adsabs/AstroCLIMB huggingface dataset:
Paper: Revealing the Mysteries of Venus: The DAVINCI Mission
Authors: James B. Garvin, Stephanie A. Getty, Giada N. Arney, Natasha M. Johnson, Erika Kohler, Kenneth O. Schwer, Michael Sekerak, Arlin Bartels, Richard S. Saylor, Vincent E. Elliott, Colby S. Goodloe, Matthew B. Garrison, Valeria Cottini, Noam Izenberg, Ralph Lorenz, Charles A. Malespin, Michael Ravine, Christopher R. Webster, David H. Atkinson, Shahid Aslam, Sushil Atreya, Brent J. Bos, William B. Brinckerhoff, Bruce Campbell, David Crisp, Justin R. Filiberto, Francois Forget, Martha Gilmore, Nicolas Gorius, David Grinspoon, Amy E. Hofmann, Stephen R. Kane, Walter Kiefer, Sebastien Lebonnois, Paul R. Mahaffy, Alexander Pavlov, Melissa Trainer, Kevin J. Zahnle, Mikhail Zolotov
Figure caption: Alpha Regio at approximately 20 S latitude with up to 3 km of total relief above the adjacent plains. Left-side map view is derived from Arecibo Earth-based radar mapping using 1988 and 2015 data sets controlled by Magellan radar altimetry, with the red “ellipse” being the 3σ error ellipse that constitutes the imaging descent corridor. The color scaling represents pseudo-topography from dark blue (0 km at the mean planetary radius, MPR, of 6051.84 km) to dark brown (over 2.5 km above MPR, AMPR). At right is a perspective view of the entry corridor (red ellipse is ∼310 km in its long-axis) atop the ridged mountains of Alpha Regio with over 900 m of local relief. Arecibo data analysis and processing by the DAVINCI team.
Paper: Revealing the Mysteries of Venus: The DAVINCI Mission
Authors: James B. Garvin, Stephanie A. Getty, Giada N. Arney, Natasha M. Johnson, Erika Kohler, Kenneth O. Schwer, Michael Sekerak, Arlin Bartels, Richard S. Saylor, Vincent E. Elliott, Colby S. Goodloe, Matthew B. Garrison, Valeria Cottini, Noam Izenberg, Ralph Lorenz, Charles A. Malespin, Michael Ravine, Christopher R. Webster, David H. Atkinson, Shahid Aslam, Sushil Atreya, Brent J. Bos, William B. Brinckerhoff, Bruce Campbell, David Crisp, Justin R. Filiberto, Francois Forget, Martha Gilmore, Nicolas Gorius, David Grinspoon, Amy E. Hofmann, Stephen R. Kane, Walter Kiefer, Sebastien Lebonnois, Paul R. Mahaffy, Alexander Pavlov, Melissa Trainer, Kevin J. Zahnle, Mikhail Zolotov
Figure caption: Top panel: a DAVINCI half-scale engineering test unit (ETU) descent sphere (DS) before a Venus environment test as part of the development of the overall mission concept. Bottom panel: a full-scale DS ETU was tested to Venus temperature profiles in 2021 January–February, with successful verification of performance at temperature. The diameter of the sphere is 0.98 m. Cables are related to engineering testing apparatus. This ETU validated the descent timeline temperature profile performance from ∼70 km down to Venus’s surface during DAVINCI mission Phase A activities.
Paper: Revealing the Mysteries of Venus: The DAVINCI Mission
Authors: James B. Garvin, Stephanie A. Getty, Giada N. Arney, Natasha M. Johnson, Erika Kohler, Kenneth O. Schwer, Michael Sekerak, Arlin Bartels, Richard S. Saylor, Vincent E. Elliott, Colby S. Goodloe, Matthew B. Garrison, Valeria Cottini, Noam Izenberg, Ralph Lorenz, Charles A. Malespin, Michael Ravine, Christopher R. Webster, David H. Atkinson, Shahid Aslam, Sushil Atreya, Brent J. Bos, William B. Brinckerhoff, Bruce Campbell, David Crisp, Justin R. Filiberto, Francois Forget, Martha Gilmore, Nicolas Gorius, David Grinspoon, Amy E. Hofmann, Stephen R. Kane, Walter Kiefer, Sebastien Lebonnois, Paul R. Mahaffy, Alexander Pavlov, Melissa Trainer, Kevin J. Zahnle, Mikhail Zolotov
Figure caption: The DAVINCI descent timeline is a carefully choreographed sequence of events. Surface touchdown occurs at 57.04–66.7 minutes at 99% confidence. The timeline for the reference touchdown at 59.7 minutes is shown here.
