adsabs/AstroCLIMB huggingface dataset:
Paper: Tilting Uranus via Spin–Orbit Resonance with Planet Nine
Authors: Tiger Lu, Gregory Laughlin
Figure caption: Evolution of the four outer planets as described by the secular theory of Laplace (1784). The upper panel shows the evolution of inclination of all four outer planets; note the complex yet semiperiodic behavior. The bottom panel shows the evolution of g, the rate of change of Uranus’s node position.
Paper: Exploring the Shallow Subsurface of Mars with the Ma_MISS Spectrometer on the ExoMars Rover Rosalind Franklin
Authors: M. C. De Sanctis, F. Altieri, E. Ammannito, S. De Angelis, B. Ehlmann, M. Ferrari, A. Frigeri, S. Fonte, M. Formisano, M. Giardino, A. Apuzzo, J. Brossier, N. Costa, L. Rossi, G. Vizzini, G. V. Ciarletti, F. Westall
Figure caption: (a) Rock/mineral slab spectra acquired with the Ma_MISS flight model during the on-ground calibration campaign; data are compared with spectra acquired on the same samples at the INAF laboratory (labeled FSpec). (b) Rock/mineral slab spectra acquired with the Ma_MISS flight model (cross lines) during the on-ground calibration campaign; data are compared with spectra acquired on the same samples at the INAF laboratory (solid lines). Here the spectra have been normalized at 1450, 1500, and 1700 nm for gypsum, Lava Montiferru MFEB1, and dunite, respectively.
Paper: Exploring the Shallow Subsurface of Mars with the Ma_MISS Spectrometer on the ExoMars Rover Rosalind Franklin
Authors: M. C. De Sanctis, F. Altieri, E. Ammannito, S. De Angelis, B. Ehlmann, M. Ferrari, A. Frigeri, S. Fonte, M. Formisano, M. Giardino, A. Apuzzo, J. Brossier, N. Costa, L. Rossi, G. Vizzini, G. V. Ciarletti, F. Westall
Figure caption: WCS-MC standard spectral target (LabSphere©) WCS-MC, acquired with Ma_MISS FM integrated within the drill FM. Spectra have been acquired with the Ma_MISS tip only (thick blue line), and with the extension rods mounted up to three rods (tip + one rod: orange; tip + two rods: yellow; tip + three rods: magenta). The spectrum of WCS-MC acquired during the on-ground calibration campaign (TDet = −50 °C) is shown for comparison (black). The spectrum of WCS-MC measured with FieldSpec at the IAPS laboratory is also shown (thin blue line). In panel (a), the spectra are shifted in reflectance for clarity. In panel (b), the spectra have been normalized at 1430 nm. The spectral resolution of the FieldSpec is about 10 times better with respect to the Ma_MISS one.
Paper: Exploring the Shallow Subsurface of Mars with the Ma_MISS Spectrometer on the ExoMars Rover Rosalind Franklin
Authors: M. C. De Sanctis, F. Altieri, E. Ammannito, S. De Angelis, B. Ehlmann, M. Ferrari, A. Frigeri, S. Fonte, M. Formisano, M. Giardino, A. Apuzzo, J. Brossier, N. Costa, L. Rossi, G. Vizzini, G. V. Ciarletti, F. Westall
Figure caption: Left: spectra of different minerals acquired with the Ma_MISS breadboard and resampled and processed to simulate the Ma_MISS FM spectral sampling and resolution. Right: zoom-in of the region of 1.4 μm for two phyllosilicates: nontronite (Fe-rich) and hectorite (Mg-rich). The laboratory spectra are affected by gaps due to the low S/N occurring in the 1.0–1.1 μm and 1.7–1.8 μm ranges of the spectrometer (FieldSpec) used in the laboratory. The Ma_MISS instrument is not affected by these gaps.
Paper: Exploring the Shallow Subsurface of Mars with the Ma_MISS Spectrometer on the ExoMars Rover Rosalind Franklin
Authors: M. C. De Sanctis, F. Altieri, E. Ammannito, S. De Angelis, B. Ehlmann, M. Ferrari, A. Frigeri, S. Fonte, M. Formisano, M. Giardino, A. Apuzzo, J. Brossier, N. Costa, L. Rossi, G. Vizzini, G. V. Ciarletti, F. Westall
Figure caption: (a) Slab of dunite rock; (b) slab of gypsum; (c) slab of Montiferru (Bonàrcado) lava. These pictures were taken during the acquisition with Ma_MISS (panels (a)–(b)) and before the measurements (panel (c)).
