adsabs/AstroCLIMB huggingface dataset:
Paper: Spectrophotometry of Selected Regions of Europa—Revisiting Galileo NIMS Data
Authors: Ines Belgacem, Thomas Cornet, Bonnie Buratti, François Andrieu, Guillaume Cruz Mermy, Frédéric Schmidt, Ishan Mishra
Figure caption: Variation of the macroscopic roughness ﹩\bar{\theta }﹩ vs. the single-scattering albedo ω for ROI # 3.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Spectrophotometry of Selected Regions of Europa—Revisiting Galileo NIMS Data
Authors: Ines Belgacem, Thomas Cornet, Bonnie Buratti, François Andrieu, Guillaume Cruz Mermy, Frédéric Schmidt, Ishan Mishra
Figure caption: Retrieved values of the macroscopic roughness ﹩\bar{\theta }﹩ for a range of wavelengths for ROI #3. (The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Spectrophotometry of Selected Regions of Europa—Revisiting Galileo NIMS Data
Authors: Ines Belgacem, Thomas Cornet, Bonnie Buratti, François Andrieu, Guillaume Cruz Mermy, Frédéric Schmidt, Ishan Mishra
Figure caption: Retrieved values of the single-scattering albedo ω for a range of wavelengths for ROI #3.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Spectrophotometry of Selected Regions of Europa—Revisiting Galileo NIMS Data
Authors: Ines Belgacem, Thomas Cornet, Bonnie Buratti, François Andrieu, Guillaume Cruz Mermy, Frédéric Schmidt, Ishan Mishra
Figure caption: Detailed phase coverage for every 40 nm wavelength interval in ROI #3. In particular, it is clear that the coverage is not equivalent for all wavelengths and that this is directly impacting the constraints we can derive for the different photometric parameters in the model.
Paper: Spectrophotometry of Selected Regions of Europa—Revisiting Galileo NIMS Data
Authors: Ines Belgacem, Thomas Cornet, Bonnie Buratti, François Andrieu, Guillaume Cruz Mermy, Frédéric Schmidt, Ishan Mishra
Figure caption: Detailed phase coverage for every 40 nm wavelength interval in ROI #2. In particular, it is clear that the coverage is not equivalent for all wavelengths and that this is directly impacting the constraints we can derive for the different photometric parameters in the model.
Paper: Multiple Giant Impacts and Chemical Equilibria: An Integrated Approach to Rocky Planet Formation
Authors: Haruya Maeda, Takanori Sasaki
Figure caption: (a) Initial semimajor axes and masses of protoplanets and (b) their random distribution in the azimuthal direction, with arrows showing the velocity vectors. Yellow, blue, and red lines indicate the orbital radii of Mercury, Earth, and Mars, respectively. Error bars show the extent of solid material accumulation for each protoplanet, spanning ±4 rHill.
Paper: Multiple Giant Impacts and Chemical Equilibria: An Integrated Approach to Rocky Planet Formation
Authors: Haruya Maeda, Takanori Sasaki
Figure caption: Relationship between the initial amount of hydrogen atmosphere and the core density deficit. The dashed line shows the results after re-equilibration: hydrogen is artificially removed from the atmosphere after the initial equilibrium calculation, and equilibrium is recalculated. An 8% density deficit (orange line) corresponds to the present-day Earth. As the initial hydrogen content increases, more hydrogen enters the core, but this effect saturates. Re-equilibration returns some hydrogen from the core back to the atmosphere. Our first equilibrium calculations follow E. D. Young et al. (2023), although they explored only a narrow range of initial hydrogen mass fractions (near 0.2 wt%).
Paper: Multiple Giant Impacts and Chemical Equilibria: An Integrated Approach to Rocky Planet Formation
Authors: Haruya Maeda, Takanori Sasaki
Figure caption: Orbital evolution of protoplanets over the full simulation time. Colored circles indicate protoplanets immediately after experiencing giant impacts and mergers. Blue circles correspond to protoplanets with mass less than 0.2 M⊕, and orange ones correspond protoplanets with mass of 0.2 M⊕ or more. (a) Case No.6, (b) case No.7, (c) case No.11, and (d) case No.12 in Table 2. The system rapidly becomes unstable, triggering initial giant impacts. Although about half of the giant impacts occur within the first million years, additional impacts continue to occur later, even beyond 107 yr.
