adsabs/AstroCLIMB huggingface dataset:
Paper: Retention of Water in Terrestrial Magma Oceans and Carbon-rich Early Atmospheres
Authors: Dan J. Bower, Kaustubh Hakim, Paolo A. Sossi, Patrick Sanan
Figure caption: Atmospheric composition during magma ocean outgassing for C/H = 1 and different fO2. Columns from left to right show hydrogen (H) budgets of 1, 3, and 10 oceans, respectively. Rows from top to bottom show fO2 of ΔIW = −2, ΔIW = 0.5, ΔIW = 2, and ΔIW = 4. Magma ocean lifetime corresponds to the termination of the colored region (at ≈2% melt for fractional crystallization, between 104 and 107 yr). White dotted lines correspond to 30% melt, which indicates both the duration and atmospheric composition if instead the mantle underwent equilibrium crystallization. Initial volatile partial pressures (p init) are for a completely molten magma ocean and T surf = 2700 K. Final partial pressures (p final) are for complete solidification and outgassing of all volatiles and T surf = 1400 K.
Paper: Retention of Water in Terrestrial Magma Oceans and Carbon-rich Early Atmospheres
Authors: Dan J. Bower, Kaustubh Hakim, Paolo A. Sossi, Patrick Sanan
Figure caption: Summary of atmospheric composition and hydrogen depletion of the interior during magma ocean cooling at 100%, 30%, and 0% melt, where the surface temperature is given below the melt fraction. Transition from carbon-dominated to hydrogen-dominated atmospheres depends on surface lid formation and the style of magma ocean crystallization, which may prevent or hinder interior outgassing below 30% melt fraction.
Paper: Retention of Water in Terrestrial Magma Oceans and Carbon-rich Early Atmospheres
Authors: Dan J. Bower, Kaustubh Hakim, Paolo A. Sossi, Patrick Sanan
Figure caption: Comparison of atmospheric composition and interior depletion at ΔIW = 0.5 for (1) C/H = 0.1, thee H oceans, γ = 1; (2) C/H = 1, three H oceans, γ = 1; (3) C/H = 0.1, one H ocean, γ = 1; and (4) “large escape” with C/H = 0.1, three H oceans, and an escape prefactor γ = 1000 (Equation (9)). (a, b) H2 partial pressure and volume mixing ratio; (d, e) CO partial pressure and volume mixing ratio; (c, f) interior depletion of H and C, respectively.
Paper: Retention of Water in Terrestrial Magma Oceans and Carbon-rich Early Atmospheres
Authors: Dan J. Bower, Kaustubh Hakim, Paolo A. Sossi, Patrick Sanan
Figure caption: Atmospheric pressures during magma ocean outgassing for different C/H and fO2. Columns from left to right show hydrogen (H) budgets of 1, 3, and 10 oceans, respectively. Rows from top to bottom show fO2 of ΔIW = −2, ΔIW = 0.5, and ΔIW = 4. Colors denote volatiles (red: CO; green: CO2; orange: H2; blue: H2O; purple: CH4), where solid lines show C/H = 1 and dashed lines show C/H = 5.
Paper: Retention of Water in Terrestrial Magma Oceans and Carbon-rich Early Atmospheres
Authors: Dan J. Bower, Kaustubh Hakim, Paolo A. Sossi, Patrick Sanan
Figure caption: Depletion of hydrogen (H) vs. melt fraction at ΔIW = 0.5 for H budgets of 1, 3, and 10 oceans and different C/H by weight. For each shaded region, the upper bound is C/H = 0, lower bound is C/H = 5, and black line is C/H = 1. Symbols indicate times of C/H = 1 cases near 20% melt and 5% melt.
Paper: Retention of Water in Terrestrial Magma Oceans and Carbon-rich Early Atmospheres
Authors: Dan J. Bower, Kaustubh Hakim, Paolo A. Sossi, Patrick Sanan
Figure caption: Depletion of hydrogen (H) vs. time at ΔIW = 0.5 for different C/H, where colored lines show constant melt fraction. Dashed lines show C/H = 0 for H budgets from 1 to 10 Earth oceans; these are the solid lines in Figure 3(b). Departing from the dashed lines, circles show three oceans and C/H = X, where X is 0, 1, or 5. Similarly, rectangles show 10 oceans and C/H = X, where X is 0, 1, or 5.
