hr around closest approach to Saturn. The a priori uncertainty value was chosen according to Cassini gravity science results (Iess et al. 2019).
Paper: Gravity Investigation of Saturn’s Inner System with the Innovative Skimmer Concept
Authors: Marzia Parisi, Mar Vaquero, Matthew M. Hedman, and Matthew S. Tiscareno
Figure caption: Results of the gravity experiment simulations for Scenario 1, in terms of the mass of Prometheus (a) and Pandora (b), and Saturn’s Love number (c). The plots show the uncertainties (3σ) considering a purely zonal field for Saturn (solid lines), or considering longitudinal/temporal variations of the gravity field absorbed by constant accelerations around closest approach (dashed lines). The black dashed–dotted lines in panels (a) and (b) show the distance of the spacecraft from the moon for each flyby under the nominal trajectory. Flybys at less than 104 km distance drive the accuracy of the measurement. Just by chance, the nominal trajectory has two such flybys for Prometheus and three for Pandora. The dotted lines represent the nominal values (NV) (Jacobson 2016; Lainey et al. 2017).
Paper: Gravity Investigation of Saturn’s Inner System with the Innovative Skimmer Concept
Authors: Marzia Parisi, Mar Vaquero, Matthew M. Hedman, and Matthew S. Tiscareno
Figure caption: Equivalent of Figure 5 for Scenario 2.
Paper: Gravity Investigation of Saturn’s Inner System with the Innovative Skimmer Concept
Authors: Marzia Parisi, Mar Vaquero, Matthew M. Hedman, and Matthew S. Tiscareno
Figure caption: Equivalent of Figure 8 for Scenario 2.
Paper: Gravity Investigation of Saturn’s Inner System with the Innovative Skimmer Concept
Authors: Marzia Parisi, Mar Vaquero, Matthew M. Hedman, and Matthew S. Tiscareno
Figure caption: Correlation matrix among the parameters of interest (Table 3, on the vertical axis), as well as with additional gravitational parameters (horizontal axis). Correlations are considered low below 50%.
Paper: Gravity Investigation of Saturn’s Inner System with the Innovative Skimmer Concept
Authors: Marzia Parisi, Mar Vaquero, Matthew M. Hedman, and Matthew S. Tiscareno
Figure caption: (a) Spacecraft ground tracks during the six close flybys of Mimas (background image credit: NASA/JPL-Caltech/Space Science Institute). (b) Altitude of the flybys as a function of longitude. (c) Mimas’s true anomaly around Saturn as a function of flyby number.
Paper: Gravity Investigation of Saturn’s Inner System with the Innovative Skimmer Concept
Authors: Marzia Parisi, Mar Vaquero, Matthew M. Hedman, and Matthew S. Tiscareno
Figure caption: Predicted uncertainty (3σ) for Mimas’s Love number (k2), as a function of flyby number.
Paper: Active Main-belt Asteroid (6478) Gault: Constraint on Its Cohesive Strength and the Fate of Ejected Particles in the Solar System
Authors: Pierce M. Jackson, Ryota Nakano, Yaeji Kim, and Masatoshi Hirabayashi
Figure caption: Distribution of Y* at the x-z plane (the cross section along the spin axis). The spin period is P = 2.5 hr. Panels (a), (b), (c), and (d) describe the bulk densities of 1.50, 1.75, 2.50, and 3.00 g cm−3, respectively.
Paper: Active Main-belt Asteroid (6478) Gault: Constraint on Its Cohesive Strength and the Fate of Ejected Particles in the Solar System
Authors: Pierce M. Jackson, Ryota Nakano, Yaeji Kim, and Masatoshi Hirabayashi
Figure caption: Structural conditions as functions of spin period and bulk density. The red line is the critical spin period Pc as a function of the bulk density. The purple line is the spin period at which the central region structurally fails as a function of the bulk density, which is obtained by polynomial interpolation of the structural model results (purple circles). The gravitational acceleration dominant regime is indicated by the purple shaded region. The centrifugal acceleration dominant regime is indicated by the red shaded region.
