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Convective shutdown in the atmospheres of lava worlds

T0 review · 0 major / 7 minor · reviewed 2026-08-11 · deepseek-v4-flash

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Pith's one-line read A lava world can hold a permanent magma ocean even when its atmosphere becomes stable to convection.

desk verdict The central claim holds: convectively stable atmospheres can still maintain permanent magma oceans, and this paper deserves a serious referee. read the letter →

arxiv 2412.11987 v1 pith:C6LQ274X submitted 2024-12-16 astro-ph.EP

Harrison Nicholls , Raymond T. Pierrehumbert , Tim Lichtenberg , Laurent Soucasse , Stef Smeets This is my paper · ORCID
classification astro-ph.EP
keywords lavaworldsmagmaoceansconvectiveshutdownradiative-convectiveequilibriumexoplanetatmospheresoxygenfugacityHD63433dTRAPPIST-1c
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The reading

The paper challenges a standard assumption in models of lava worlds: that the atmospheres above magma oceans are always fully convective. It presents a one-dimensional radiative-convective model that allows atmospheric layers to become stable to convection, and couples it to an interior-evolution model to simulate two Earth-sized exoplanets. The central result is that a convectively stable, largely isothermal atmosphere can still insulate a permanently molten surface, so convective shutdown does not preclude a permanent magma ocean. Applied to HD 63433 d, the model keeps a magma ocean to the present day with an atmosphere depleted in water; applied to TRAPPIST-1 c, it predicts solidification within about 100 million years. These outcomes matter because they change how the emission spectra of lava planets should be interpreted and what they can reveal about mantle redox state.

What carries the argument

The central object is AGNI, a new one-dimensional radiative-convective atmosphere model for lava planets. AGNI computes radiative transfer with a spectral radiation scheme, parameterises convection with mixing-length theory, treats latent heat transport from condensing volatiles, and solves for the temperature-pressure profile by requiring the total energy flux to be constant with height using a Newton-Raphson root-finding method. It is coupled through the PROTEUS interior-atmosphere framework to a magma-ocean evolution code, allowing outgassed volatile composition (including sulphur, via a new solubility law) to feed back on cooling. The model's key capability is that convective instability is diagnosed rather than assumed, which is what allows convective shutdown to occur.

What would settle it

Run a 3D general circulation model of HD 63433 d's atmosphere with the same outgassed compositions: if day-night dynamics or resolved convection keep the deep atmosphere convectively mixed even where the 1D profile is isothermal, then the permanent-magma-ocean-without-convection state would not survive in more dimensions.

Watch

Extended reading notes

Core claim

The paper's central claim is that it is possible to maintain permanent magma oceans underneath atmospheres without convection. In the model atmospheres of HD 63433 d, deep isothermal layers form that are stable to convection, yet the surface remains hot enough to keep the mantle substantially molten; under reducing conditions the whole atmosphere becomes purely radiative. Convection, where it occurs, is driven by absorption of downwelling stellar radiation rather than by interior heat, while for TRAPPIST-1 c the opposite holds: convection is sustained by heat escaping the cooling magma ocean, and the planet solidifies within 5 to 96 million years depending on oxygen fugacity. The paper also shows that the strength of CO2 and SO2 absorption features in synthetic emission spectra tracks the mantle's oxygen fugacity, so future observations of HD 63433 d could probe the redox state of an Earth-like magma ocean. Finally, near-isothermal stratospheres produced by low-molecular-weight, reduced atmospheres can mimic the blackbody emission of an atmosphere-less rocky body, cautioning against simple brightness-temperature interpretations.

Load-bearing premise

The simulations hold the mantle's oxygen fugacity fixed for the entire run, so if it drifts as crystals form or as the melt reacts with water and hydrogen, the resulting atmospheres and solidification times could differ.

Editorial extensions

If this is right

  • The standard fully-convective assumption in lava-world evolution models should be relaxed; radiative-convective models can give qualitatively different evolutionary outcomes, including permanent magma oceans where older models predicted solidification or vice versa.
  • HD 63433 d may still host a permanent magma ocean and a water-depleted secondary atmosphere today, making it an observable analogue for a young Earth or Venus.
  • TRAPPIST-1 c is predicted to have solidified within about 100 Myr, outgassing a thick atmosphere whose composition depends strongly on mantle oxygen fugacity.
  • Emission spectra of these planets carry redox-sensitive CO2 and SO2 features within JWST MIRI and NIRSpec bandpasses, potentially constraining magma ocean geochemistry.
  • A cool isothermal stratosphere above a reduced atmosphere can mimic the emission of an atmosphere-less body, so secondary-eclipse photometry alone may not distinguish bare rocks from some lava planets.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • If mantle oxygen fugacity evolves during crystallization, as the paper notes it would in reality, the predicted atmospheric composition and solidification times could shift; re-running the simulations with self-consistent redox evolution would map that sensitivity.
  • The blackbody mimicry of reduced atmospheres suggests that other observations of apparently airless lava planets may also need to consider isothermal H2/CO atmospheres as degenerate alternatives to bare rock.
  • Tidal heating, especially in the TRAPPIST-1 system, could supply the upward heat flux needed to keep convection alive and stall solidification; coupling the present framework to tidal dissipation models would test whether any TRAPPIST-1 planet can hold a magma ocean.
  • If photochemical S8 haze forms in the upper atmosphere, as the equilibrium-chemistry case study hints, redox-driven spectral features could be dampened; combining the model with photochemistry would test whether the oxygen-fugacity diagnostic survives real atmospheric processing.
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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