Paper: Revealing the Mysteries of Venus: The DAVINCI Mission
Authors: James B. Garvin, Stephanie A. Getty, Giada N. Arney, Natasha M. Johnson, Erika Kohler, Kenneth O. Schwer, Michael Sekerak, Arlin Bartels, Richard S. Saylor, Vincent E. Elliott, Colby S. Goodloe, Matthew B. Garrison, Valeria Cottini, Noam Izenberg, Ralph Lorenz, Charles A. Malespin, Michael Ravine, Christopher R. Webster, David H. Atkinson, Shahid Aslam, Sushil Atreya, Brent J. Bos, William B. Brinckerhoff, Bruce Campbell, David Crisp, Justin R. Filiberto, Francois Forget, Martha Gilmore, Nicolas Gorius, David Grinspoon, Amy E. Hofmann, Stephen R. Kane, Walter Kiefer, Sebastien Lebonnois, Paul R. Mahaffy, Alexander Pavlov, Melissa Trainer, Kevin J. Zahnle, Mikhail Zolotov
Figure caption: DAVINCI nominal mission timeline from launch in 2029 June through descent sphere (DS) release in 2031 June. Note that the baseline mission ends in 2031 September after relay of all acquired data sets (DS and flybys) to Earth.
Paper: Revealing the Mysteries of Venus: The DAVINCI Mission
Authors: James B. Garvin, Stephanie A. Getty, Giada N. Arney, Natasha M. Johnson, Erika Kohler, Kenneth O. Schwer, Michael Sekerak, Arlin Bartels, Richard S. Saylor, Vincent E. Elliott, Colby S. Goodloe, Matthew B. Garrison, Valeria Cottini, Noam Izenberg, Ralph Lorenz, Charles A. Malespin, Michael Ravine, Christopher R. Webster, David H. Atkinson, Shahid Aslam, Sushil Atreya, Brent J. Bos, William B. Brinckerhoff, Bruce Campbell, David Crisp, Justin R. Filiberto, Francois Forget, Martha Gilmore, Nicolas Gorius, David Grinspoon, Amy E. Hofmann, Stephen R. Kane, Walter Kiefer, Sebastien Lebonnois, Paul R. Mahaffy, Alexander Pavlov, Melissa Trainer, Kevin J. Zahnle, Mikhail Zolotov
Figure caption: DAVINCI's descent sphere protects the instruments inside from the harsh Venusian ambient environment.
Paper: Chemical Equilibrium between Cores, Mantles, and Atmospheres of Super-Earths and Sub-Neptunes and Implications for Their Compositions, Interiors, and Evolution
Authors: Hilke E. Schlichting, Edward D. Young
Figure caption: Calculated oxygen fugacities of the silicate mantle and atmosphere relative to that of the IW buffer for a 4 M ⊕ planet with unreactive metal. The effects of varying the hydrogen fractions from 1% to 14% by weight at a fixed magma ocean surface temperature of 4500 K are shown here.
Paper: Chemical Equilibrium between Cores, Mantles, and Atmospheres of Super-Earths and Sub-Neptunes and Implications for Their Compositions, Interiors, and Evolution
Authors: Hilke E. Schlichting, Edward D. Young
Figure caption: Mean molecular weights for atmospheres based on equilibration of a 4 M ⊕ planet at 1400 K as a function of total H ranging from 1% to 14% by weight. On the left is the variation with total mass fraction for the reactive metal case at 4500 K, and on the right is the same for the unreactive metal case.