Paper: Multiple Giant Impacts and Chemical Equilibria: An Integrated Approach to Rocky Planet Formation
Authors: Haruya Maeda, Takanori Sasaki
Figure caption: Evolution of chemical compositions of some planets. These results correspond to an atmospheric mass of Mtorus. We show the evolution of (a) a third planet in case No.6 and (b) a second planet in case No.12 at tend. The horizontal axis represents time, and each point corresponds to a protoplanet immediately after a giant impact, with the symbol area proportional to its mass. Here 7.5%–10.0% of the core density deficit and 0.023 wt% of the water content represent the current Earth’s value. For water content, we assume that one to three ocean masses can reproduce the current surface ocean. Protoplanets incorporate a large amount of hydrogen into their cores during initial giant impacts (t ≲ 106 yr). These protoplanets have too large a core density deficit to reproduce the current Earth. However, through late giant impacts (after gas dissipation), collisions between hydrogen-rich and hydrogen-poor protoplanets can yield final planets with moderate core density deficits similar to Earth.
Paper: Multiple Giant Impacts and Chemical Equilibria: An Integrated Approach to Rocky Planet Formation
Authors: Haruya Maeda, Takanori Sasaki
Figure caption: A distribution of (a) planetary masses and (b) eccentricities for the remaining planets at tend in all calculations. The open circles are the result of our calculations, and the filled black ones are current rocky planets in the solar system. The filled orange circles for eccentricity represent planets with a mass of 0.2 M⊕ or more. Error bars represent perihelion and aphelion. The solid line and dashed lines represent mean and standard deviation values of the common logarithm of eccentricity for planets with a mass of 0.2 M⊕ or more. The distributions of the finally formed planets roughly cover the current semimajor axis, mass, and eccentricity distributions of the rocky planets in the solar system.
Paper: Multiple Giant Impacts and Chemical Equilibria: An Integrated Approach to Rocky Planet Formation
Authors: Haruya Maeda, Takanori Sasaki
Figure caption: Process flow diagram of our calculations. Initially, 21 protoplanets collide and merge due to mutual gravitational interactions, ultimately forming four rocky planets analogous to Mercury, Venus, Earth, and Mars. Meanwhile, the protoplanetary disk gas dissipates exponentially with time. Depending on disk conditions and the mass threshold for atmospheric capture, giant impacts repeatedly melt the mantle, triggering chemical equilibria. We perform equilibrium calculations at each giant impact event to update the protoplanet’s composition accordingly.
Paper: Multiple Giant Impacts and Chemical Equilibria: An Integrated Approach to Rocky Planet Formation
Authors: Haruya Maeda, Takanori Sasaki
Figure caption: A distribution of (a) planetary masses and (b) eccentricities for the remaining protoplanets at t = 1.6 × 106 yr in all calculations. The filled circles in orange represent protoplanets with a mass of 0.2 M⊕ or more. These protoplanets are assumed to acquire a hydrogen-rich atmosphere and incorporate it in their interior. Hydrogen-rich protoplanets are distributed evenly relative to the total distribution.
Paper: Multiple Giant Impacts and Chemical Equilibria: An Integrated Approach to Rocky Planet Formation
Authors: Haruya Maeda, Takanori Sasaki
Figure caption: Key reactions that produce Earth’s current environment. (1) Silicates decompose in the magma ocean and release oxygen, which combines with atmospheric hydrogen to form water. (2) Hydrogen migrates from the atmosphere through the mantle into the core, decreasing the core density. (3) Silicate-derived oxygen oxidizes iron in the core, creating an overall more oxidized planet.
Paper: Multiple Giant Impacts and Chemical Equilibria: An Integrated Approach to Rocky Planet Formation
Authors: Haruya Maeda, Takanori Sasaki
Figure caption: Chemical re-equilibration process. After the initial equilibrium calculation, all hydrogen in the atmosphere is artificially removed, and equilibrium is recalculated.