Paper: Retention of Water in Terrestrial Magma Oceans and Carbon-rich Early Atmospheres
Authors: Dan J. Bower, Kaustubh Hakim, Paolo A. Sossi, Patrick Sanan
Figure caption: Depletion of hydrogen (H) vs. time for different fO2, where colored lines show constant melt fraction. Dashed lines show ΔIW = 0.5 and C/H = 0 for H budgets from 1 to 10 Earth oceans; these are the solid lines in Figure 3b. Departing from the dashed lines, circles show three oceans and C/H = 1 for ΔIW = X, where X is −2, 0.5, or 4. Similarly, rectangles show 10 oceans and C/H = 1 for ΔIW = X, where X is −2, 0.5, or 4.
Paper: Retention of Water in Terrestrial Magma Oceans and Carbon-rich Early Atmospheres
Authors: Dan J. Bower, Kaustubh Hakim, Paolo A. Sossi, Patrick Sanan
Figure caption: Depletion of hydrogen (H) vs. melt fraction for H budgets of 1 and 10 oceans and different fO2. For each shaded region, the upper bound is ΔIW = −2, lower bound is ΔIW = 4, and black line (same as Figure 6) is ΔIW = 0.5. Symbols indicate times of ΔIW = 0.5 cases near 20% and 5% melt.
Paper: Geologic Context of the OSIRIS-REx Sample Site from High-resolution Topography and Imaging
Authors: O. S. Barnouin, E. R. Jawin, R. T. Daly, R.-L. Ballouz, M. G. Daly, J. A. Seabrook, P. Michel, Y. Zhang, C. L. Johnson, K. J. Walsh, M. M. Al Asad, R. Gaskell, J. Weirich, E. Palmer, E. B. Bierhaus, M. C. Nolan, C. W. V. Wolner, D. S. Lauretta
Figure caption: Regional area of Hokioi crater shown on the GTDM overlaid with (a) notation of features, (b) slope, and (d) OLA albedo measurements. The terrace, several craters of comparable size to Hokioi, a bright deposit apparently associated with a bright boulder, and a dark region surrounding the Hokioi crater are indicated. Arrows in panel (b) and the side view (panel (c)) show the slope break associated with the terrace mapped in panel (a). Arrows in panel (d) point to the bright deposit; the bright boulder is circled.
Paper: Geologic Context of the OSIRIS-REx Sample Site from High-resolution Topography and Imaging
Authors: O. S. Barnouin, E. R. Jawin, R. T. Daly, R.-L. Ballouz, M. G. Daly, J. A. Seabrook, P. Michel, Y. Zhang, C. L. Johnson, K. J. Walsh, M. M. Al Asad, R. Gaskell, J. Weirich, E. Palmer, E. B. Bierhaus, M. C. Nolan, C. W. V. Wolner, D. S. Lauretta
Figure caption: Northern view of the OLA GDTM (a) focusing on the Nightingale sample site and the Hokioi crater (star). The GDTM is overlaid with elevation relative to Bennu’s (b) geoid, (c) slope, (d) geologic units (Smooth Unit in pink and Rugged Unit in gray; Jawin et al. 2022), and (e) radius (i.e., distance to the facet from the center of figure). Notable features providing global context for the Nightingale site include longitudinal ridges (dashed lines in panel (a)), morphological evidence of a rock fall (long arrow in panels (a) and (c)), an unnamed ∼120 m crater enclosing Hokioi and Nightingale (dotted–dashed circle in panels (a), (c), (d), and (e)), and an area of high boulder density (gray hash in panel (b)). The profile of the 120 m crater (dashed magenta line in panel (e)) is shown in radius from center (panel (f)) and elevation (panel (g)).
Paper: Geologic Context of the OSIRIS-REx Sample Site from High-resolution Topography and Imaging
Authors: O. S. Barnouin, E. R. Jawin, R. T. Daly, R.-L. Ballouz, M. G. Daly, J. A. Seabrook, P. Michel, Y. Zhang, C. L. Johnson, K. J. Walsh, M. M. Al Asad, R. Gaskell, J. Weirich, E. Palmer, E. B. Bierhaus, M. C. Nolan, C. W. V. Wolner, D. S. Lauretta
Figure caption: (a) Close-up PolyCam image (∼5 cm pixel−1) and (b) LDTM (0.05 m GSD) of the bright boulder. The blue and magenta profiles overlaid on the topographic data in panel (b) are shown in panels (c) and (d). The blue profile indicates a probable impact crater on the boulder (black dashed and dotted lines). The magenta profile shows the flat edges of the boulder, reminiscent of fracture planes.
