adsabs/AstroCLIMB huggingface dataset:
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: Close-up of Figure 16 showing the details of the relationships between solar system rocky planets, those of Trappist-1 b, c, d, e, f, g, and h after Agol et al. (2021), compared with mass–radius relations for various density deficits due to H and O in metal cores. Curves are the same as in Figure 16. Inner solar system planets are shown for comparison. Interestingly, the various underdense Trappist-1 planets can be explained by standard core fractions when accounting for light elements in the core found in our reactive core models. Our results, therefore, may offer an alternative explanation for the lower-than-expected densities of the planets in the Trappist-1 system (e.g., Agol et al. 2021).
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: Distribution of H in an equilibrated 4 M ⊕ planet. The panel on the left shows the variability in the fraction of H in each reservoir as a function of 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 H fraction refers to the fraction of total H present in each of the reservoirs.
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: Deficit in uncompressed density, ρ 0, for a 4 M ⊕ planet as a function of temperature of equilibration and total H. The panel on the left shows the variability in ρ 0 as a function of 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: Mole fractions of species in the atmosphere as a function of magma ocean–atmosphere boundary temperature with an initial H2-rich primary atmosphere comprising 4% of the body by weight. These results are for the reactive metal scenario. 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: The wt% elements in metal for the reactive core model for a 4 M ⊕ planet. 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 an atmosphere equilibrated with the magma ocean for a 4 M ⊕ planet with no reactive metal as a function of magma ocean surface pressure. Each pressure represents a different total mass fraction of hydrogen, ranging from 1% to 14% 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: Distribution of H in an equilibrated 4 M ⊕ planet with unreactive metal as a function of varying the hydrogen fractions from 1% to 14% by weight at a fixed magma ocean surface temperature of 4500 K. Here the H fraction refers to the fraction of total H present in each of the reservoirs.
Paper: Simulation of Freezing Cryomagma Reservoirs in Viscoelastic Ice Shells
Authors: Elodie Lesage, Hélène Massol, Samuel M. Howell, Frédéric Schmidt
Figure caption: Critical freezing time necessary to trigger an eruption from a reservoir filled with ((a), (c), and (e)) pure liquid water and ((b), (d), and (f)) a mixture of liquid water and salts. The following situations are represented. (a) and (b) The reservoir wall does not deform during freezing (nondeformable wall approximation as in Lesage et al. 2020). The dark blue area represents reservoirs that are too large to be stored in a 10 km thick conductive ice crust. (c) and (d) The reservoir wall deformation is taken into account using the algorithm described in Section 2.5. The algorithm diverges for the reservoirs in the dark blue area; these reservoirs accommodate the overpressure by deformation and cannot trigger eruptions. (e) and (f) We take into account the wall deformation as in panels (c) and (d), but we add a filter using the Maxwell time criterion: the reservoirs for which τ M < τ  c  cannot trigger eruptions (dark blue area). The white dashed line corresponds to the limit between the elastic and viscoelastic reservoirs (Maxwell time criterion) in panels (e) and (f). This line is reported in panels (c) and (d) to show the similarity with the reservoirs for which the algorithm converges (eruption possible) or diverges (overpressure accommodated by deformation).