Paper: Atmospheric Overturning Circulation on Dry, Tidally Locked Rocky Planets Is Mainly Driven by Radiative Cooling
Authors: Shuang Wang, Jun Yang
Figure caption: Thermal structures in the CAM3 experiments. (a) Surface temperatures in the pure N2 (black solid) and N2+CO2 (red solid) experiments, and the red dashed line represents CO2 condensation temperature at 1.0 bar. (b) Substellar-point (solid) and nightside-averaged (dashed) temperature profiles. The substellar-point and nightside-averaged surface temperatures are marked by crosses and circles, respectively. (c) Temperature structure in the pure N2 experiment. (d) Same as (c) but in the N2+CO2 experiment, with dashed lines representing the differences from (c) (in units of K). Panels (a), (c), and (d) are shown in tidally locked coordinates and are averaged over the tidally locked longitude. AP is the antistellar point, and SP is the substellar point.
Paper: Atmospheric Overturning Circulation on Dry, Tidally Locked Rocky Planets Is Mainly Driven by Radiative Cooling
Authors: Shuang Wang, Jun Yang
Figure caption: Schematic diagrams of (a) long-term mean tropical Walker circulation on Earth and (b) atmospheric circulation on moist, tidally locked rocky planets. Gray arrows represent overturning circulations, and the black arrow in panel (b) represents equatorial superrotation. The red and blue arrows represent sensible heat and longwave radiation, respectively. Clouds form over the convective regions and are blown by upper winds. During cloud formation, latent heat releases, and it promotes the strong overturning circulation. In panel (b), the potential temperature profile in the substellar region (red line on the left) shows an isentropic structure in the troposphere, indicating the range of the deep convection.
Paper: Atmospheric Overturning Circulation on Dry, Tidally Locked Rocky Planets Is Mainly Driven by Radiative Cooling
Authors: Shuang Wang, Jun Yang
Figure caption: Vertical velocities in pressure coordinates (color shading, negative: upwelling, and positive: downwelling) and mass stream functions (contour lines, in units of 1010 kg s−1) in the pure N2 (a)–(b) and N2+CO2 (c)–(d) experiments. Left and right columns are for CAM3 and ExoCAM, respectively. Panels are shown in tidally locked coordinates. AP is the antistellar point, and SP is the substellar point.
Paper: Atmospheric Overturning Circulation on Dry, Tidally Locked Rocky Planets Is Mainly Driven by Radiative Cooling
Authors: Shuang Wang, Jun Yang
Figure caption: Same as Figure 2 but for the results of ExoCAM experiments.
Paper: Ultraviolet Spectroscopy of Lucy Mission Targets with the Hubble Space Telescope
Authors: Oriel A. Humes, Cristina A. Thomas, Joshua P. Emery, Will M. Grundy
Figure caption: Visible spectra of Patroclus (a) and Orus (b) as observed by the HST and LDT. Spectra were normalized at 0.5 μm. The observed slopes of Patroclus in the 0.4–0.55 μm region agree for the two observations, but the HST spectrum shows a flattening in reflectance starting at 0.55 μm that is not seen in the LDT spectrum. Because this feature has not been reported in the spectrum of Patroclus before, it may be due to instrumental error or rotational variability (see text). In the same wavelength region, the two spectra of Orus are in better agreement.
Paper: Ultraviolet Spectroscopy of Lucy Mission Targets with the Hubble Space Telescope
Authors: Oriel A. Humes, Cristina A. Thomas, Joshua P. Emery, Will M. Grundy
Figure caption: Effect of changing grain sizes of different components of the best-fit model for Orus (see Table 6, Orus 1). Changing the grain size of the pyroxene in this model (panel (a)) controls the magnitude of the slope in the visible and the extent of absorption in the UV. Changing the grain size of the iron scatterers in this model (panel (b)) controls the spectral contrast of the bump feature in the UV, as well as the wavelength at which the spectrum begins to brighten. The spectrum of Orus is also shown for reference purposes, without error bars for clarity; note that the scale used to display the finer details of the spectra cuts off one prominent outlier.
Paper: Ultraviolet Spectroscopy of Lucy Mission Targets with the Hubble Space Telescope
Authors: Oriel A. Humes, Cristina A. Thomas, Joshua P. Emery, Will M. Grundy
Figure caption: The UV and visible spectra of Orus, the Patroclus–Menoetius binary, Eurybates, and Leucus from HST. Spectra are normalized to 0.5 μm and offset for clarity.(The data used to create this figure are available.)