Paper: Geologic Context of the OSIRIS-REx Sample Site from High-resolution Topography and Imaging
Authors: O. S. Barnouin, E. R. Jawin, R. T. Daly, R.-L. Ballouz, M. G. Daly, J. A. Seabrook, P. Michel, Y. Zhang, C. L. Johnson, K. J. Walsh, M. M. Al Asad, R. Gaskell, J. Weirich, E. Palmer, E. B. Bierhaus, M. C. Nolan, C. W. V. Wolner, D. S. Lauretta
Figure caption: Example of creep inside Hokioi crater, consistent with mass movement downslope toward the south. (a) Context image of Hokioi crater from the global image mosaic (Bennett et al. 2021), in sinusoidal projection. The yellow box shows the extent of panel (b). (b) The yellow arrow indicates particles that have mantled a larger boulder owing to creep toward the south (from PolyCam image ocams20200303t211013s895; pixel scale, 0.0036 m; phase angle, 56°). The crater wall slope in this area is 40° based on the OLA DTM shown in Figure 5. (c) 0.5 m GSD LDTM of Hokioi crater. (d) Yellow outlines indicate subtle lobate features (see also the oblique perspective in Figure 5(a)) indicating surface slumps and material migration toward the south. Several events may have occurred, leading to the multiple lobate features. The orange circle approximately indicates the crater rim.
Paper: Geologic Context of the OSIRIS-REx Sample Site from High-resolution Topography and Imaging
Authors: O. S. Barnouin, E. R. Jawin, R. T. Daly, R.-L. Ballouz, M. G. Daly, J. A. Seabrook, P. Michel, Y. Zhang, C. L. Johnson, K. J. Walsh, M. M. Al Asad, R. Gaskell, J. Weirich, E. Palmer, E. B. Bierhaus, M. C. Nolan, C. W. V. Wolner, D. S. Lauretta
Figure caption: A 0.05 m GSD OLA LDTM illustrating the detailed morphology of the Nightingale site within Hokioi crater, including (a) an interior slump (black arrows), (b) OLA albedo, and (c) slopes. Panel (a) views the LDTM obliquely; panels (b) and (c) view it from above. The point on the surface where the OSIRIS-REx sampling mechanism made contact is indicated with a star.
Paper: Geologic Context of the OSIRIS-REx Sample Site from High-resolution Topography and Imaging
Authors: O. S. Barnouin, E. R. Jawin, R. T. Daly, R.-L. Ballouz, M. G. Daly, J. A. Seabrook, P. Michel, Y. Zhang, C. L. Johnson, K. J. Walsh, M. M. Al Asad, R. Gaskell, J. Weirich, E. Palmer, E. B. Bierhaus, M. C. Nolan, C. W. V. Wolner, D. S. Lauretta
Figure caption: Textures near the Nightingale sample site. (a) Context image of Hokioi crater from the global image mosaic (Bennett et al. 2021), in sinusoidal projection. The yellow box shows the extent of panel (b). (b) The region surrounding Nightingale contains a mixture of angular to subangular rock fragments and fine-grained material. Albedo variations are also apparent. The yellow star indicates the OSIRIS-REx contact point. From PolyCam image ocams20200303t210644s436 (pixel scale, 0.003 7 m; phase angle, 56°).
Paper: Geologic Context of the OSIRIS-REx Sample Site from High-resolution Topography and Imaging
Authors: O. S. Barnouin, E. R. Jawin, R. T. Daly, R.-L. Ballouz, M. G. Daly, J. A. Seabrook, P. Michel, Y. Zhang, C. L. Johnson, K. J. Walsh, M. M. Al Asad, R. Gaskell, J. Weirich, E. Palmer, E. B. Bierhaus, M. C. Nolan, C. W. V. Wolner, D. S. Lauretta
Figure caption: Sketch map of the Nightingale region, including Hokioi crater (orange outline), small candidate craters (red outlines with shading), the 120 m crater in which Hokioi is located (long red outline on the western side of Hokioi), and the edge of an adjacent high-standing region (green outline). Fine-grained deposits surrounding the crater (yellow) are interpreted to be crater ejecta. The basemap over which these features are annotated is from the global image mosaic (Bennett et al. 2021), in sinusoidal projection.