0 major / 7 minor

Summary. This paper introduces AGNI, a 1D radiative-convective atmosphere model with mixing-length convection, latent-heat transport, and SOCRATES-based radiative transfer, coupled to the PROTEUS magma-ocean evolution framework. The authors apply it to HD 63433 d and TRAPPIST-1 c over mantle fO2 values from IW-5 to IW+5, comparing AGNI against the fully convective JANUS model. The central finding is that HD 63433 d can maintain a permanent magma ocean despite deep convective shutdown in its outgassed atmosphere, while TRAPPIST-1 c solidifies within roughly 100 Myr in the AGNI runs. Synthetic emission spectra show CO2 and SO2 features that correlate with mantle redox, and the paper argues that isothermal H2-rich stratospheres can masquerade as bare-rock emission.

Significance. The central result is significant: it demonstrates that convective shutdown does not preclude permanent magma oceans, contradicting a direct extrapolation of Selsis et al. (2023) to mixed-composition atmospheres and challenging the fully-convective assumption used in most magma-ocean evolution models. The paper is strong in benchmarking and transparency: AGNI reproduces the deep isothermal layers and general structure of the independent Selsis et al. (2023) pure-steam calculations with small per-level flux residuals (Fig. 2), all code is open source, data are deposited on Zenodo, and the limitations (constant fO2, 1D geometry, MT_CKD continuum, escape, tidal heating) are explicitly acknowledged in Section 4.4. The constant-fO2 concern, which might otherwise be the weakest assumption, is mitigated by the complete fO2 sweep: across all 11 AGNI cases HD 63433 d retains significant melt, so moderate fO2 drift would not overturn the qualitative central claim. The observational predictions for CO2 and SO2 as redox tracers in HD 63433 d are concrete and falsifiable.

minor comments (7)
  1. [Table 2] The semi-major axis quoted for HD 63433 d is 0.503 AU, which is inconsistent with the stated equilibrium temperature of 1040 K and with the planet's treatment as a highly irradiated lava world; this appears to be a missing leading zero (0.0503 AU) and should be corrected.
  2. [Section 2.3] The closing sentence of Section 2.3 says the atmosphere model "is validated against previous work in Section 2.3", but the validation actually appears in Section 3.2; the cross-reference should be fixed.
  3. [Section 2.2] The eccentricity discussion refers to "HD 63443 d"; this should read "HD 63433 d".
  4. [Section 3.3 / Fig. 3 caption] The text refers to the surface-temperature curve in the top panel as a black line and to the solidification-time curve in the bottom panel as a black line, while the figure caption describes these as red and blue lines, respectively; the color references should be made consistent.
  5. [Section 4.1] The comparison that AGNI surface temperatures are approximately 2000 K lower than JANUS surface temperatures is stated without a directly corresponding panel; adding JANUS surface temperatures to Fig. 3 or citing a specific panel would make this claim easier to verify.
  6. [Section 4.2] In the paragraph discussing the TRAPPIST-1 c spectra, the phrase "there are there are clear molecular features" contains a duplicated phrase, and the following sentence again misspells the planet as "HD 63443 d".
  7. [Introduction, first paragraph] The phrase "which could be be equilibrium with a permanently molten interior" contains a grammar error and should read "which could be in equilibrium with a permanently molten interior".

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity identified; conclusions emerge from forward radiative-convective modeling with external validation.

full rationale

The paper's central claims — that mixed-composition atmospheres over magma oceans can be convectively stable and that convective shutdown does not preclude permanent magma oceans — are outputs of a forward 1D radiative-convective model (AGNI) coupled to an interior evolution framework (PROTEUS). The radiative transfer uses the externally developed SOCRATES scheme with tabulated opacities, and the model is validated against the independent Selsis et al. (2023) pure-steam calculations. No model parameter is fitted to the target planets' observed properties; instead, the paper sweeps mantle oxygen fugacity over IW−5 to IW+5 and reports the resulting evolutionary outcomes. The key atmospheric structures (deep isothermal layers, convective shutdown) are diagnosed from the solved temperature profiles, not imposed by construction. The convective flux is computed from mixing-length theory with standard parameters, and the energy-conservation root-finding determines the temperature structure rather than assuming a convective or radiative profile a priori. The paper's self-citations to Nicholls et al. (2024) and the PROTEUS/JANUS framework concern software implementation and prior modeling assumptions, not an unverified uniqueness theorem or a fitted parameter renamed as a prediction; these citations are appropriate and not load-bearing in a circular sense. The acknowledged limitations (constant fO2, MT_CKD continuum extrapolation, 1D global-mean geometry, neglect of escape) are honest uncertainties that affect quantitative outcomes but do not reduce the central possibility claim to its own inputs. No equation in the paper is shown to be equivalent to another by definition in a way that would force the result, and no quantity fitted to a subset is later reported as an independent prediction. The manuscript is therefore self-contained against external benchmarks, and no significant circularity is present.