Paper: Active Main-belt Asteroid (6478) Gault: Constraint on Its Cohesive Strength and the Fate of Ejected Particles in the Solar System
Authors: Pierce M. Jackson, Ryota Nakano, Yaeji Kim, and Masatoshi Hirabayashi
Figure caption: Average particle distance (blue) from Gault of simulated particles ejected during the 2018 December 24 event after 1500 yr for cases (a) Qpr = 0, (b) Qpr = 1, and (c) Qpr = 2. Red indicates the maximum distance obtained by any particle at that time. Green indicates the minimum distance obtained by any particle at that time. Cases (b) and (c) have critical times (tc) of 1160 and 542 yr, respectively. This is where the minimum distances (green curve) return to near zero and indicates the amount of time it takes for ejected particles to migrate along Gault’s orbit and potentially return to or impact Gault. None of these minimum values reach 0, but they have averages of 5.7 × 10−5 au, 0.06 au (beyond critical time of 1160 yr), and 0.08 au (beyond critical time of 542 yr) for each respective case.
Paper: Active Main-belt Asteroid (6478) Gault: Constraint on Its Cohesive Strength and the Fate of Ejected Particles in the Solar System
Authors: Pierce M. Jackson, Ryota Nakano, Yaeji Kim, and Masatoshi Hirabayashi
Figure caption: Schematic of Gault’s structure and ejected dust particle evolution: (a) surface structure failure, (b) internal structure failure, (c) orbital evolution of dust particles not perturbed by SRP and PRD (Qpr = 0), and (d) orbital evolution of dust particles perturbed by SRP and PRD (Qpr > 0). For the Qpr = 0 case, none of the ejected particles came back on the timescales we tested, i.e., the times we considered were less than its critical time. For Qpr > 0, the particles are fully distributed along the Gault’s orbit after tc ranging between 700 and 5300 yr (see the online animated figure included in Appendix B). Here tc strongly depends on Qpr.
Paper: Active Main-belt Asteroid (6478) Gault: Constraint on Its Cohesive Strength and the Fate of Ejected Particles in the Solar System
Authors: Pierce M. Jackson, Ryota Nakano, Yaeji Kim, and Masatoshi Hirabayashi
Figure caption: Distribution of Y* at the x-z plane. The oblateness is 0.889, which is the same as Bennu’s. The spin period is P = 2.5 hr. Panels (a), (b), (c), and (d) describe the bulk densities of 1.50, 1.75, 2.50, and 3.00 g cm−3, respectively.
Paper: Active Main-belt Asteroid (6478) Gault: Constraint on Its Cohesive Strength and the Fate of Ejected Particles in the Solar System
Authors: Pierce M. Jackson, Ryota Nakano, Yaeji Kim, and Masatoshi Hirabayashi
Figure caption: Distribution of Y* at the x-z plane. The oblateness is 0.635, which is the same as Betulia’s. The spin period is P = 2.5 hr. Panels (a), (b), (c), and (d) describe the bulk densities of 1.50, 1.75, 2.50, and 3.00 g cm−3, respectively.
Paper: Modeling Meteoroid Impacts on the Juno Spacecraft
Authors: Petr Pokorný, Jamey R. Szalay, Mihály Horányi, and Marc J. Kuchner
Figure caption: Variations of the heliocentric distance, Rhel, of Juno and the pointing angles of the solar array, (λJuno − λ⊙, βJuno), in time starting on 2013 January 1. The primary x-axis shows the number of days since 2013 January 1 (τ), whereas the secondary (top) x-axis shows the calendar years. The solar-array pointing longitude, λJuno − λ⊙, and latitude, βJuno, in heliocentric ecliptic coordinates are represented by blue and green solid lines, respectively. The pointing angle values in degrees are denoted by the left-hand-side y-axis. The spacecraft heliocentric distance, Rhel, in au is represented by the red/white solid line where its values are denoted by the right-hand-side y-axis. The Rhel line is color-coded by the distance of Juno from the ecliptic (in au), where the range of values is shown in the legend. The three cyan shaded areas represent time periods with limited/no detection rates. G1 and G2 data gaps are caused by a significant orientation change of the spacecraft. G3 represents a period when the instruments were in a different operational mode, during which impact detection was suppressed.