Paper: Geologic Context of the OSIRIS-REx Sample Site from High-resolution Topography and Imaging
Authors: O. S. Barnouin, E. R. Jawin, R. T. Daly, R.-L. Ballouz, M. G. Daly, J. A. Seabrook, P. Michel, Y. Zhang, C. L. Johnson, K. J. Walsh, M. M. Al Asad, R. Gaskell, J. Weirich, E. Palmer, E. B. Bierhaus, M. C. Nolan, C. W. V. Wolner, D. S. Lauretta
Figure caption: Schematic of the geological history of the Nightingale sample site. The schematic approximates the region of Bennu shown in Figure 2.
Paper: Geologic Context of the OSIRIS-REx Sample Site from High-resolution Topography and Imaging
Authors: O. S. Barnouin, E. R. Jawin, R. T. Daly, R.-L. Ballouz, M. G. Daly, J. A. Seabrook, P. Michel, Y. Zhang, C. L. Johnson, K. J. Walsh, M. M. Al Asad, R. Gaskell, J. Weirich, E. Palmer, E. B. Bierhaus, M. C. Nolan, C. W. V. Wolner, D. S. Lauretta
Figure caption: (a) Location (black box) in the 0.05 m OLA LDTM (Figure 5) of (b) the 0.01 m GSD SPO LDTM of the Nightingale site. (c) Surface height profiles at the OSIRIS-REx contact area (magenta circle).
Paper: The Spatial Distribution and Temperature of Mercury's Potassium Exosphere
Authors: Patrick Lierle, Carl Schmidt, Jeffrey Baumgardner, Luke Moore, Tom Bida, Ryan Swindle
Figure caption: Exospheric potassium brightness from the RIPS 5 s integration full-disk scans on 2018 December 12. North is up, and this faces Mercury's evening hemisphere. Pictured at right is an unconvolved photometric reflectance model of Mercury at the time and geometry of observation, which has been overlaid with surface topography. The green contours are constructed from the photometric model after it has been convolved to match the mean atmospheric seeing.
Paper: The Spatial Distribution and Temperature of Mercury's Potassium Exosphere
Authors: Patrick Lierle, Carl Schmidt, Jeffrey Baumgardner, Luke Moore, Tom Bida, Ryan Swindle
Figure caption: Locations of the EXPRES aperture for each of the six frames acquired on 2018 December 13. This shows fast tip-tilt slit-viewing camera frames co-aligned over all measurements with a plate scale of 0.″16 pixel−1. Pointing is concentrated just off-disk beyond the evening terminator.
Paper: The Spatial Distribution and Temperature of Mercury's Potassium Exosphere
Authors: Patrick Lierle, Carl Schmidt, Jeffrey Baumgardner, Luke Moore, Tom Bida, Ryan Swindle
Figure caption: A forward model of the potassium D1 emission line at five temperatures ranging from 50 to 1200 K incorporating hyperfine components from Welty et al. (1994, Table 4).
Paper: The Spatial Distribution and Temperature of Mercury's Potassium Exosphere
Authors: Patrick Lierle, Carl Schmidt, Jeffrey Baumgardner, Luke Moore, Tom Bida, Ryan Swindle
Figure caption: A raw 200 s RIPS integration of Mercury at 81° phase angle with the K λ7699 solar absorption line nearly centered. This is a single CCD image with the spectra recorded on the top half of the detector and the narrowband image on the bottom half. The spectral channel has been multiplied by 15 artificially here to improve visibility.
Paper: The Spatial Distribution and Temperature of Mercury's Potassium Exosphere
Authors: Patrick Lierle, Carl Schmidt, Jeffrey Baumgardner, Luke Moore, Tom Bida, Ryan Swindle
Figure caption: (a) A raw narrowband image of Mercury reflected by RIPS's mirrored slit jaws. (b) A photometric model of Mercury's surface reflectance matched to the observation geometry. (c) The photometric model, blurred to match the atmospheric seeing, superimposed with a re-creation of RIPS's slit.