Paper: Multiple Giant Impacts and Chemical Equilibria: An Integrated Approach to Rocky Planet Formation
Authors: Haruya Maeda, Takanori Sasaki
Figure caption: A distribution of core density deficits and atmospheric water contents for the remaining planets at tend in all calculations. Open circles correspond to results with an atmospheric mass of Mmid, and error bars correspond to that of Mtorus and Mcylinder. Planets with masses less than 0.2 M⊕ have no core density deficit, since we conducted chemical equilibrium calculation for only that greater than 0.2 M⊕ (Assumption of atmospheric acquisition in the Method section). A core density deficit of 7.5%–10.0% represents a range consistent with the current Earth, and about 12.7% is the saturated value. Low-mass planets formed in early giant impacts acquire a large amount of disk gas and get a high core density deficit. As the planetary mass increases due to subsequent giant impacts, the core density deficit decreases and approaches a value consistent with that of the current Earth. As with the core density deficit, water content also decreases as planetary mass increases.
Paper: Multiple Giant Impacts and Chemical Equilibria: An Integrated Approach to Rocky Planet Formation
Authors: Haruya Maeda, Takanori Sasaki
Figure caption: Orbital evolution of protoplanets and changes in core density deficit and water content in atmospheres for case (a) No.6, (b) No.7, (c) No.11, and (d) No.12 (see Table 2). We show results with an atmospheric mass of Mmid. Early giant impacts in the inner region do not lead to atmospheric acquisition because the merged mass remains below the threshold for atmospheric capture (Mproto = 0.2 M⊕). Even in the presence of inclination, the core density deficit evolves in a multistage manner. As cases where planets with a value close to the Earth’s core density deficit were obtained, a planet with a final mass of 0.871 M⊕ and a core density deficit of 8.68% forms at a final orbit of 1.085 au (third planet in No.6), and a planet with a final mass of 0.795 M⊕ and a core density deficit of 7.95% forms at a final orbit of 0.887 au (second planet in No.12).
Paper: Multiple Giant Impacts and Chemical Equilibria: An Integrated Approach to Rocky Planet Formation
Authors: Haruya Maeda, Takanori Sasaki
Figure caption: Orbital evolution of the protoplanets for (a) 0 Myr ≤ t ≤ 1.0 Myr and (b) 1.0 Myr ≤ t ≤ 100 Myr, assuming ﹩{{\rm{\Sigma }}}_{{\rm{gas}}}(0)=0.01\,{{\rm{\Sigma }}}_{{\rm{gas}}}^{{\rm{\min }}}﹩ and τdiss = 106 yr. The black dots represent the semimajor axis, while the blue and red lines indicate perihelion and aphelion distances, respectively. Giant impacts cluster at t ≃ 0.1 Myr (first stage) and t ≃ 20 Myr (second stage).
Paper: Multiple Giant Impacts and Chemical Equilibria: An Integrated Approach to Rocky Planet Formation
Authors: Haruya Maeda, Takanori Sasaki
Figure caption: Initial H2 mass fraction and (a) core density deficit and (b) water content, comparing cases where all hydrogen is supplied at once vs. supplied incrementally. For example, to model a 0.5 wt% hydrogen atmosphere, five equilibrium calculations were performed, each adding 0.1 wt% hydrogen (0.1 + 0.1 + 0.1 + 0.1 + 0.1 = 0.5). The incremental addition better reflects the physical constraints on atmosphere retention. Nevertheless, the differences between the two approaches are minor.
Paper: Multiple Giant Impacts and Chemical Equilibria: An Integrated Approach to Rocky Planet Formation
Authors: Haruya Maeda, Takanori Sasaki
Figure caption: A distribution of core density deficit for semimajor axis and planetary mass. The core density deficit is the result with an atmospheric mass of Mmid. As the planetary mass increases, the core density deficit tends to decrease. On the other hand, there seems to be no apparent correlation between semimajor axis and core density deficit.