Paper: Modeling Meteoroid Impacts on the Juno Spacecraft
Authors: Petr Pokorný, Jamey R. Szalay, Mihály Horányi, and Marc J. Kuchner
Figure caption: The same as Figure 2, but now for dust particles released from the Martian Hill sphere. For each particle diameter, we scaled the according simulation to provide a maximum of N = 200 modeled STEs per day. Particle cloud with D = 1.5 μm peak around 2013 January 1, while the particle clouds of larger particles with D > 1.5 μm have peak values around the G2 gap (τ ≈ 278). No dust size or their combination is able to reproduce the STE rate profile reported in Jorgensen et al. (2021).
Paper: Modeling Meteoroid Impacts on the Juno Spacecraft
Authors: Petr Pokorný, Jamey R. Szalay, Mihály Horányi, and Marc J. Kuchner
Figure caption: Meteoroid impact directions of the four model populations. Panel (A): number of impacts per day per 2° × 2° solid angle in Sun-centered ecliptic coordinates for MBA, JFC, HTC, and OCC model meteoroids (color-coded). We assume that the target is a sphere with a cross-section of 60 m2 and the impact detection efficiency is 7%. Juno’s solar-array pointing direction is represented by a cross symbol that is surrounded by dashed circles showing levels of ﹩\cos \varphi ﹩ factor (Equation (3)), i.e., the attenuation of the effective collecting area due to shallower impact angles. Any impacts outside the “0” contour result in no STEs. This panel shows impactor distribution on 2013 May 5 (τ = 124) when Juno reported 163 STEs and our model predicted N = 0.12 STEs. The spacecraft was at heliocentric distance Rhel = 1.5 au, moving toward perihelion. Most of the impactors striked Juno from the sunward direction and are not expected to produce STEs. Panel (B): the same as Panel A but now for the postperihelion passage on 2013 December 6 (τ = 339). The spacecraft was at Rhel = 1.38 au; Juno reported 43 STEs and our model predicted N = 2.43 STEs. All meteoroid populations were concentrated in the antihelion region and were impacting Juno’s solar array efficiently.
Paper: The Ice Coverage of Earth-like Planets Orbiting FGK Stars
Authors: Caitlyn Wilhelm, Rory Barnes, Russell Deitrick, and Rachel Mellman
Figure caption: Annual climate of an Earth-like planet if its obliquity is 55° and its insolation is 96% of the solar constant. Left: the incident solar radiation as a function of day and latitude. Middle: surface temperature. Right: ice formation rate on land. Positive values indicate ice accumulation; negative values, ice melting/ablation. VPLanet:examples/IceBelts
Paper: The Ice Coverage of Earth-like Planets Orbiting FGK Stars
Authors: Caitlyn Wilhelm, Rory Barnes, Russell Deitrick, and Rachel Mellman
Figure caption: Formation of an ice belt on the planet shown in Figure 1. Top panel: surface temperature. Note that the values are averaged over the orbit and over land and sea. Temperatures over land are, in fact, below freezing for much of the year. Second panel: albedo of the sea at the TOA. Third panel: albedo of the land at the TOA. Fourth panel: height of the ice sheet on land. Bottom panel: depression of the lithosphere due to ice mass loading. Note that in this case sea ice does not form. The open water at the equator maintains an annually averaged temperature above 0° C even though ice sheets persist throughout the year on land. VPLanet:examples/IceBelts
Paper: The Ice Coverage of Earth-like Planets Orbiting FGK Stars
Authors: Caitlyn Wilhelm, Rory Barnes, Russell Deitrick, and Rachel Mellman
Figure caption: Top: parameter combinations that permit ice belt formation for a planet orbiting a G dwarf on a circular orbit. The light-blue area is where ice belts are stable, dark blue is where no permanent ice is possible, purple is where ice caps are stable, and white is where the planet is completely ice covered. Bottom: the same parameter combinations as above, but with a cold start to highlight hysteresis. GDwarfStatic
Paper: The Ice Coverage of Earth-like Planets Orbiting FGK Stars
Authors: Caitlyn Wilhelm, Rory Barnes, Russell Deitrick, and Rachel Mellman
Figure caption: Same as Figure 3, but for an F dwarf host star. FDwarfStatic
Paper: The Ice Coverage of Earth-like Planets Orbiting FGK Stars
Authors: Caitlyn Wilhelm, Rory Barnes, Russell Deitrick, and Rachel Mellman