Paper: Simulation of Freezing Cryomagma Reservoirs in Viscoelastic Ice Shells
Authors: Elodie Lesage, Hélène Massol, Samuel M. Howell, Frédéric Schmidt
Figure caption: Review of the mechanisms proposed in the literature to explain the emplacement of liquid reservoirs invoked to correspond to a variety of geological features at Europa’s surface. Tidally activated strike-slip faults may produce local partial melting and draining, as modeled by Kalousová et al. (2016) and Hammond (2020). Meteorite impacts may generate melted brine that, after percolating, can form shallow lenses per Steinbrügge et al. (2020). Double ridges may form by freezing of shallow liquid water intrusions as modeled by Johnston & Montési (2014) and recently observed in Greenland (Culberg et al. 2022). A wide range of features, such as chaos (Schmidt et al. 2011), microchaos, lenticulae, pits and domes (Manga & Michaut 2017), and smooth plains (Lesage et al. 2021), may be morphologically explained by the presence of water sills or elongated reservoirs in the shallow subsurface. Craft et al. (2016) demonstrated that horizontal sills can propagate in the ice shell (this study is applied to the formation of double ridges but is not represented here for simplicity of the figure), but this mechanism is challenging. Connection between the sills and the subsurface ocean is unlikely, as demonstrated by Walker et al. (2021). Finally, deep in situ partial melting on top of convective ice plumes has been modeled in several studies, e.g., Vilella et al. (2020) and references therein. We indicate with a dashed line the elastic–viscoelastic transition determined by comparing the ice Maxwell time, τ M, and the reservoir critical freezing time, τ  c , assuming that all reservoirs represented have an identical critical freezing time. The figure is not to scale.
Paper: Simulation of Freezing Cryomagma Reservoirs in Viscoelastic Ice Shells
Authors: Elodie Lesage, Hélène Massol, Samuel M. Howell, Frédéric Schmidt
Figure caption: Volume of the first eruption of a reservoir filled with ((a), (c), and (e)) pure liquid water or ((b), (d), and (f)) a mixture of liquid water and salts. See caption of Figure 10 for the three different cases represented.
Paper: Simulation of Freezing Cryomagma Reservoirs in Viscoelastic Ice Shells
Authors: Elodie Lesage, Hélène Massol, Samuel M. Howell, Frédéric Schmidt
Figure caption: Critical freezing time before eruption of a 500 m radius reservoir as a function of its depth in the nondeformable wall approximation (gray line) and with the wall deformation (black line). Two cryomagma compositions are modeled: (a) pure liquid water and (b) a briny cryomagma (81 wt% H2O + 16 wt% MgSO4 + 3 wt% Na2SO4).
Paper: Simulation of Freezing Cryomagma Reservoirs in Viscoelastic Ice Shells
Authors: Elodie Lesage, Hélène Massol, Samuel M. Howell, Frédéric Schmidt
Figure caption: Critical freezing time and erupted volume for an ellipsoidal reservoir filled with pure water. The aspect ratio of the reservoir is 500 (a = b = 500c).
Paper: Atmospheric Overturning Circulation on Dry, Tidally Locked Rocky Planets Is Mainly Driven by Radiative Cooling
Authors: Shuang Wang, Jun Yang
Figure caption: (a) Temperature, (b) potential temperature, (c) vertical velocity in pressure coordinates, (d) heating rate from longwave radiation, (e) turbulent thermal diffusion, (f) vertical thermal advection, (g) horizontal thermal advection, (h) mass stream function (color shading) and zonal-mean zonal winds (contour lines, interval is 2 m s−1), and (i) the acceleration on the zonal winds caused by wave activities. CO2 concentrations are 10−6, 10−5, 10−4, 10−3, 10−2, 10−1, and 1 ppmv (from left to right). The black line in (a) and (e) represents the height of the planetary boundary layer. Panels (a) to (g) are shown in tidally locked coordinates and are averaged over tidally locked longitude, AP is the antistellar point, and SP is the substellar point; panels (h) and (i) are in standard coordinates.
Paper: Atmospheric Overturning Circulation on Dry, Tidally Locked Rocky Planets Is Mainly Driven by Radiative Cooling
Authors: Shuang Wang, Jun Yang
Figure caption: Zonal-mean zonal winds (left) and wave activities (right) in the CAM3 experiments of pure N2 (a)–(b) and N2+CO2 (c)–(d). In (b) and (d), color shading is the convergence of eddy momentum flux and vectors are the E-P flux. Note that the arrow scales are different between (b) and (d). These panels are shown in standard coordinates, latitude–pressure.