Paper: Multiple Giant Impacts and Chemical Equilibria: An Integrated Approach to Rocky Planet Formation
Authors: Haruya Maeda, Takanori Sasaki
Figure caption: Orbital evolution of the protoplanets for two additional runs using the same parameters as Figure 15 but with different random initial placements of protoplanets. (a) and (b) show the system’s evolution for t ≤ 1 Myr and 1 Myr ≤ t ≤ 100 Myr, respectively. Random differences in initial azimuthal positions affect the timing and extent of the second giant impact stage.
Paper: Multiple Giant Impacts and Chemical Equilibria: An Integrated Approach to Rocky Planet Formation
Authors: Haruya Maeda, Takanori Sasaki
Figure caption: Initial H2 mass fraction and (a) core density deficit and (b) water content as a function of protoplanet mass. Increasing protoplanet mass results in higher surface pressure, leading to greater hydrogen dissolution into the interior and less water production per unit mass. This calculation modifies only the protoplanet mass Mproto (and the corresponding initial H2 mass fraction range) relative to the models of E. D. Young et al. (2023).
Paper: Multiple Giant Impacts and Chemical Equilibria: An Integrated Approach to Rocky Planet Formation
Authors: Haruya Maeda, Takanori Sasaki
Figure caption: Orbital evolution of the protoplanets and changes in core density deficit and water content for ﹩{{\rm{\Sigma }}}_{{\rm{gas}}}(0)=0.01\,{{\rm{\Sigma }}}_{{\rm{gas}}}^{{\rm{\min }}}﹩ and τdiss = 106 yr. Circle colors denote the protoplanets’ core density deficits and water contents. Initially, several protoplanets gain excess hydrogen in their cores (first giant impact stage), but subsequent collisions can moderate the core density deficit.
Paper: Multiple Giant Impacts and Chemical Equilibria: An Integrated Approach to Rocky Planet Formation
Authors: Haruya Maeda, Takanori Sasaki
Figure caption: (a) Number of protoplanets and hydrogen-rich-core protoplanets remaining after the first giant impact stage (0.7–1.3 au). (b) Total mass of hydrogen-rich-core protoplanets, also 0.7–1.3 au. The final number of protoplanets is almost independent of the initial gas surface density, suggesting that as long as the disk is sufficiently dense for collisions, the overall dynamical evolution—and hence the giant impact sequence—remains similar.
Paper: Modeling Low-temperature Plasmas Simulating Titan’s Atmosphere
Authors: David Dubois, Alexander W. Raymond, Ella Sciamma-O'Brien, Farid Salama
Figure caption: (a) Cross-section schematic view of the THS plasma channel (not to scale). The pathway along which reactions are calculated by the model in the plasma channel is indicated in blue. The temperature inside the plasma cavity is on the order of T = 150 K (L. Biennier et al. 2006a; E. Sciamma-O’Brien et al. 2014). (b) Top-view cross-section schematic view of the plasma cavity (not to scale) indicating the dominant collisional processes occurring in the plasma and controlling the formation of the first building blocks leading to larger products, illustrated in the case of a N2–CH4-based atmosphere relevant to Titan. (c) Simplified schematic representation of CO-PRISM. Each simulation is controlled by the initial precursor gas composition (blue triangle). Green boxes correspond to the chemical input parameters (list of species, molecular reactions, and surface reactions), purple ellipses correspond to plasma physics and grid geometry parameters, and outputs are represented with red triangles. The model parameters that were updated and modified in the study presented here are circled in orange. Synthetic mass spectra can then be retrieved from the computed mole fractions.
Paper: Modeling Low-temperature Plasmas Simulating Titan’s Atmosphere
Authors: David Dubois, Alexander W. Raymond, Ella Sciamma-O'Brien, Farid Salama
Figure caption: Comparison of the original calculated and experimental mass spectra (in red diamonds from A. W. Raymond et al. 2018 and yellow bars from E. Sciamma-O’Brien et al. 2014, respectively) with newly calculated mass spectra (in blue circles; this study) in N2–CH4 (90%:10%), N2–CH4–C2H2 (85%:10%:5%), and N2–CH4–C2H4 (85%:10%:5%) gas mixtures. Intensities are normalized over the intensity at m/z 16, and all measurements and calculations were performed with a −800 V cathode potential.