Paper: Exploring the Shallow Subsurface of Mars with the Ma_MISS Spectrometer on the ExoMars Rover Rosalind Franklin
Authors: M. C. De Sanctis, F. Altieri, E. Ammannito, S. De Angelis, B. Ehlmann, M. Ferrari, A. Frigeri, S. Fonte, M. Formisano, M. Giardino, A. Apuzzo, J. Brossier, N. Costa, L. Rossi, G. Vizzini, G. V. Ciarletti, F. Westall
Figure caption: Ma_MISS lamp illuminating a spectral target during the measurements on the tip and rods in Leonardo Nerviano (MI).
Paper: Simulation of Freezing Cryomagma Reservoirs in Viscoelastic Ice Shells
Authors: Elodie Lesage, Hélène Massol, Samuel M. Howell, Frédéric Schmidt
Figure caption: (a) Deformation and (b) radial and (c) tangential stress fields around a spherical 500 m radius reservoir located 2 km deep within the ice shell (reservoir A; see Table 2). Reservoir A is surrounded by a 10 m viscoelastic ice shell, itself embedded in elastic ice. Results are plotted at time τ  c , which is the critical freezing time required to reach an eruption under the nondeformable wall approximation calculated at the first iteration of our algorithm. As σ  θ θ  reaches the critical value ΔP/2 (see Equation (4)), an eruption is possible in the case of a nondeformable wall, but in reality, a longer critical freezing time τ cv will be necessary to reach the critical overpressure once we take into account the wall deformation.
Paper: Simulation of Freezing Cryomagma Reservoirs in Viscoelastic Ice Shells
Authors: Elodie Lesage, Hélène Massol, Samuel M. Howell, Frédéric Schmidt
Figure caption: (a) Pressure in the reservoir due to cryomagma freezing as modeled by Lesage et al. (2020) under the nondeformable wall approximation. Here ΔP  c  is the critical overpressure necessary to trigger an eruption, and τ  c  is the critical freezing time necessary to reach ΔP  c . (b) Linear pressure source function used in this model.
Paper: Simulation of Freezing Cryomagma Reservoirs in Viscoelastic Ice Shells
Authors: Elodie Lesage, Hélène Massol, Samuel M. Howell, Frédéric Schmidt
Figure caption: (a) Deformation and (b) radial and (c) tangential stress fields around a spherical 500 m radius reservoir located 8 km deep in the ice shell (reservoir B; see Table 2). Reservoir B is surrounded by viscoelastic ice only. Results are plotted at time t = τ  c , which is the critical freezing time required to reach an eruption under the nondeformable wall approximation calculated at the first iteration of our algorithm. As σ  θ θ  never reaches the critical value ΔP/2 (see Equation (4)), eruptions cannot be triggered (τ cv tends toward ∞).
Paper: Simulation of Freezing Cryomagma Reservoirs in Viscoelastic Ice Shells
Authors: Elodie Lesage, Hélène Massol, Samuel M. Howell, Frédéric Schmidt
Figure caption: Black line: Maxwell time τ M of the ice, far from any reservoir. Blue line: critical freezing time τ  c  of a 500 m radius reservoir. When τ M ≫ τ  c  (light blue region), the ice can be approximated as an elastic medium, and the viscous component is negligible. When τ M ≲ τ  c  (white region), the ice behaves as a viscoelastic material. The transition takes place at H ≃ 6 km for a 500 m radius reservoir at a temperature T ≃ 194 K.
Paper: Simulation of Freezing Cryomagma Reservoirs in Viscoelastic Ice Shells
Authors: Elodie Lesage, Hélène Massol, Samuel M. Howell, Frédéric Schmidt
Figure caption: Schematic model of a cryomagma reservoir surrounded by viscoelastic and elastic ice. The cryomagma reservoir has a radius R 1, and the viscoelastic shell has a radius R 2. Here K 1 and K 2 are the bulk moduli of, respectively, the viscoelastic and elastic ice, and G 1 and G 2 are their respective shear moduli. Here r is the radial coordinate, and η is the viscosity of the viscoelastic ice (where R 1 < r < R 2). In the reservoir, the overpressure ΔP comes from cryomagma freezing. Adapted from Dragoni & Magnanensi (1989).
Paper: Simulation of Freezing Cryomagma Reservoirs in Viscoelastic Ice Shells
Authors: Elodie Lesage, Hélène Massol, Samuel M. Howell, Frédéric Schmidt
Figure caption: Pressure drop in the reservoir at each iterative step of the algorithm and the associated critical freezing time. The algorithm converges to a realistic critical freezing time τ cv in 17 iterations. The results were obtained with a shallow reservoir (see reservoir A in Table 2).