Paper: Spitzer Dayside Emission of WASP-34b
Authors: Ryan C. Challener, Joseph Harrington, Patricio E. Cubillos, Jasmina Blecic, Barry Smalley
Figure caption: Lowest BIC BART-retrieved spectra as planet-to-star flux ratio. The black circles are the spectrum integrated over the filters. The black circles, not the light-blue line, should match the red data. The shaded region denotes the 3σ uncertainty on the best-fit isothermal atmosphere. The IRAC response functions are plotted along the y-axis (arbitrary units). Left: isothermal (blackbody) spectrum retrieved using the BLISS eclipse depths. Features are caused by the stellar spectrum (ATLAS9; Castelli & Kurucz 2004); the planetary spectrum is a smooth blackbody curve. Right: the isothermal spectrum retrieved using the PLD eclipse depths.
Paper: Spitzer Dayside Emission of WASP-34b
Authors: Ryan C. Challener, Joseph Harrington, Patricio E. Cubillos, Jasmina Blecic, Barry Smalley
Figure caption: Lowest BIC BART-retrieved temperature–pressure profiles. Dark-blue and light-blue regions denote the 1σ and 2σ boundaries, respectively. We have overplotted contribution functions for the two Spitzer data points, which show the portion of the atmosphere probed by our retrieval. Left: the isothermal (case 7) profile retrieved from the BLISS eclipse depths. Right: the thermal profile retrieved using PLD eclipse depths (case 6).
Paper: Spitzer Dayside Emission of WASP-34b
Authors: Ryan C. Challener, Joseph Harrington, Patricio E. Cubillos, Jasmina Blecic, Barry Smalley
Figure caption: Comparison of fit residual rms versus bin size with the expected standard error. If the fit residual rms is above the standard error, there is correlated noise present at that timescale. For all four cases, the standard error is within the uncertainties of the residual fit rms at nearly all bin sizes, indicating low residual correlated noise.
Paper: Spitzer Dayside Emission of WASP-34b
Authors: Ryan C. Challener, Joseph Harrington, Patricio E. Cubillos, Jasmina Blecic, Barry Smalley
Figure caption: Eccentricity histograms derived from MCMC posterior distributions of ﹩e{\rm{\sin }}\omega ﹩ and ﹩e{\rm{\cos }}\omega ﹩. The red line marks the best-fit value, and the blue regions denote the 1σ, 2σ, and 3σ regions. Top: posterior from the fit to the BLISS results. Bottom: posterior from the fit to the PLD results.
Paper: Retention of Water in Terrestrial Magma Oceans and Carbon-rich Early Atmospheres
Authors: Dan J. Bower, Kaustubh Hakim, Paolo A. Sossi, Patrick Sanan
Figure caption: Coupled interior and atmosphere evolution during magma ocean outgassing at ΔIW = 0.5 with a hydrogen budget of one Earth ocean (no carbon), where E1 shows equilibrium crystallization and F1 shows fractional crystallization. For E1 and F1: (a, d) interior temperature, with gray showing the mixed phase region where melt and solid coexist; (b, e) interior melt fraction. (c) Atmospheric partial pressure of H2 and H2O for E1 and F1, where the pressures of F1 (black lines) initially follow E1 (gray lines) before departing at late time. Colored vertical ticks and lines show times in panels (a), (b), (d), and (e), and labels show when a surface lid forms for E1 and F1. (f) Interior depletion of melt (“Melt”) and hydrogen (“Hydr.”) for E1 and F1.
Paper: Retention of Water in Terrestrial Magma Oceans and Carbon-rich Early Atmospheres
Authors: Dan J. Bower, Kaustubh Hakim, Paolo A. Sossi, Patrick Sanan
Figure caption: Depletion of hydrogen (H) from the interior during magma ocean outgassing at ΔIW = 0.5 for H budgets from 1 to 10 Earth oceans: (a) equilibrium crystallization, and (b) fractional crystallization. Lines show constant melt fraction, and circles show the H budget. Magma ocean stage ends at around 30% melt for equilibrium crystallization and 2% melt for fractional crystallization. Cases E1 and F1 (Figure 2) correspond to 1 H ocean for equilibrium and fractional crystallization, respectively. Dashed lines in panel (a) with a “W” suffix denote models that only include H as H2O, i.e., a completely oxidized mantle.