Paper: Modeling Low-temperature Plasmas Simulating Titan’s Atmosphere
Authors: David Dubois, Alexander W. Raymond, Ella Sciamma-O'Brien, Farid Salama
Figure caption: (a) Electron density profiles calculated along the plasma channel in seven different mixing ratio conditions. The origin coordinate, x = 0 mm, starts at the anode (see Figure 1). The inset shows a zoom on the lower five similar curves. (b) Electron density profiles near the anode and near the cathode calculated as a function of time during one plasma pulse, showing that the electron density steady-state conditions are reached around 0.25 μs. Phase I near breakdown shows the migration of electrons toward the anode in the first 0.1 μs. Phase II starts once a maximum density of ∼1.5 × 1019 is reached with a migration of electrons to the cathode until steady-state conditions are reached around 0.25 μs (phase III).
Paper: Modeling Low-temperature Plasmas Simulating Titan’s Atmosphere
Authors: David Dubois, Alexander W. Raymond, Ella Sciamma-O'Brien, Farid Salama
Figure caption: Top: mean electron energies (or temperatures) in eV calculated across the plasma channel for a N2–CH4 (90:10) plasma discharge (red). The origin coordinate starts at x = 0 mm (see Figure 1). Bottom: inelastic electron collision frequency across the plasma channel calculated in steady-state conditions with a source voltage of −1000 V (black). Inelastic collisions (source term Se; see Equation (6)) lead to direct ionization and excitation of neutrals.
Paper: Modeling Low-temperature Plasmas Simulating Titan’s Atmosphere
Authors: David Dubois, Alexander W. Raymond, Ella Sciamma-O'Brien, Farid Salama
Figure caption: Mass spectra of various N2–CH4-based plasmas computed with 1% and 10% CH4 and 5% C2H2 and C2H4. Intensities are normalized to the peak at m/z = 16.
Paper: Modeling Low-temperature Plasmas Simulating Titan’s Atmosphere
Authors: David Dubois, Alexander W. Raymond, Ella Sciamma-O'Brien, Farid Salama
Figure caption: Schematic diagram showing all the model pathways leading to the production of both neutrals and cations. Each molecular species indicated here has a node whose size is proportional to the number of times this species is either lost or produced in the overall scheme. The larger the node, the more important that molecule’s contribution to the network. In blue are species participating mainly as a formed product. In gold are species participating mainly as a reactant. Species in crimson are in reactant–product equilibrium.
Paper: Modeling Low-temperature Plasmas Simulating Titan’s Atmosphere
Authors: David Dubois, Alexander W. Raymond, Ella Sciamma-O'Brien, Farid Salama
Figure caption: Mass spectra of a modeled plasma generated in a N2–CH4–C2H2 (85%:10%:5%) gas mixture with the updated version of CO-PRISM at three different locations in the plasma channel: x = 0.004 mm (blue; anode), x = 0.075 mm (green; midpoint), and x = 1.496 mm (red; cathode). Peaks are normalized by the intensity at m/z 28.
Paper: Modeling Low-temperature Plasmas Simulating Titan’s Atmosphere
Authors: David Dubois, Alexander W. Raymond, Ella Sciamma-O'Brien, Farid Salama
Figure caption: Total neutral and positive ion density profiles calculated in a N2–CH4 (90–10) gas mixture with a −1000 V source voltage.
Paper: Modeling Low-temperature Plasmas Simulating Titan’s Atmosphere
Authors: David Dubois, Alexander W. Raymond, Ella Sciamma-O'Brien, Farid Salama
Figure caption: Schematic diagram showing the model pathways only involving neutral species in neutral–neutral reactions. The interpretation of the diagram is the same as in Figure 2.