Paper: Ultraviolet Spectroscopy of Lucy Mission Targets with the Hubble Space Telescope
Authors: Oriel A. Humes, Cristina A. Thomas, Joshua P. Emery, Will M. Grundy
Figure caption: Best-fit models for Orus and Patroclus (solid and dashed lines) plotted alongside geometric albedo data from HST and LDT observations (filled and open circles). The spectrum for Patroclus a uses only HST data, while the spectrum for Patroclus b uses HST data for short wavelengths (<0.55 μm) spliced with LDT data at longer wavelengths (>0.55 μm). Patroclus b is offset for clarity. See Table 6 for details of the best-fit models.
Paper: Ring Seismology of the Ice Giants Uranus and Neptune
Authors: Joseph A. A'Hearn, Matthew M. Hedman, Christopher R. Mankovich, Hima Aramona, Mark S. Marley
Figure caption: Radial scan of Uranian rings compared to Lindblad resonance predictions from the medium model. The cyan curve shows the mean ring normal I/F as a function of radius. While the named narrow rings are labeled, many other narrow features can be seen in this scan. The tallest dashed–dotted lines, in red, show the locations of the ℓ = m mode resonances; the intermediate-sized dashed–dotted lines, in green, show the locations of the ℓ − m = 2 mode resonances, and the shortest dashed–dotted lines, in blue, show the locations of the ℓ − m = 4 mode resonances. The integer above each dashed–dotted line corresponds to the azimuthal order m of the mode.
Paper: Ring Seismology of the Ice Giants Uranus and Neptune
Authors: Joseph A. A'Hearn, Matthew M. Hedman, Christopher R. Mankovich, Hima Aramona, Mark S. Marley
Figure caption: Normal-mode resonance location predictions for Neptune. The azimuthal order m is the vertical axis, and distance from the center of Neptune is the horizontal axis, shown in Neptune radii on the bottom and in km on the top. Both OLR and OVR are shown. Several resonances fall in the Galle ring, and others may perturb the inner moons Naiad and Thalassa.
Paper: Ring Seismology of the Ice Giants Uranus and Neptune
Authors: Joseph A. A'Hearn, Matthew M. Hedman, Christopher R. Mankovich, Hima Aramona, Mark S. Marley
Figure caption: Resonance location predictions for Neptunian g-modes. The azimuthal order m is the vertical axis, and distance from the center of Neptune is the horizontal axis, shown in Neptune radii on the bottom and in km on the top. OLRs with ℓ = m, n = 1 are shown as filled circles, while corotation resonances associated with these Lindblad resonances are shown as open circles.
Paper: Ring Seismology of the Ice Giants Uranus and Neptune
Authors: Joseph A. A'Hearn, Matthew M. Hedman, Christopher R. Mankovich, Hima Aramona, Mark S. Marley
Figure caption: Resonance location predictions for Uranian g-modes. The azimuthal order m is the vertical axis, and distance from the center of Uranus is the horizontal axis, shown in Uranus radii on the bottom and in km on the top. Only OLRs with ℓ = m, n = 1 are shown.
Paper: Insight into the Distribution of High-pressure Shock Metamorphism in Rubble-pile Asteroids
Authors: Nicole Güldemeister, Juulia-Gabrielle Moreau, Tomas Kohout, Robert Luther, Kai Wünnemann
Figure caption: Fractions of shocked material. The y-axis indicates the apparent fraction of area shocked to a certain stage (Stöffler et al. 2018) as a function of the impact velocity shown on the x-axis. The numbers on the right sides of the images indicate shock stages of individual gray polygons, for better identification. In panel (a), a 1600 m impactor collides with a 5 km rubble-pile asteroid with boulders of 10% porosity surrounded by a matrix with 75% porosity. In panel (b), the impactor size is decreased to 800 m in diameter. Panel (c) displays the results of a model where the boulder porosity has been increased to 30%, compared with (a). In panel (d), the matrix consists of void (empty space) and all other parameters are constant, as in (a).