Paper: Atmospheric Overturning Circulation on Dry, Tidally Locked Rocky Planets Is Mainly Driven by Radiative Cooling
Authors: Shuang Wang, Jun Yang
Figure caption: Spatial distributions of CO2 concentration (a)–(h) and corresponding surface temperature (i)–(p) in regionally prescribed CO2 experiments. CO2 concentration is 100 ppmv in the region filled with oblique lines and zero in the white region. The ranges of filled regions in (b)–(d) are 10°, 20°, and 30° of longitudes and latitudes around the substellar point. In the opposite, the nonfilled regions in (f)–(h) are 10°, 20°, and 30° of longitudes and latitudes around the substellar point. Panel (i) is the surface temperature without any CO2, and panels (j)–(p) are the differences of the surface temperature from that in panel (i) for the experiments of (b)–(h), respectively. The four panels of the leftmost column are the same as the control experiments shown in Section 3.1.
Paper: Atmospheric Overturning Circulation on Dry, Tidally Locked Rocky Planets Is Mainly Driven by Radiative Cooling
Authors: Shuang Wang, Jun Yang
Figure caption: The abrupt transition experiment from a pure N2 atmosphere to a N2+CO2 atmosphere. Time series of (a) CO2 concentration, (b) surface temperature, (c) vertically integrated mass-weighted air temperature, (d) the strength of mass stream function, (e) vertical velocity in pressure coordinates at the substellar point, and (f) zonal-mean zonal wind at the equator. Solid and dashed lines in (b) and (c) represent the dayside mean and nightside mean, respectively. CO2 of 100 ppmv is added to the atmosphere on Day 0.
Paper: Atmospheric Overturning Circulation on Dry, Tidally Locked Rocky Planets Is Mainly Driven by Radiative Cooling
Authors: Shuang Wang, Jun Yang
Figure caption: Vertical profiles of heating rates in the CAM3 experiments of pure N2 (a)–(d) and N2+CO2 (e)–(h). (a) and (e) global mean; (b) and (f) nightside mean; (c) and (g) dayside mean; (d) and (h) substellar region. Blue: heating rate from longwave radiation (Q LW); red: turbulent thermal diffusion (Q  D ); solid green: vertical advection (adv v ); dashed green: horizontal advection (adv h ); and black: the sum.
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) for pure N2 (upper row) and N2+CO2 (lower row). The stellar fluxes at the substellar point are 1400, 1600, 1800, 2000, and 3000 W m−2 (from left to right). The global-mean surface temperature of each simulation is shown at the top-left corner. The coordinates are the same as those in Figure 4.
Paper: Atmospheric Overturning Circulation on Dry, Tidally Locked Rocky Planets Is Mainly Driven by Radiative Cooling
Authors: Shuang Wang, Jun Yang
Figure caption: Horizontal wave patterns at 300 hPa (a)–(b), 500 hPa (c)–(d), and 850 hPa (e)–(f) in the CAM3 experiments. Left and right columns are for pure N2 and N2+CO2, respectively. The black dot represents the substellar point. Color shading is the sum of longwave radiative and diffusion heating rates (K day−1). Vectors are the horizontal winds (m s−1). Contour lines are the geopotential height (m), and the intervals are 1 and 20 m for the left and right columns, respectively. The blue contour lines represent the geopotential height in low-pressure Rossby lobes.
Paper: Atmospheric Overturning Circulation on Dry, Tidally Locked Rocky Planets Is Mainly Driven by Radiative Cooling
Authors: Shuang Wang, Jun Yang
Figure caption: Surface temperature and zonal equatorial atmosphere circulations for modern Earth, simulated by a coupled atmosphere-ocean model CESM Lan et al. (2022). (a) Tropical surface air temperature. (b) Winds (vectors) and total heating rate (color shading). The vertical components of vectors are magnified by 200 times for clearly showing the overturning structure. (c) Shortwave heating rate, (d) longwave heating rate, (e) heating rate associated with convection process, and (f) turbulent thermal diffusion. All quantities in panels (b)–(f) are weighted averages between 5°S and 5°N.