Assumptions & free parameters 6 free parameters · 7 assumptions · 0 invented entities

The central results depend on standard physical equations plus a chain of clearly stated domain assumptions: 1D global-mean geometry, constant fO2, chemical equilibrium outgassing, a conductive magma-ocean boundary layer, and neglect of escape and tidal heating. These assumptions are stated in Sections 2.3-2.4 and their weaknesses are revisited in Section 4.4. No new physical entities are introduced.

free parameters (6)
  • Bulk water inventory = 8 Earth oceans
    Assumed total hydrogen inventory for both simulated planets (Salvador et al. 2023; Lichtenberg & Miguel 2025); strongly affects H2O outgassing, greenhouse trapping, and magma ocean lifetime.
  • HD 63433 d mass = 1.0 Earth mass
    The mass is unmeasured and assumed; the authors argue this is unlikely an underestimate because no sub-Earth exoplanet with Earth-like radius is known (Parc et al. 2024).
  • Condensation timescale tau = 3 x 10^4 s
    Fixed value from Trenberth (1992) for latent heat transport; microphysical self-consistency is beyond scope (Section 2.3).
  • Sensible heat exchange coefficients = Cd = 0.001, U = 2 m/s
    Fixed surface drag coefficient and wind speed used for surface-atmosphere sensible heat flux (Eq. 8; Pierrehumbert 2010).
  • Bond albedo = 0.3 (spectrally grey)
    Assumed from Essack et al. (2020) and Fortin et al. (2024); sets the absorbed stellar radiation.
  • Core radius fraction = 0.55
    Fixed core-to-mantle radius ratio from Lodders & Fegley (1998); affects interior cooling and melt evolution.
assumptions (7)
  • standard math Hydrostatic balance, ideal gas law, and plane-parallel radiative transfer describe the atmosphere
    Used throughout Section 2.3 to construct the 1D atmosphere model.
  • domain assumption The atmosphere is well-mixed except for condensation, and outgassed composition is set by equilibrium with the magma ocean at constant fO2
    Stated in Sections 2.3 and 2.4; fO2 is held fixed, and the authors acknowledge in Section 4.4 that fO2 should evolve.
  • domain assumption A tidally locked planet is represented by a single global-mean column with zenith angle cos^-1(1/sqrt(3)) and 1/4 stellar flux scaling
    Section 2.4; ignores day-night heat redistribution and 3D dynamics.
  • domain assumption The magma ocean surface has a thin conductive boundary layer with heat flux given by Fourier's law (Eq. 18)
    Section 2.3, following Solomatov (2007) and prior PROTEUS works.
  • domain assumption Volatile outgassing follows the solubility laws of Gaillard et al. (2022) and Boulliung & Wood (2022), including S2 oxidation to SO2
    Section 2.1; the resulting compositions are shown in Fig. 1 and drive the radiative-convective structure.
  • domain assumption Atmospheric escape, tidal heating, and time-variable fO2 are neglected
    Acknowledged in Section 4.4 as limitations that could alter the fate of both planets.
  • domain assumption The MT_CKD water continuum, calibrated at temperate conditions, applies at magma-ocean temperatures
    Used for H2O continuum opacity; the authors flag the extrapolation as a potential error source (Section 4.4).

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Cite this review

Pith. "Pith review of Convective shutdown in the atmospheres of lava worlds." pith.science (2026). https://pith.science/paper/C6LQ274X

@misc{pith2026241211987,
  author       = {Pith},
  title        = {Pith review of: Convective shutdown in the atmospheres of lava worlds},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/C6LQ274X}},
  note         = {Machine review of arXiv:2412.11987}
}
read the original abstract

Atmospheric energy transport is central to the cooling of primordial magma oceans. Theoretical studies of atmospheres on lava planets have assumed that convection is the only process involved in setting the atmospheric temperature structure. This significantly influences the ability for a magma ocean to cool. It has been suggested that convective stability in these atmospheres could preclude permanent magma oceans. We develop a new 1D radiative-convective model in order to investigate when the atmospheres overlying magma oceans are convectively stable. Using a coupled interior-atmosphere framework, we simulate the early evolution of two terrestrial-mass exoplanets: TRAPPIST-1 c and HD 63433 d. Our simulations suggest that the atmosphere of HD 63433 d exhibits deep isothermal layers which are convectively stable. However, it is able to maintain a permanent magma ocean and an atmosphere depleted in H2O. It is possible to maintain permanent magma oceans underneath atmospheres without convection. Absorption features of CO2 and SO2 within synthetic emission spectra are associated with mantle redox state, meaning that future observations of HD 63433 d may provide constraints on the geochemical properties of a magma ocean analogous with the early Earth. Simulations of TRAPPIST-1 c indicate that it is expected to have solidified within 100 Myr, outgassing a thick atmosphere in the process. Cool isothermal stratospheres generated by low molecular-weight atmospheres can mimic the emission of an atmosphere-less body. Future work should consider how atmospheric escape and chemistry modulates the lifetime of magma oceans, and the role of tidal heating in sustaining atmospheric convection

Figures

Figures reproduced from arXiv: 2412.11987 by the authors.