Paper: Retention of Water in Terrestrial Magma Oceans and Carbon-rich Early Atmospheres
Authors: Dan J. Bower, Kaustubh Hakim, Paolo A. Sossi, Patrick Sanan
Figure caption: Experimentally determined solubility data of H2O for several melt compositions and temperatures, for fugacities from 0 to 200 bars (Table 1). Dotted lines denote β = 2.0, and α is reported at the end of the lines (Equation (1)).
Paper: Retention of Water in Terrestrial Magma Oceans and Carbon-rich Early Atmospheres
Authors: Dan J. Bower, Kaustubh Hakim, Paolo A. Sossi, Patrick Sanan
Figure caption: The fugacity of CO in equilibrium with graphite (Equation (11)) assuming ideal gas behavior as a function of temperature at ΔIW = −2 (dashed black line) and ΔIW = 0.5 (dashed gray line). All cases at ΔIW = −2 and C/H = 5 (colored lines) intercept the CCO buffer at ΔIW = −2, indicating graphite precipitation. Only cases that intercept the CCO buffer are plotted.
Paper: Retention of Water in Terrestrial Magma Oceans and Carbon-rich Early Atmospheres
Authors: Dan J. Bower, Kaustubh Hakim, Paolo A. Sossi, Patrick Sanan
Figure caption: Atmospheric composition during magma ocean outgassing at fO2 of ΔIW = −2. See Figure 4 caption.
Paper: Retention of Water in Terrestrial Magma Oceans and Carbon-rich Early Atmospheres
Authors: Dan J. Bower, Kaustubh Hakim, Paolo A. Sossi, Patrick Sanan
Figure caption: Atmospheric composition during magma ocean outgassing at fO2 of ΔIW = 2. See Figure 4 caption.
Paper: Retention of Water in Terrestrial Magma Oceans and Carbon-rich Early Atmospheres
Authors: Dan J. Bower, Kaustubh Hakim, Paolo A. Sossi, Patrick Sanan
Figure caption: Atmospheric composition during magma ocean outgassing at fO2 of ΔIW = 4. See Figure 4 caption.
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: VenDI simulation utilizing data from the Zagros Mountains in Iran as a tessera analog at scales anticipated during the DS descent (FOV 7 km × 7 km). Satellite image data courtesy Maxar WorldView (WV-02) processed by NASA Goddard to produce VenDI-like band-ratio maps and to construct a ∼3 m ground-scale distance digital elevation map (DEM), as shown here in a color-scaled perspective view. DAVINCI's VenDI will produce similar data sets for Alpha Regio from altitudes below ∼7 km, depending on the final descent timeline during the actual DS entry-descent-science phase. Left: the Structure-from-Motion-based DEM has been ray-traced to be an oblique view to highlight geological structures at 30 m scale for stratigraphic analysis. Right: band-ratio compositional imaging overlain on the DEM will allow potential identification of felsic rocks on Venus in their stratigraphic settings.
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: Mass–radius relations for differentiated rocky planets. The solid blue curve is for an Earth-like planet with a pure Fe core and a MgSiO3 perovskite mantle. This case corresponds to an unreactive core in our calculations. All curves correspond to a core mass fraction of 32%. The solid and dashed black curves represent solutions for planets with reactive cores, in which the Fe metal cores have density deficits of 28% and 43% due to H and O in the metal. A 28% density deficit in Fe corresponds to about 2% H and 8% O by mass, corresponding to a metal core–silicate mantle equilibration temperature of about 5000 K with 4 wt% total H (black line) in our models. The 43% density deficit in Fe represents the maximum amount of H and O we expect to be dissolved in Fe because otherwise the core will become less dense than the mantle and corresponds to 3% H and 14% O by mass (black dashed line). Also shown are masses and radii for planets where uncertainties in mass and radius are <35% and <15%, respectively, as reported in the NASA Exoplanet Archive. Each datum is color-coded for nominal densities relative to Earth (see text for details). The gray shaded area spans the region for pure Fe core mass fractions ranging from 0.17 to 0.34, representing an estimate of the 1σ density uncertainty among rocky super-Earths derived from planetary evolution and mass-loss models that successfully explain the radius gap in the exoplanet size distribution (Rogers & Owen 2021). Solar system rocky planets are shown for reference.