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) and mass stream functions (contour lines, 1010 kg s−1) in regionally prescribed CO2 experiments. Distributions of CO2 concentration for (a)–(h) correspond to those in Figures 11(a)–(h), respectively. The coordinates are same as those in Figure 4.
Paper: Identifying Interstellar Object Impact Craters
Authors: Samuel H. C. Cabot, Gregory Laughlin
Figure caption: Dimensionless scaling parameter outcomes for the iSALE simulations. Results for gravity-dominated craters are shown in the top panel, whereas those for strength-dominated craters are in the bottom panel. Colors denote three different target porosities, and the sizes of the data points are proportional to the projectile diameter. The best-fit power-law equations are denoted in the top right corner of each panel.
Paper: Identifying Interstellar Object Impact Craters
Authors: Samuel H. C. Cabot, Gregory Laughlin
Figure caption: Toomre diagram for Gaia EDR3 stars within 200 pc of the Sun, which have full phase-space measurements. The origin represents the rest frame of the Sun. Values have been normalized to depict the encounter rate of ISOs within 1 au of the Sun. Curves correspond to, from innermost to outermost, constant encounter speeds of 50, 100, 150, 200, and 300 km s−1. Labels indicate the summed encounter rate of all ISOs with velocities enclosed by the curve.
Paper: Chemical Fractionation Modeling of Plumes Indicates a Gas-rich, Moderately Alkaline Enceladus Ocean
Authors: Lucas M. Fifer, David C. Catling, Jonathan D. Toner
Figure caption: Model predictions for dissolved concentrations of NH3 (horizontal axis) and CO2 (vertical axis). The flat-color regions (dark blue, cyan, orange) show the range of oceanic dissolved gas predictions for each outgassing model (thin-film exsolution, boiling-dominated exsolution, and droplet degassing, respectively). For each model, the full range of predictions includes uncertainty from both the range of fissure geometries that reproduce observed eruption rates of 180–338 kg s−1 (Hansen et al. 2017, 2020) and produce fissure outlet temperatures ≤220 K, and uncertainty in the plume measurements of gas mixing ratios (Waite et al. 2017; see Table 1). Generally the extent of each of the three regions from upper left to lower right corresponds to uncertainty in the plume mixing ratios, while the extent from lower left to upper right corresponds to uncertainty from the range of fissure geometries that match observations (both directions are indicated with labeled black arrows). The striped green region indicates the combination of CO2 and NH3 concentrations that are reconcilable with CDA measurements of salts; that is, [NaCl] = 0.05–0.2 molal, [Na2CO3 or NaHCO3] = 0.01–0.1 molal (Postberg et al. 2009), and all ion concentrations ≤0.2 molal. The region of overlap between the striped green region and any of the other regions shows the range of predictions for a given outgassing model that is compatible with CDA measurements. The thin-film exsolution model produces the largest range in possible oceanic concentrations, the boiling-dominated exsolution model has a smaller range with similar upper limits, and the droplet degassing model does not produce any chemistries that are reconcilable with CDA measurements.
Paper: Chemical Fractionation Modeling of Plumes Indicates a Gas-rich, Moderately Alkaline Enceladus Ocean
Authors: Lucas M. Fifer, David C. Catling, Jonathan D. Toner
Figure caption: Predicted gas and ion concentrations from this work, using the thin-film model of exsolution (shown with dark blue error bars) and the boiling-dominated model of exsolution (cyan error bars) compared to previous studies. The two estimates from this work are shown as solid error bars for limits that are consistent with CDA analysis of salt content, while the dashed parts of the error bars are not consistent due to ion concentrations greater than 0.2 molal. Marion et al. (2012; green dots) assumed no fractionation between the plume and ocean. Waite et al. (2017; orange error bars) assumed a pH range of 9–11 based on prior studies, and found a CO2 concentration that was consistent with that pH. They then used gas-to-gas ratios in the plume to find gas-to-gas ratios in the ocean. Glein et al. (2015; gray error bars) accounted for water vapor loss during condensation for a plume that stays in vapor pressure equilibrium with fissure walls that cool toward the surface. Glein & Waite (2020; red error bar) later reported an updated range for oceanic CO2 using the same model of condensation as Glein et al. (2015) and additionally incorporating limits based on CDA measurements of salts. The open purple circles show the lowest concentration at which each gas would spontaneously form bubbles, as in a carbonated drink (Liger-Belair 2012). A limit for bubble nucleation that is below the estimates for gas concentration (seen for H2) suggests that H2 bubbles are likely forming in the near-surface ocean. NH3 bubbles will not form because the required limit for bubble nucleation is far above the estimated oceanic concentrations.