Figure 1
Figure 1. Gas partial pressures at 2500 K versus 𝑓 O2. Mid-ocean ridge basalt has an 𝑓 O2 approximately equal to the Fayalite-Magnetite-Quartz (FMQ) buffer, equivalent to IW+3.69 (Schaefer & Elkins-Tanton 2018). Observations indicate that Mercury’s surface probably erupted with an 𝑓 O2 between IW￾6.5 and IW-3.5 (Namur et al. 2016), overlapping with the 𝑓 O2 of the Solar nebula at approximately IW-7 to IW-6 (Doyle et al. 2019;… view at source ↗
Figure 3
Figure 3. shows how the melt fractions (y-axes) calculated in our sim￾ulations depend on the oxygen fugacity of the mantle (x-axes) and the atmosphere model (top and bottom panels). The top panel shows this for HD 63433 d, where square scatter points show the resul￾tant melt fraction from simulations coupled to AGNI, while circular scatter point show the results from those coupled to JANUS. The bot￾tom panel shows the corresp… view at source ↗
Figure 4
Figure 4. Outgassed atmospheric composition at model termination for HD 63433 d (top) and TRAPPIST-1 c (bottom), versus mantle 𝑓 O2 (x-axis), simulated with both atmosphere models (y-axis). Pie chars show volatile volume mixing ratios and white numbers show log10 total surface pressure [bar]. CO2 dominated, with little atmospheric H2O due to its favourable dissolution into the large amount of melt (Nicholls et al. 2024). Ther… view at source ↗
Figures from the paper (3 more)
Figure 5
Figure 5. Figure 5: Atmospheric temperature profiles at model termination for HD 63433 d (top) and TRAPPIST-1 c (bottom), versus mantle 𝑓 O2 (line colour), simulated with both atmosphere models (line style). Square markers denote the presence of convective regions in the AGNI cases, where…
Figure 6
Figure 6. Figure 6: Top-of-atmosphere flux representative of the planet-averaged outgoing radiation at model termination for HD 63433 d and a young TRAPPIST-1 c, versus mantle 𝑓 O2 (colourbar). For HD 63433 d (top panel) this corresponds to the planet at radiative equilibrium at an early …
Figure 7
Figure 7. Figure 7: Composition and temperature versus pressure in the model at￾mosphere of a young TRAPPIST-1 c (IW+5). This corresponds to the point of magma ocean solidification, with elemental abundances derived from time-evolution with AGNI/PROTEUS (dashed lines) and then used to det…

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Works this paper leans on

148 extracted references · 14 canonical work pages

  1. [1]

    Abe Y., Matsui T., 1986, @doi [Journal of Geophysical Research: Solid Earth] https://doi.org/10.1029/JB091iB13p0E291 , 91, E291

    doi:10.1029/jb091ib13p0e291 1986

  2. [2]

    Agol E., et al., 2021, @doi [The Planetary Science Journal] 10.3847/PSJ/abd022 , 2, 1

    doi:10.3847/psj/abd022 2021

  3. [3]

    R., Furtenbacher T., Tennyson J., Yurchenko S

    Al Derzi A. R., Furtenbacher T., Tennyson J., Yurchenko S. N., Császár A. G., 2015, @doi [Journal of Quantitative Spectroscopy and Radiative Transfer] https://doi.org/10.1016/j.jqsrt.2015.03.034 , 161, 117

    doi:10.1016/j.jqsrt.2015.03.034 2015

  4. [4]

    K., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2411.03154 , https://ui.adsabs.harvard.edu/abs/2024arXiv241103154A p

    Alam M. K., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2411.03154 , https://ui.adsabs.harvard.edu/abs/2024arXiv241103154A p. arXiv:2411.03154

    arXiv doi:10.48550/arxiv.2411.03154 2024

  5. [5]

    Amundsen D., Baraffe I., Tremblin P., Manners J., Hayek W., Mayne N., Acreman D., 2014, @doi [A&A] 10.1051/0004-6361/201323169 , 564, A59

    doi:10.1051/0004-6361/201323169 2014

  6. [6]

    C., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2410.11048 , https://ui.adsabs.harvard.edu/abs/2024arXiv241011048A p

    August P. C., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2410.11048 , https://ui.adsabs.harvard.edu/abs/2024arXiv241011048A p. arXiv:2410.11048

    arXiv doi:10.48550/arxiv.2410.11048 2024

  7. [7]

    Azzam A. A. A., Tennyson J., Yurchenko S. N., Naumenko O. V., 2016, @doi [Monthly Notices of the Royal Astronomical Society] 10.1093/mnras/stw1133 , 460, 4063

    doi:10.1093/mnras/stw1133 2016

  8. [8]

    Banerjee A., et al., 2024, @doi [The Astrophysical Journal Letters] 10.3847/2041-8213/ad73d0 , 975, L11

    doi:10.3847/2041-8213/ad73d0 2024

Show all 148 references
  1. [9]

    Baraffe I., Homeier D., Allard F., Chabrier G., 2015, @doi [Astronomy & Astrophysics] 10.1051/0004-6361/201425481 , 577, A42

    2015 doi

  2. [10]