Paper: Insight into the Distribution of High-pressure Shock Metamorphism in Rubble-pile Asteroids
Authors: Nicole Güldemeister, Juulia-Gabrielle Moreau, Tomas Kohout, Robert Luther, Kai Wünnemann
Figure caption: Efficiency of shock-darkening as a function of impact velocity. Efficiency is given by the shock-darkened mass normalized to the projectile mass. Square symbols represent simulations with boulder porosities of 10% within the rubble-pile asteroid, and triangular symbols represent boulders with 30% porosity. The ratio of target mass to projectile mass (m t /m p ) corresponds to different impactor sizes. Thus, the respective values for m t /m p  are: 25 for a 1600 m impactor, 60 for a 1200 m impactor, and 200 for an 800 m impactor.
Paper: Insight into the Distribution of High-pressure Shock Metamorphism in Rubble-pile Asteroids
Authors: Nicole Güldemeister, Juulia-Gabrielle Moreau, Tomas Kohout, Robert Luther, Kai Wünnemann
Figure caption: Snapshot series of the evolution of pressure (left panels) and porosity (right panels) during the collision of a 1600 m diameter projectile impacting with 10 km s−1 velocity into a 5 km diameter rubble-pile asteroid. (a) Tracers are displayed at their initial position for better visibility of pressure and porosity values. (b) Tracers are displayed at their current position at a fixed time after impact.
Paper: Insight into the Distribution of High-pressure Shock Metamorphism in Rubble-pile Asteroids
Authors: Nicole Güldemeister, Juulia-Gabrielle Moreau, Tomas Kohout, Robert Luther, Kai Wünnemann
Figure caption: Pressure distribution after collision of an impactor of 10% porosity into a 5 km rubble-pile asteroid with boulders surrounded by fine matrix material. In (a) and (c), the projectile has a diameter of 1600 m, in (b) 800 m. The matrix porosity is 75% in (a) and (b), as well as in the left panel of (c). The boulder porosity is always 10%, except in the left panel of (c), where it is 30%. The matrix in the right panel of (c) is void (100% porosity). The respective impact velocities are noted on each subplot. Thus, (a) shows a comparison of two different impact velocities, in (b) the same scenario is presented for decreased impactor size, and in (c) the boulder porosity is increased in the left panel, whereas in the right panel, the matrix porosity is increased (void). In all figures, the tracers recording the pressure have been set to their initial position, for better visibility.
Paper: Insight into the Distribution of High-pressure Shock Metamorphism in Rubble-pile Asteroids
Authors: Nicole Güldemeister, Juulia-Gabrielle Moreau, Tomas Kohout, Robert Luther, Kai Wünnemann
Figure caption: Sketch of the material ejection from a spherical heterogeneous asteroid (matrix in blue, boulders in orange). The ejection altitude criterion is represented by the black dashed line. The dotted lines respectively show the tangential and normal lines to the criterion circle for the ejected red particle at distance x on the circle. The ejection angle is measured against the local tangent. The ejection velocity is indicated by a black arrow. The escape velocity is indicated by gray arrows and in a normal direction for different positions. Note that the launch distance is constructed from the extrapolation of the velocity vector to the asteroid surface.
Paper: Insight into the Distribution of High-pressure Shock Metamorphism in Rubble-pile Asteroids
Authors: Nicole Güldemeister, Juulia-Gabrielle Moreau, Tomas Kohout, Robert Luther, Kai Wünnemann
Figure caption: Setup of a modeled rubble-pile asteroid with variation of target and projectile properties. Porosity is heterogeneously distributed (macroporosity) and ranges from 10% to 30% for the boulders of various sizes and from 75% to 100% for the surrounding loose material.
Paper: Tilting Uranus via Spin–Orbit Resonance with Planet Nine
Authors: Tiger Lu, Gregory Laughlin
Figure caption: Summary of the results of our simulations. Each grid cell contains the most stable result for that eccentricity/inclination pairing. The background color of each grid cell shows the maximum obliquity reached (see color bar on the right). The size of the central black dot represents the mass of Planet Nine used in that run: small for 5 M ⊕, medium for 7 M ⊕, and large for 10 M ⊕. The number inside each black dot is the maximum obliquity reached to the nearest degree. The colored square in the upper left corner of each grid cell represents the stability of that run: green for stable, yellow for slightly unstable, and orange for significantly unstable. The number in the upper right corner of each cell is the value of α used to achieve the maximum obliquity in arcseconds per year. The slider at the bottom of each cell represents the final semimajor axis of Planet Nine on a scale from 400 to 900 au. Three boxes in this plot show yellow or orange stability; this indicates that there was no perfectly stable run associated with that cell, and the best alternative was selected.