Paper: Simulation of Freezing Cryomagma Reservoirs in Viscoelastic Ice Shells
Authors: Elodie Lesage, Hélène Massol, Samuel M. Howell, Frédéric Schmidt
Figure caption: Numerical procedure used to calculate the critical pressure and freezing time in the case of a deformable wall.
Paper: Simulation of Freezing Cryomagma Reservoirs in Viscoelastic Ice Shells
Authors: Elodie Lesage, Hélène Massol, Samuel M. Howell, Frédéric Schmidt
Figure caption: Dimensionless thickness of the viscoelastic shell around a 500 m radius reservoir at the end of the freezing (t = τ  c  calculated with the nondeformable wall approximation) as a function of its depth in the ice crust.
Paper: Callisto and Europa Gravity Measurements from JUICE 3GM Experiment Simulation
Authors: Paolo Cappuccio, Mauro Di Benedetto, Daniele Durante, Luciano Iess
Figure caption: Callisto degree strength and JUICE ground tracks. Panel (a) reports the results for the nominal tour, while panel (b) reports the results for the backup tour.
Paper: Callisto and Europa Gravity Measurements from JUICE 3GM Experiment Simulation
Authors: Paolo Cappuccio, Mauro Di Benedetto, Daniele Durante, Luciano Iess
Figure caption: Callisto k 2 with and without an ocean, from Moore & Schubert (2003). The value of the Love number is reported for different values of the viscosity μ and the shell thickness d. The dark-gray shaded area represents the uncertainty, ﹩{\sigma }_{{k}_{2}}=0.059,﹩ obtained from the numerical simulations, while the lighter-gray shaded area corresponds to ﹩3{\sigma }_{{k}_{2}}﹩. The expected range for the ice viscosity is between 1014 and 1018 Pa s (Durham & Stern 2003 Nagel et al. 2004).
Paper: Callisto and Europa Gravity Measurements from JUICE 3GM Experiment Simulation
Authors: Paolo Cappuccio, Mauro Di Benedetto, Daniele Durante, Luciano Iess
Figure caption: Callisto gravity field power of normalized coefficient. The black line represents the simulated gravity field with Ak  = 1, the blue line is the 3σ reconstructed uncertainty with the nominal tour, and the red line is the 3σ uncertainty obtained with the backup tour. Note that for the backup trajectory the estimation of the gravity field could be limited to a lower degree.
Paper: Callisto and Europa Gravity Measurements from JUICE 3GM Experiment Simulation
Authors: Paolo Cappuccio, Mauro Di Benedetto, Daniele Durante, Luciano Iess
Figure caption: Callisto flybys’ mean anomaly distribution. The flybys of the nominal tour 150l0a are shown in blue, and those for the backup launch option are in red.
Paper: Callisto and Europa Gravity Measurements from JUICE 3GM Experiment Simulation
Authors: Paolo Cappuccio, Mauro Di Benedetto, Daniele Durante, Luciano Iess
Figure caption: Representations of time slot mask for radio-tracking passes during a flyby. Note that the expected coverage from ground stations during each slot has been considered.
Paper: Callisto and Europa Gravity Measurements from JUICE 3GM Experiment Simulation
Authors: Paolo Cappuccio, Mauro Di Benedetto, Daniele Durante, Luciano Iess
Figure caption: Callisto gravity anomaly uncertainties. Panel (a) reports the map for the nominal tour, while panel (b) reports the map of the backup tour.
Paper: Unsupervised Machine Learning for Exploratory Data Analysis of Exoplanet Transmission Spectra
Authors: Konstantin T. Matchev, Katia Matcheva, Alexander Roman
Figure caption: A three-dimensional visualization of the transit spectra in the benchmark database in the three-dimensional space of the first three PCA components, viewed from two different vantage points. In each panel, the points are color-coded according to one of the input variables: ﹩{X}_{{{\rm{H}}}_{2}{\rm{O}}}﹩ (first row), ﹩{X}_{\mathrm{HCN}}﹩ (second row), ﹩{X}_{{\mathrm{NH}}_{3}}﹩ (third row), and κ cl (last row).
Paper: Unsupervised Machine Learning for Exploratory Data Analysis of Exoplanet Transmission Spectra
Authors: Konstantin T. Matchev, Katia Matcheva, Alexander Roman
Figure caption: The results from K-means clustering with four clusters in the two PCA planes of Figure 7. Note that the clustering was performed in the full 13-dimensional space of standardized PCA components, with the results then being plotted in two dimensions only for visualization purposes. The four clusters found by the algorithm are color-coded with blue, green, yellow, and black.