    J., Strange J

    Barber R. J., Strange J. K., Hill C., Polyansky O. L., Mellau G. C., Yurchenko S. N., Tennyson J., 2013, @doi [Monthly Notices of the Royal Astronomical Society] 10.1093/mnras/stt2011 , 437, 1828

    2013 doi

  3. [11]

    Baumeister P., Tosi N., Brachmann C., Grenfell, John Lee Noack, Lena 2023, @doi [A&A] 10.1051/0004-6361/202245791 , 675, A122

    2023 doi

  4. [12]

    B., 2017, @doi [SIAM R eview] 10.1137/141000671 , 59, 65

    Bezanson J., Edelman A., Karpinski S., Shah V. B., 2017, @doi [SIAM R eview] 10.1137/141000671 , 59, 65

    2017 doi

  5. [13]

    K., 1962, @doi [Journal of Geophysical Research] 10.1029/JZ067i008p03095 , 67, 3095

    Blackadar A. K., 1962, @doi [Journal of Geophysical Research] 10.1029/JZ067i008p03095 , 67, 3095

    1962 doi

  6. [14]

    J., Timpe M

    Bonati I., Lichtenberg T., Bower D. J., Timpe M. L., Quanz S. P., 2019, @doi [ ] 10.1051/0004-6361/201833158 , https://ui.adsabs.harvard.edu/abs/2019A&A...621A.125B 621, A125

    2019 doi

  7. [15]

    T., 2021, @doi [The Astrophysical Journal] 10.3847/1538-4357/ac1345 , 919, 130

    Boukrouche R., Lichtenberg T., Pierrehumbert R. T., 2021, @doi [The Astrophysical Journal] 10.3847/1538-4357/ac1345 , 919, 130

    2021 doi

  8. [16]

    J., 2022, @doi [Geochimica et Cosmochimica Acta] https://doi.org/10.1016/j.gca.2022.08.032 , 336, 150

    Boulliung J., Wood B. J., 2022, @doi [Geochimica et Cosmochimica Acta] https://doi.org/10.1016/j.gca.2022.08.032 , 336, 150

    2022 doi

  9. [17]

    J., Sanan P., Wolf A

    Bower D. J., Sanan P., Wolf A. S., 2018, @doi [Physics of the Earth and Planetary Interiors] 10.1016/j.pepi.2017.11.004 , https://ui.adsabs.harvard.edu/abs/2018PEPI..274...49B 274, 49

    2018 doi

  10. [18]

    J., Hakim K., Sossi P

    Bower D. J., Hakim K., Sossi P. A., Sanan P., 2022, @doi [The Planetary Science Journal] 10.3847/PSJ/ac5fb1 , 3, 93

    2022 doi

  11. [19]

    M., Asphaug E., 2001, , https://ui.adsabs.harvard.edu/abs/2001Natur.412..708C 412, 708

    Canup R. M., Asphaug E., 2001, , https://ui.adsabs.harvard.edu/abs/2001Natur.412..708C 412, 708

    2001

  12. [20]

    K., et al., 2024, @doi [The Astronomical Journal] 10.3847/1538-3881/ad1039 , 167, 54

    Capistrant B. K., et al., 2024, @doi [The Astronomical Journal] 10.3847/1538-3881/ad1039 , 167, 54

    2024 doi

  13. [21]

    arXiv:2410.13457

    Cesario L., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2410.13457 , https://ui.adsabs.harvard.edu/abs/2024arXiv241013457C p. arXiv:2410.13457

    2024 doi arXiv

  14. [22]

    L., et al., 2018, @doi [Journal of Quantitative Spectroscopy and Radiative Transfer] https://doi.org/10.1016/j.jqsrt.2018.07.012 , 218, 178

    Chubb K. L., et al., 2018, @doi [Journal of Quantitative Spectroscopy and Radiative Transfer] https://doi.org/10.1016/j.jqsrt.2018.07.012 , 218, 178

    2018 doi

  15. [23]

    Gulf Professional Publishing, Burlington, @doi 10.1016/B978-0-7506-7766-0.X5000-3

    Coker A., 2007, Ludwig's Applied Process Design for Chemical and Petrochemical Plants. Gulf Professional Publishing, Burlington, @doi 10.1016/B978-0-7506-7766-0.X5000-3

    2007 doi

  16. [24]

    A., Yurchenko S

    Coles P. A., Yurchenko S. N., Tennyson J., 2019, @doi [Monthly Notices of the Royal Astronomical Society] 10.1093/mnras/stz2778 , 490, 4638

    2019 doi

  17. [25]

    Demory B.-O., et al., 2016, @doi [Nature] 10.1038/nature17169 , https://ui.adsabs.harvard.edu/abs/2016Natur.532..207D 532, 207

    2016 doi

  18. [26]

    B., Ghosh D

    Deng J., Du Z., Karki B. B., Ghosh D. B., Lee K. K. M., 2020, @doi [Nature Communications] 10.1038/s41467-020-15757-0 , 11, 2007

    2020 doi

  19. [27]

    Cycle 2, ID

    Diamond-Lowe H., et al., 2023, The Hot Rocks Survey: Testing 9 Irradiated Terrestrial Exoplanets for Atmospheres , JWST Proposal. Cycle 2, ID. \#3730