Paper: Chemical Fractionation Modeling of Plumes Indicates a Gas-rich, Moderately Alkaline Enceladus Ocean
Authors: Lucas M. Fifer, David C. Catling, Jonathan D. Toner
Figure caption: A subset of our modeling results to show the effect of fissure geometry on condensation. Top row: the fraction of plume vapor loss (a model output, defined in Equation (9)) that occurs due to condensation for different fissure geometries (model inputs), varying (a) fissure width at the ocean–plume interface, (b) fissure width at the plume outlet, (c) the tapering factor Y (see Equation (6)), and (d) the depth of the fissure from outlet to ocean–plume interface. Bottom row: the temperature of the ice walls at the fissure outlet (a model output) for different fissure geometries varying (e) fissure width at the ocean–plume interface, (f) fissure width at the plume outlet, (g) the tapering factor Y, and (h) the depth of the fissure from outlet to ocean–plume interface. In all subplots shown here, the fissure’s geometrical parameters are held constant at the following values unless varied on the x-axis: δ 0 = 50 m, δ outlet = 0.07 m, Y = 55 m, D = 4500 m. Blue points indicate unrestricted model results, points with black “×”s are models that reproduce observed eruption rates of 180–338 kg s−1 (Hansen et al. 2017, 2020), and models with black “+”s produce fissure outlet temperatures ≤220 K (the gray dashed line in the bottom row also indicates this temperature limit). Only fissures that fit both restrictions (points with “×” and “+”, also indicated by the shaded region) are deemed viable. Fissures that are narrower at the outlet or deeper overall result in a larger fraction of the plume’s water vapor being removed ((b) and (d)), and thus will produce larger differences between relative gas abundances in the plume at the bottom of the conduit versus at the top (at Enceladus’ surface). Fissures that are narrower at the ocean interface or have a smaller tapering factor Y also tend to lose more water vapor ((a) and (c)), but the effect is less pronounced. Across all plots, T outlet is anticorrelated with the fraction of water vapor lost, because the final vapor pressure of the plume is tied directly to the temperature of the ice wall at the outlet (Equation (4)).
Paper: Chemical Fractionation Modeling of Plumes Indicates a Gas-rich, Moderately Alkaline Enceladus Ocean
Authors: Lucas M. Fifer, David C. Catling, Jonathan D. Toner
Figure caption: (a) A diagram showing the ocean source to Enceladus’ plumes, and two key fractionation processes. In the lower-right circle, water evaporation and gas exsolution occur at different rates, enriching the plume in water vapor and those gases that exsolve rapidly. The vapor pressure of the liquid (p  ℓ ) is larger than the partial pressure of water vapor directly above the ocean (p 0), driving evaporation (Nakajima & Ingersoll 2016). Solid ice grains in the plume are formed via freezing of aerosol-like droplets of water, and carried in the plume gas (Postberg et al. 2009). In the upper-right circle, water vapor condenses out of the plumes onto the walls of the ice fissures, whereas other gases do not condense out significantly (Glein et al. 2015). (b) Diagrams of the modeled fissure geometries, with depth D measured from the surface to the ocean—plume boundary, fissure length L, and either constant diameter δ or a tapering diameter starting from δ 0 at the ocean and narrowing to δ outlet at the plume outlet (see Equation (6)).