Figure caption: Same as Figure 3, but for a K dwarf host star. KDwarfStatic
Paper: The Ice Coverage of Earth-like Planets Orbiting FGK Stars
Authors: Caitlyn Wilhelm, Rory Barnes, Russell Deitrick, and Rachel Mellman
Figure caption: Comparison of the ice caps and belt parameter space ranges for warm-start planets on circular orbits of F (light blue), G (orange), and K (red) dwarf stars, with each region labeled accordingly. The dashed lines between the cap and belt regions are the approximate location of the boundary between snowball and ice-free ice states. StaticCompare
Paper: The Ice Coverage of Earth-like Planets Orbiting FGK Stars
Authors: Caitlyn Wilhelm, Rory Barnes, Russell Deitrick, and Rachel Mellman
Figure caption: Comparisons of ice caps and belt regimes for planets orbiting F (top), G (middle), and K (bottom) as a function of eccentricity, with e = 0 (solid), e = 0.1 (dashed), e = 0.2 (dotted), and e = 0.3 (dashed–dotted). Ice belts are unstable at e > 0.3 for G star planets and e > 0.1 for F star planets; thus, the respective curves are omitted. EccCompare
Paper: The Ice Coverage of Earth-like Planets Orbiting FGK Stars
Authors: Caitlyn Wilhelm, Rory Barnes, Russell Deitrick, and Rachel Mellman
Figure caption: Outcomes of our five cases of evolving planets, grouped by host star spectral type. (Note the logarithmic scale.) Despite wide ranges of assumptions, the outcomes are relatively constant, suggesting that variations in albedo, rotational cycle, or orbital cycle do not strongly influence the climate states. DynamicCompare
Paper: The Ice Coverage of Earth-like Planets Orbiting FGK Stars
Authors: Caitlyn Wilhelm, Rory Barnes, Russell Deitrick, and Rachel Mellman
Figure caption: An example from the dynamic case G dwarf set that generated a stable ice belt. Top left: surface temperature. Top middle left: TOA albedo. Bottom middle left: ice sheet height. Bottom left: bedrock height (note the negative scale). Top right: annual average instellation. Top middle right: obliquity. Bottom middle right: eccentricity. Bottom right: COPP; see Equation (5). DynamicExample
Paper: The Ice Coverage of Earth-like Planets Orbiting FGK Stars
Authors: Caitlyn Wilhelm, Rory Barnes, Russell Deitrick, and Rachel Mellman
Figure caption: An example of a planet whose ε cycle causes the planet to periodically possess ice belts and ice caps, with ice-free epochs in between. The format is the same as in Figure 9. PeriodicExample
Paper: The Ice Coverage of Earth-like Planets Orbiting FGK Stars
Authors: Caitlyn Wilhelm, Rory Barnes, Russell Deitrick, and Rachel Mellman
Figure caption: An example of a planet whose ε and eccentricity cycle cause the planet’s climate to evolve chaotically, with epochs of both equatorial ice and polar ice. The format is the same as in Figure 9. ChaoticExample
Paper: The Ice Coverage of Earth-like Planets Orbiting FGK Stars
Authors: Caitlyn Wilhelm, Rory Barnes, Russell Deitrick, and Rachel Mellman
Figure caption: Range and average ice heights of ice caps as a function of latitude for stars orbiting F (top), G (middle), and K (bottom) dwarf stars. Note the different scales of the x-axes. Light-gray curves show 100 randomly selected individual simulations, while black shows the average of all simulations that concluded with an ice belt. Although the averages are all symmetric about the poles, some individual ice caps are significantly displaced. CapHeight
Paper: The Ice Coverage of Earth-like Planets Orbiting FGK Stars
Authors: Caitlyn Wilhelm, Rory Barnes, Russell Deitrick, and Rachel Mellman
Figure caption: Same as Figure 12, but for ice belts. Note that although the averages are all symmetric about the equator, some individual ice belts are significantly displaced into either the northern or southern hemisphere. BeltHeight
Paper: Polyaromatic Units Set the Albedo of Dark Extraterrestrial Materials
Authors: Romain Maupin, Zahia Djouadi, Rosario Brunetto, Obadias Mivumbi, Christophe Sandt, and Ferenc Borondics
Figure caption: The Vis–NIR reflectance spectra of the studied IDPs. The allocated number for each IDP (see Table 1) is indicated above its spectrum. The spectra are shifted in the reflectance axis for clarity. For more details on how these spectra have been obtained, see Maupin et al. (2020).