Paper: Modeling Low-temperature Plasmas Simulating Titan’s Atmosphere
Authors: David Dubois, Alexander W. Raymond, Ella Sciamma-O'Brien, Farid Salama
Figure caption: (a) Steady-state molar fraction profiles along the plasma channel of CH+, ﹩{{\rm{CH}}}_{3}^{+}﹩, ﹩{{\rm{C}}}_{2}{{\rm{H}}}_{3}^{+}﹩, and ﹩{{\rm{C}}}_{2}{{\rm{H}}}_{5}^{+}﹩ calculated in a N2–CH4 (90–10) plasma with a −1000 V voltage. The molar fractions of ﹩{{\rm{C}}}_{4}{{\rm{H}}}_{3}^{+}﹩ and ﹩{{\rm{C}}}_{5}{{\rm{H}}}_{5}^{+}﹩ were also calculated, but their values were below 10−20, which is considered to be the physical threshold. (b) Molar fraction profiles of the same molecules, including ﹩{{\rm{C}}}_{4}{{\rm{H}}}_{3}^{+}﹩ and ﹩{{\rm{C}}}_{5}{{\rm{H}}}_{5}^{+}﹩, have values above the physical threshold this time, calculated in a N2–CH4–C2H2 (85–10–5) plasma with −1000 V voltage. Values approaching a mole fraction of 10−20 represent the lower limit of what is physically possible inside the volume of the plasma cavity. Lower values close to 10−20 approach what is physically possible in terms of mole fraction; they are shown here for comparison purposes between the multiple species.
Paper: Modeling Low-temperature Plasmas Simulating Titan’s Atmosphere
Authors: David Dubois, Alexander W. Raymond, Ella Sciamma-O'Brien, Farid Salama
Figure caption: Calculated molar fractions for ﹩{{\rm{H}}}_{2}{\rm{CNCN}}﹩ (black) and ﹩{\rm{CN}}﹩ (red) in a N2–CH4–C2H2 (85–5–5) plasma with −1000 V voltage. The reaction rate of the main reaction incorporated into our model producing ﹩{{\rm{H}}}_{2}{\rm{CNCN}}﹩ is also shown (dotted blue line).
Paper: Modeling Low-temperature Plasmas Simulating Titan’s Atmosphere
Authors: David Dubois, Alexander W. Raymond, Ella Sciamma-O'Brien, Farid Salama
Figure caption: Mass spectra computed in N2:CH4:C2H6, N2:CH4:NH3, N2:CH4:HCN, and N2:CH4:CH2NH (85:10:5) plasma conditions. Intensities are normalized to the peak at m/z 16.
Paper: Modeling Low-temperature Plasmas Simulating Titan’s Atmosphere
Authors: David Dubois, Alexander W. Raymond, Ella Sciamma-O'Brien, Farid Salama
Figure caption: The 3D representations of the molar fractions of each cation and its time dependency calculated during one plasma pulse. The x-axis represents arbitrary time steps chosen from the beginning of each simulation (t = 1) until steady-state conditions are reached by t = 17. The y-axis is the channel distance along the plasma channel (in millimeters, where x = 0 mm is the anode), and the z-axis is the color-coded molar fraction.
Paper: A Novel Metric for Assessing Climatological Surface Habitability
Authors: Hannah L. Woodward, Andrew J. Rushby, Nathan J. Mayne
Figure caption: The observed and metric-derived climatological surface habitability of Earth based upon the annual mean climate across 2003–2018. The habitability criteria for each metric can be found in Table 1.
Paper: The Surfaces of Small to Midsize Plutinos: Evidence of an Association between Inclination and Surface Type
Authors: Cameron Collyer, Rosemary E. Pike, Ying-Tung Chen, 英同 陳, Mike Alexandersen, Mark Comte, Samantha M. Lawler, Bryan J. Holler, J. J. Kavelaars, Lowell Peltier
Figure caption: Left: ﹩{{ \mathcal S }}_{g\to r}﹩ and ﹩{{ \mathcal S }}_{r\to z}﹩ spectral slopes for the TNOs in the grz sample. The solid diagonal black line represents increasing spectral slopes corresponding to linear spectral reflectance through grz. Right: PC1 and PC2 projections as described in Section 4. The dashed gray lines define the two-dimensional range in which the FaintIR surface class is identified (see Section 5.2). In both panels, the TNOs observed in our Magellan Baade program are outlined with gray squares. The other TNOs are the Col-OSSOS grz subsample. In both panels, points connected by dashed red lines correspond to measurements of the same TNO at different epochs. Somnus is located above Mors in both panels.