    2023

  20. [28]

    T., 2016, @doi [The Astrophysical Journal] 10.3847/0004-637X/822/1/24 , 822, 24

    Ding F., Pierrehumbert R. T., 2016, @doi [The Astrophysical Journal] 10.3847/0004-637X/822/1/24 , 822, 24

    2016 doi

  21. [29]

    Dorn C., Lichtenberg T., 2021, @doi [ ] 10.3847/2041-8213/ac33af , https://ui.adsabs.harvard.edu/abs/2021ApJ...922L...4D 922, L4

    2021 doi

  22. [30]

    E., Young E

    Doyle A. E., Young E. D., Klein B., Zuckerman B., Schlichting H. E., 2019, @doi [Science] 10.1126/science.aax3901 , https://ui.adsabs.harvard.edu/abs/2019Sci...366..356D 366, 356

    2019 doi

  23. [31]

    S., Mayne N

    Drummond B., Tremblin P., Baraffe I., Amundsen D. S., Mayne N. J., Venot O., Goyal J., 2016, @doi [Astronomy & Astrophysics] 10.1051/0004-6361/201628799 , 594, A69

    2016 doi

  24. [32]

    M., Slingo A., 1996, @doi [Quarterly Journal of the Royal Meteorological Society] 10.1002/qj.49712253107 , 122, 689

    Edwards J. M., Slingo A., 1996, @doi [Quarterly Journal of the Royal Meteorological Society] 10.1002/qj.49712253107 , 122, 689

    1996 doi

  25. [34]

    T., 2008b, @doi [Earth and Planetary Science Letters] 10.1016/j.epsl.2008.03.062 , https://ui.adsabs.harvard.edu/abs/2008E&PSL.271..181E 271, 181

    Elkins-Tanton L. T., 2008b, @doi [Earth and Planetary Science Letters] 10.1016/j.epsl.2008.03.062 , https://ui.adsabs.harvard.edu/abs/2008E&PSL.271..181E 271, 181

    2008 doi

  26. [35]

    Essack Z., Seager S., Pajusalu M., 2020, @doi [The Astrophysical Journal] 10.3847/1538-4357/ab9cba , 898, 160

    2020 doi

  27. [36]

    Feistel R., Wagner W., 2006, @doi [Journal of Physical and Chemical Reference Data] 10.1063/1.2183324 , https://ui.adsabs.harvard.edu/abs/2006JPCRD..35.1021F 35, 1021

    2006 doi

  28. [37]

    J., Bercovici D., Elkins-Tanton L

    Foley B. J., Bercovici D., Elkins-Tanton L. T., 2014, @doi [Journal of Geophysical Research: Solid Earth] https://doi.org/10.1002/2014JB011121 , 119, 8538

    2014 doi

  29. [38]

    B., Thompson J

    Fortin M.-A., Gazel E., Williams D. B., Thompson J. O., Kaltenegger L., Ramsey M. S., 2024, @doi [The Astrophysical Journal Letters] 10.3847/2041-8213/ad7d89 , 974, L7

    2024 doi

  30. [39]

    N., Butland J., 1984, @doi [SIAM Journal on Scientific and Statistical Computing] 10.1137/0905021 , 5, 300

    Fritsch F. N., Butland J., 1984, @doi [SIAM Journal on Scientific and Statistical Computing] 10.1137/0905021 , 5, 300

    1984 doi

  31. [40]

    S., et al., 2019, @doi [ ] 10.3847/2041-8213/aaffcd , https://ui.adsabs.harvard.edu/abs/2019ApJ...871L..26F 871, L26

    Froning C. S., et al., 2019, @doi [ ] 10.3847/2041-8213/aaffcd , https://ui.adsabs.harvard.edu/abs/2019ApJ...871L..26F 871, L26

    2019 doi

  32. [41]

    Gaillard F., et al., 2022, @doi [Earth and Planetary Science Letters] https://doi.org/10.1016/j.epsl.2021.117255 , 577, 117255

    2022

  33. [42]

    S., Zahnle K., Robinson T

    Gao P., Marley M. S., Zahnle K., Robinson T. D., Lewis N. K., 2017, @doi [The Astronomical Journal] 10.3847/1538-3881/aa5fab , 153, 139

    2017 doi

  34. [43]

    P., Sossi P

    Gillmann C., Hakim K., Lourenco D., Quanz S. P., Sossi P. A., 2024, @doi [Space: Science & Technology] 10.34133/space.0075 , 4, 0075

    2024 doi

  35. [44]

    Gillon M., et al., 2017, @doi [Nature] 10.1038/nature21360 , 542, 456

    2017 doi

  36. [45]

    D., Zahnle K

    Goldblatt C., Robinson T. D., Zahnle K. J., Crisp D., 2013, @doi [Nature Geoscience] 10.1038/ngeo1892 , 6, 661

    2013 doi

  37. [46]

    E., et al., 2022, @doi [Journal of Quantitative Spectroscopy and Radiative Transfer] 10.1016/j.jqsrt.2021.107949 , 277, 107949

    Gordon I. E., et al., 2022, @doi [Journal of Quantitative Spectroscopy and Radiative Transfer] 10.1016/j.jqsrt.2021.107949 , 277, 107949