Paper: Tilting Uranus via Spin–Orbit Resonance with Planet Nine
Authors: Tiger Lu, Gregory Laughlin
Figure caption: Spin axis evolution for one of our simulations. Top: evolution of ∣g∣ (first panel), ratio ∣α/g∣ (second panel), obliquity in degrees (third panel), and Planet Nine’s semimajor axis in au (fourth panel). The dotted red line in the first panel marks ∣α/g∣ = 1. Bottom: evolution of Uranus’s spin axis as calculated with Equation (10) with α = 5.″305 yr−1. A maximum obliquity of 103.°46 is achieved, with Planet Nine’s final semimajor axis at 445.4 au. Note the resonance kicks when the ratio ∣α/g∣ crosses unity quickly and the subsequent resonance capture when the long-term average slowly crosses unity from below.
Paper: Tilting Uranus via Spin–Orbit Resonance with Planet Nine
Authors: Tiger Lu, Gregory Laughlin
Figure caption: Closer look at two instances where the obliquity of Uranus exceeds 90°. The top panel shows the first 40 Myr of the obliquity time evolution from Figure 9. Both bottom panels show 3D scatter plots of Uranus’s spin axis in the designated time slices. The red circle represents the projection of Uranus’s orbital plane onto the unit sphere and marks the point at which the obliquity of Uranus exceeds 90°. In panel (a), we see an example of an obliquity kick, as the spin axis continues to circulate after the increase in obliquity. In panel (b), the spin axis is shown in resonance, with the characteristic banana-like libration clearly visible.
Paper: Tilting Uranus via Spin–Orbit Resonance with Planet Nine
Authors: Tiger Lu, Gregory Laughlin
Figure caption: Examples of Uranus’s and Neptune’s semimajor axis evolution for the three stability cases we have defined. The stable case was produced by a Planet Nine with m 9 = 5 M ⊕, e 9 = 0.4, i 9 = 30°; the slightly unstable case with m 9 = 5 M ⊕, e 9 = 0.6, i 9 = 20°; and the unstable case with m 9 = 7 M ⊕, e 9 = 0.4, i 9 = 15°.
Paper: Tilting Uranus via Spin–Orbit Resonance with Planet Nine
Authors: Tiger Lu, Gregory Laughlin
Figure caption: Four hundred self-consistent REBOUND simulations of Planet Nine's dynamical migration. Each line corresponds to one simulation; in each one, Planet Nine is initialized with a random phase. The yellow–purple lines represent pathways that do not deviate far from the expected analytic solution (in black), while the blue–green lines represent pathways that show large excursions from the mean.
Paper: Tilting Uranus via Spin–Orbit Resonance with Planet Nine
Authors: Tiger Lu, Gregory Laughlin
Figure caption: Summary of the results of our most stable simulations with the updated parameters from Brown & Batygin (2021). Quantities are as described in Figure 8, with the exception of mass: a small central circle for m 9 = 4.9 M ⊕, a medium one for m 9 = 6.2 M ⊕, and a large one for m 9 = 8.4 M ⊕.
Paper: Tilting Uranus via Spin–Orbit Resonance with Planet Nine
Authors: Tiger Lu, Gregory Laughlin
Figure caption: Result of a simple evolution of the ratio ∣α/g∣, obtained via integration of Equation (4). The upper left panel displays the evolution of ∣α/g∣ imposed on this simulation; note that the ratio ﹩| \alpha \cos \theta /g| ﹩ saturates at unity. The bottom left panel shows the resulting obliquity evolution. The right panel shows the location of the spin axis over the evolution period. We have zoomed in on one libration timescale to explicitly show the banana-like libration motion the spin axis exhibits when captured into resonance.
Paper: Tilting Uranus via Spin–Orbit Resonance with Planet Nine
Authors: Tiger Lu, Gregory Laughlin
Figure caption: Planet Nine’s forcing frequency on Uranus as a function of semimajor axis. Each line corresponds to a Planet Nine of varying mass (in Earth masses). Note that the forcing frequency does not go to zero, even as Planet Nine’s mass does; this is because each eigenfrequency does not correspond one-to-one with a planet but rather is simply dominated by a given body.