Paper: Polyaromatic Units Set the Albedo of Dark Extraterrestrial Materials
Authors: Romain Maupin, Zahia Djouadi, Rosario Brunetto, Obadias Mivumbi, Christophe Sandt, and Ferenc Borondics
Figure caption: The aliphatic band in the [3000–2800] cm−1 range (panel a) and the silicate band in the [1250–750] cm−1 range) for each IDP represented by its allocated number. These spectra are first corrected from a local linear baseline, then from the silicon oil contribution and finally normalized to the maximum of the silicate peak. The spectra have been shifted in the absorbance axis for clarity.
Paper: Polyaromatic Units Set the Albedo of Dark Extraterrestrial Materials
Authors: Romain Maupin, Zahia Djouadi, Rosario Brunetto, Obadias Mivumbi, Christophe Sandt, and Ferenc Borondics
Figure caption: Comparison of the Raman spectra of the studied IDPs, identified by their allocated number, and the silicon oil spectrum. The black dashed lines point out the positions of the G and D bands and the gray dashed line points out the silicon oil feature in the range of interest. The spectra have been shifted in the intensity axis for clarity.
Paper: Polyaromatic Units Set the Albedo of Dark Extraterrestrial Materials
Authors: Romain Maupin, Zahia Djouadi, Rosario Brunetto, Obadias Mivumbi, Christophe Sandt, and Ferenc Borondics
Figure caption: Panel (a) ΓG as a function of ωG for the studied IDPs (represented by the the black points and their corresponding allocated number), and the meteorites Murchison (blue square), Allende (gray square), Tagish Lake (red square), and FRO95002 (light gray square). Panel (b) ΓG + ΓD in function of ωG for IDPs (black points), Murchison (blue square), Allende (gray square), Tagish Lake (red square), and FRO95002 (light gray square) meteorites.
Paper: Polyaromatic Units Set the Albedo of Dark Extraterrestrial Materials
Authors: Romain Maupin, Zahia Djouadi, Rosario Brunetto, Obadias Mivumbi, Christophe Sandt, and Ferenc Borondics
Figure caption: The N(CH)/N(SiO) ratio vs. the phyllosilicate fraction in IDPs. The light gray symbols are the IDPs from Merouane et al. (2014). The red square shows the value obtained on a grain of the Tagish Lake (TL). The error on the phyllosilicate fraction is about 5%. The dashed line is a linear adjustment of the trend observed on hydrated materials. Note that the vertical axis is in log-scale in panel (a). Panel (b) shows the linear increase of the N(CH)/N(SiO) ratio with the phyllosilicate fraction in the hydrated IDPs.
Paper: Polyaromatic Units Set the Albedo of Dark Extraterrestrial Materials
Authors: Romain Maupin, Zahia Djouadi, Rosario Brunetto, Obadias Mivumbi, Christophe Sandt, and Ferenc Borondics
Figure caption: Reflectance level at 0.55 μm of the IDPs as a function of the N(CH)/N(SiO) ratio.
Paper: Polyaromatic Units Set the Albedo of Dark Extraterrestrial Materials
Authors: Romain Maupin, Zahia Djouadi, Rosario Brunetto, Obadias Mivumbi, Christophe Sandt, and Ferenc Borondics
Figure caption: (a) Reflectance level at 0.55 μm of IDPs, Murchison (blue square), Allende (gray square), and Tagish Lake (red square) meteorites as a function of the ωG parameter. (b) Reflectance level at 0.55 μm in function of the width of the G+D band for IDPs (black points) and Murchison (blue square), Allende (gray square), and Tagish Lake (red square) meteorites.
Paper: Polyaromatic Units Set the Albedo of Dark Extraterrestrial Materials
Authors: Romain Maupin, Zahia Djouadi, Rosario Brunetto, Obadias Mivumbi, Christophe Sandt, and Ferenc Borondics
Figure caption: IR spectra of IDPs and silicon oil. The upper spectrum in each panel is the one of the silicon oil obtained after normalization to the 800 cm−1 band. The other spectra are those of IDPs; they are normalized to the maximum of the silicate feature. The identification of each IDP is given above its spectrum. The spectra have been shifted in the vertical axis for clarity. The two bottom panels show the same spectra corrected from the silicon oil contribution.