    2022

  38. [47]

    J., Pierrehumbert R

    Graham R. J., Pierrehumbert R. T., 2024, @doi [The Astrophysical Journal] 10.3847/1538-4357/ad45fb , 970, 32

    2024 doi

  39. [48]

    J., Lichtenberg T., Boukrouche R., Pierrehumbert R

    Graham R. J., Lichtenberg T., Boukrouche R., Pierrehumbert R. T., 2021, @doi [The Planetary Science Journal] 10.3847/PSJ/ac214c , 2, 207

    2021 doi

  40. [49]

    P., Bell T

    Greene T. P., Bell T. J., Ducrot E., Dyrek A., Lagage P.-O., Fortney J. J., 2023, @doi [Nature] 10.1038/s41586-023-05951-7

    2023 doi

  41. [50]

    Gressier A., et al., 2024, @doi [ ] 10.3847/2041-8213/ad73d1 , https://ui.adsabs.harvard.edu/abs/2024ApJ...975L..10G 975, L10

    2024 doi

  42. [51]

    S., Nie N

    Grewal D. S., Nie N. X., Zhang B., Izidoro A., Asimow P. D., 2024, @doi [Nature Astronomy] 10.1038/s41550-023-02172-w , https://ui.adsabs.harvard.edu/abs/2024NatAs...8..290G 8, 290

    2024 doi

  43. [52]

    et al., 2018, @doi [A&A] 10.1051/0004-6361/201732233 , 613, A68

    Grimm, Simon L. et al., 2018, @doi [A&A] 10.1051/0004-6361/201732233 , 613, A68

    2018 doi

  44. [53]

    L., et al., 2021, @doi [The Astrophysical Journal Supplement Series] 10.3847/1538-4365/abd773 , https://ui.adsabs.harvard.edu/abs/2021ApJS..253...30G 253, 30

    Grimm S. L., et al., 2021, @doi [The Astrophysical Journal Supplement Series] 10.3847/1538-4365/abd773 , https://ui.adsabs.harvard.edu/abs/2021ApJS..253...30G 253, 30

    2021 doi

  45. [54]

    A., 2004, @doi [Solar Energy] 10.1016/j.solener.2003.08.039 , 76, 423

    Gueymard C. A., 2004, @doi [Solar Energy] 10.1016/j.solener.2003.08.039 , 76, 423

    2004 doi

  46. [55]

    2010, @doi [A&A] 10.1051/0004-6361/200913396 , 520, A27

    Guillot, T. 2010, @doi [A&A] 10.1051/0004-6361/200913396 , 520, A27

    2010 doi

  47. [56]

    M., Shorttle O., Jordan S., Rudge J

    Guimond C. M., Shorttle O., Jordan S., Rudge J. F., 2023, @doi [Monthly Notices of the Royal Astronomical Society] 10.1093/mnras/stad2486 , p. stad2486

    2023 doi

  48. [57]

    H., 2024, @doi [Nature Astronomy] 10.1038/s41550-024-02269-w , 8, 920

    Guo J. H., 2024, @doi [Nature Astronomy] 10.1038/s41550-024-02269-w , 8, 920

    2024 doi

  49. [58]

    T., 2024, @doi [ ] 10.3847/1538-4357/ad04e2 , https://ui.adsabs.harvard.edu/abs/2024ApJ...961...35H 961, 35

    Habib N., Pierrehumbert R. T., 2024, @doi [ ] 10.3847/1538-4357/ad04e2 , https://ui.adsabs.harvard.edu/abs/2024ApJ...961...35H 961, 35

    2024 doi

  50. [59]

    Hakim K., et al., 2021, @doi [The Planetary Science Journal] 10.3847/PSJ/abe1b8 , 2, 49

    2021 doi

  51. [60]

    L., 2015, @doi [The Astrophysical Journal] 10.1088/0004-637X/806/2/216 , 806, 216

    Hamano K., Kawahara H., Abe Y., Onishi M., Hashimoto G. L., 2015, @doi [The Astrophysical Journal] 10.1088/0004-637X/806/2/216 , 806, 216

    2015 doi

  52. [61]

    T., 2021, @doi [Proceedings of the National Academy of Sciences] 10.1073/pnas.2022705118 , 118

    Hammond M., Lewis N. T., 2021, @doi [Proceedings of the National Academy of Sciences] 10.1073/pnas.2022705118 , 118

    2021 doi

  53. [62]

    arXiv:2409.04386

    Hammond M., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2409.04386 , https://ui.adsabs.harvard.edu/abs/2024arXiv240904386H p. arXiv:2409.04386

    2024 doi arXiv

  54. [63]

    J., et al., 2019, @doi [Journal of Quantitative Spectroscopy and Radiative Transfer] https://doi.org/10.1016/j.jqsrt.2019.04.040 , 232, 35

    Hargreaves R. J., et al., 2019, @doi [Journal of Quantitative Spectroscopy and Radiative Transfer] https://doi.org/10.1016/j.jqsrt.2019.04.040 , 232, 35

    2019 doi

  55. [64]

    J., Tennyson J., Kaminsky B

    Harris G. J., Tennyson J., Kaminsky B. M., Pavlenko Y. V., Jones H. R. A., 2006, @doi [Monthly Notices of the Royal Astronomical Society] 10.1111/j.1365-2966.2005.09960.x , 367, 400