Paper: Unsupervised Machine Learning for Exploratory Data Analysis of Exoplanet Transmission Spectra
Authors: Konstantin T. Matchev, Katia Matcheva, Alexander Roman
Figure caption: Four transit spectra from the very tips of each of the four different branches discussed in the text: thick cloud (black circles), high H2O (blue squares), high HCN (red diamonds), and high NH3 (green triangles). The input parameters for each spectrum are listed in Table 2.
Paper: Let It Go: Geophysically Driven Ejection of the Haumea Family Members
Authors: Jessica L. Noviello, Steven J. Desch, Marc Neveu, Benjamin C. N. Proudfoot, Sarah Sonnett
Figure caption: Stages in our hypothesized evolution of Haumea. In stage 1, two similar KBOs have partially differentiated and have small rock cores and ice mantles underneath undifferentiated rock/ice. In stage 2, the bodies collide in a graze-and-merge type collision, shedding rock/ice material that is lost. In stage 3, radiogenic heating drives further differentiation, which reduces Haumea’s MOI, spinning it up. In stage 4, during the final formation of the core, the spin rate is sufficient to eject material from the long axis of Haumea, forming a disk of icy material. The loss of angular momentum slows Haumea’s spin, and in stage 5, the hydration and swelling of the core increase Haumea’s MOI and slow its spin rate further. Icy moonlets formed in the disk are lost as family members. Modern Haumea in stage 6 retains two large moons and a thin ring and is characterized by an ice mantle overlying a large rocky core of mostly hydrated silicate. Image credit: Sue Selkirk, ASU.
Paper: Let It Go: Geophysically Driven Ejection of the Haumea Family Members
Authors: Jessica L. Noviello, Steven J. Desch, Marc Neveu, Benjamin C. N. Proudfoot, Sarah Sonnett
Figure caption: Thermal and geophysical evolution of a spherical object with a mass and bulk density close to Haumea’s. Temperature (left; in K), interior structure (middle; gray = undifferentiated, sky blue = ice, dark blue = liquid water, brown = rock), and density (right; in kg m−3) are shown as a function of radius and time. Differentiation and hydration take place largely sequentially in the first 100 Myr postimpact.
Paper: Let It Go: Geophysically Driven Ejection of the Haumea Family Members
Authors: Jessica L. Noviello, Steven J. Desch, Marc Neveu, Benjamin C. N. Proudfoot, Sarah Sonnett
Figure caption: Variation with assumed mantle density ρ m of various outputs calculated using the kyushu code. Generally, the increase in mantle density corresponds to an increase in core density ρ c and a decrease in the core size, as well as an increase in the overall ice fraction.
Paper: Let It Go: Geophysically Driven Ejection of the Haumea Family Members
Authors: Jessica L. Noviello, Steven J. Desch, Marc Neveu, Benjamin C. N. Proudfoot, Sarah Sonnett
Figure caption: Variation with assumed mantle density ρ m of calculated semiaxis c, average density ρ avg, and core density ρ c for the case of modern-day Haumea.
Paper: Let It Go: Geophysically Driven Ejection of the Haumea Family Members
Authors: Jessica L. Noviello, Steven J. Desch, Marc Neveu, Benjamin C. N. Proudfoot, Sarah Sonnett
Figure caption: Calculated volume and density of cores for pre- and post-fling solutions (labeled with run number), demonstrating that both the high-mass, high angular momentum pre-fling states and the modern-mass, modern angular momentum post-fling cases can share common core properties. We particularly favor case 41 for the pre-fling state and case 55 for the post-fling state.
Paper: Let It Go: Geophysically Driven Ejection of the Haumea Family Members
Authors: Jessica L. Noviello, Steven J. Desch, Marc Neveu, Benjamin C. N. Proudfoot, Sarah Sonnett
Figure caption: Length of c-axis as a function of axes a and b.
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: Plot of the equilibrium constant for H2 solubility in molten mafic silicate vs. total vapor pressure above the melt (Reaction (R15)). Crosses are the experimental results from Hirschmann et al. (2012). Solid curves show the model used in this work, in which the decrease in the equilibrium constant with pressure is attributed solely to the increase in total pressure. Dashed curves show the same model where the nonideal behavior of H2 is included based on the EOS of Chabrier et al. (2019). The horizontal line shows the equilibrium constant with no pressure dependence as assumed Kite et al. (2019). The choice of temperatures for the nonideal H2 behavior is constrained by the tables provided by Chabrier et al. (2019).
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 reactive metal. The panel on the left shows the variability of ﹩{f}_{{{\rm{O}}}_{2}}﹩ with temperature at the magma ocean–atmosphere boundary with an initial primary atmosphere comprising 4% of the body by weight. Pressures along the upper, auxiliary x-axis refer to the pressures corresponding to each temperature from the equilibrium solutions. The panel on the right shows the effect of varying the hydrogen fractions from 1% to 14% by weight at a fixed magma ocean surface temperature of 4500 K.
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: Chemical composition of an atmosphere equilibrated with the magma ocean for a 4 M ⊕ planet with reactive metal. The panel on the left shows the variability in wt% with temperature at the magma ocean–atmosphere boundary with an initial primary atmosphere comprising 4% of the body by weight. Pressures along the upper, auxiliary x-axis refer to the pressures corresponding to each temperature from the equilibrium solutions. The panel on the right shows the effect of varying the hydrogen fractions from 1% to 14% by weight at a fixed magma ocean surface temperature of 4500 K.
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 mass fractions of atmosphere, silicate, and metal for a 4 M ⊕ planet with reactive metal. The panel on the left shows the variability of mass fractions with temperature at the magma ocean–atmosphere boundary with an initial primary atmosphere comprising 4% of the body by weight. Pressures along the upper, auxiliary x-axis refer to the pressures corresponding to each temperature from the equilibrium solutions. The panel on the right shows the effect of varying the hydrogen fractions from 1% to 14% by weight at a fixed magma ocean surface temperature of 4500 K. Here the pressure varies at the constant magma ocean surface temperature of 4500 K.
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: Simplified depiction of the net reactions comprising the hydrogen cycle for a planet with an H2-rich primary atmosphere in the reactive core model. Redox chemistry leads to water formation in the atmosphere and light elements in the metal core. Here Fe, H, O, and Si refer to the elements in the metal phase.
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: Chemical composition of the silicate magma ocean equilibrated with the atmosphere for a 4 M ⊕ planet with reactive metal. The panel on the left shows the variability in wt% with temperature at the magma ocean–atmosphere boundary with an initial primary atmosphere comprising 4% of the body by weight. Pressures along the upper, auxiliary x-axis refer to the pressures corresponding to each temperature from the equilibrium solutions. The panel on the right shows the effect of varying the hydrogen fractions from 1% to 14% by weight at a fixed magma ocean surface temperature of 4500 K.
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: Chemical composition of the silicate magma ocean equilibrated with the atmosphere for a 4 M ⊕ planet with unreactive metal. These results are for a fixed equilibration temperature of 4500 K with the mass fraction of total H varying from 1% to 14% by weight.
Paper: Identifying Interstellar Object Impact Craters
Authors: Samuel H. C. Cabot, Gregory Laughlin
Figure caption: Two example simulations of ice projectiles impacting into a basalt target, shown to highlight similarities in transient craters under different impact conditions. The left panels correspond to a slow impact (30 km s−1) and large projectile diameter (80 m), and the right panels correspond to a fast impact (100 km s−1) and small projectile diameter (40 m). The simulated targets have identical initial target distensions (α 0) and negligible cohesive strength. The top panels depict the transient crater profiles. The reported transient radii (﹩{D}_{{tr}}/2﹩) are measured relative to the preimpact surface. The bottom panels depict the peak shock pressures experienced by tracer particles, which were embedded in the high-resolution zone. The contours are derived from the initial position tracer particles. The critical shock pressure for complete melting is P  c  = 106 GPa. Note the different abscissa and ordinate scales between the top and bottom panels.
Paper: Identifying Interstellar Object Impact Craters
Authors: Samuel H. C. Cabot, Gregory Laughlin
Figure caption: Analytic estimates of impact speed as a function of melt volume and diameter of the transient crater for six examples of target materials that are explored theoretically without dedicated simulations in this study. The panels show predictions for impacts into targets with various scaling parameterizations (representing different materials), which are listed in Table 3. Lines of constant impact velocity are drawn for 16, 30, and 100 km s−1, denoted by varying line colors. The larger the separation between these lines, the greater the difference in melt volume produced in craters of the same diameter, and hence the easier to determine projectile characteristics.
Paper: Identifying Interstellar Object Impact Craters
Authors: Samuel H. C. Cabot, Gregory Laughlin
Figure caption: Dependence of maximum pressure on simulation resolution for the nominal simulation setup in this study (ice projectile striking a cohesionless basalt target). Each panel depicts the original locations of tracer particles embedded in the high-resolution zone of the simulation, color coded by the maximum pressure they experience following the impact. The top row shows results for a 30 km s−1 impact, whereas the bottom row is for a 100 km s−1 impact. The CPPR takes values of 10, 20, 40, 60, and 80. Note that the color scales for the top and bottom rows have different maxima but the same minima at 106 GPa (Quintana et al. 2015).