    2006

  56. [65]

    Hay H. C. F. C., Matsuyama I., 2019, @doi [ ] 10.3847/1538-4357/ab0c21 , https://ui.adsabs.harvard.edu/abs/2019ApJ...875...22H 875, 22

    2019 doi

  57. [66]

    Heng K., 2023, @doi [ ] 10.3847/2041-8213/acfe05 , https://ui.adsabs.harvard.edu/abs/2023ApJ...956L..20H 956, L20

    2023 doi

  58. [67]

    Hirschmann M., 2022, @doi [Geochimica et Cosmochimica Acta] https://doi.org/10.1016/j.gca.2022.04.005 , 328, 221

    2022 doi

  59. [68]

    o gstr \

    H \"o gstr \"o m U., 1988, @doi [Boundary-Layer Meteorology] 10.1007/BF00119875 , https://ui.adsabs.harvard.edu/abs/1988BoLMe..42...55H 42, 55

    1988 doi

  60. [69]

    Hu R., et al., 2024, @doi [Nature] 10.1038/s41586-024-07432-x , https://ui.adsabs.harvard.edu/abs/2024Natur.630..609H 630, 609

    2024 doi

  61. [70]

    M., Pepin R

    Hunten D. M., Pepin R. O., Walker J. C., 1987, @doi [Icarus] https://doi.org/10.1016/0019-1035(87)90022-4 , 69, 532

    1987 doi

  62. [71]

    T., 2023, @doi [ ] 10.3847/1538-4357/ace346 , https://ui.adsabs.harvard.edu/abs/2023ApJ...953..168I 953, 168

    Innes H., Tsai S.-M., Pierrehumbert R. T., 2023, @doi [ ] 10.3847/1538-4357/ace346 , https://ui.adsabs.harvard.edu/abs/2023ApJ...953..168I 953, 168

    2023 doi

  63. [72]

    P., Rae A

    Itcovitz J. P., Rae A. S. P., Citron R. I., Stewart S. T., Sinclair C. A., Rimmer P. B., Shorttle O., 2022, @doi [The Planetary Science Journal] 10.3847/PSJ/ac67a9 , 3, 115

    2022 doi

  64. [73]

    J., Woitke P., Herbort O., Min M., Chubb K

    Janssen L. J., Woitke P., Herbort O., Min M., Chubb K. L., Helling C., Carone L., 2023, @doi [Astronomische Nachrichten] 10.1002/asna.20230075 , https://ui.adsabs.harvard.edu/abs/2023AN....34430075J 344, e20230075

    2023 doi

  65. [74]

    P., Bartel M., Güdel M., 2021, @doi [Astronomy & Astrophysics] 10.1051/0004-6361/202038407 , 649, A96

    Johnstone C. P., Bartel M., Güdel M., 2021, @doi [Astronomy & Astrophysics] 10.1051/0004-6361/202038407 , 649, A96

    2021 doi

  66. [75]

    Joyce M., Tayar J., 2023, @doi [Galaxies] 10.3390/galaxies11030075 , 11, 75

    2023 doi

  67. [76]

    Kaltenegger L., Sasselov D., 2010, @doi [ ] 10.1088/0004-637X/708/2/1162 , https://ui.adsabs.harvard.edu/abs/2010ApJ...708.1162K 708, 1162

    2010 doi

  68. [77]

    A., 1987, @doi [Reviews of Geophysics] https://doi.org/10.1029/RG025i008p01609 , 25, 1609

    Kaye J. A., 1987, @doi [Reviews of Geophysics] https://doi.org/10.1029/RG025i008p01609 , 25, 1609

    1987 doi

  69. [78]

    Kite E. S., Jr. B. F., Schaefer L., Gaidos E., 2016, @doi [The Astrophysical Journal] 10.3847/0004-637X/828/2/80 , 828, 80

    2016 doi

  70. [79]

    A., et al., 2009, @doi [ ] 10.1088/0004-637X/690/1/822 , https://ui.adsabs.harvard.edu/abs/2009ApJ...690..822K 690, 822

    Knutson H. A., et al., 2009, @doi [ ] 10.1088/0004-637X/690/1/822 , https://ui.adsabs.harvard.edu/abs/2009ApJ...690..822K 690, 822

    2009 doi

  71. [80]

    Koll D. D. B., 2022, @doi [The Astrophysical Journal] 10.3847/1538-4357/ac3b48 , 924, 134

    2022 doi

  72. [81]

    L., 2011, @doi [Geophysical Research Letters] https://doi.org/10.1029/2010GL045777 , 38

    Kopp G., Lean J. L., 2011, @doi [Geophysical Research Letters] https://doi.org/10.1029/2010GL045777 , 38

    2011 doi

  73. [82]

    K., et al., 2013, @doi [The Astrophysical Journal] 10.1088/0004-637X/765/2/131 , 765, 131

    Kopparapu R. K., et al., 2013, @doi [The Astrophysical Journal] 10.1088/0004-637X/765/2/131 , 765, 131

    2013 doi

  74. [83]

    J., 2024, @doi [Nature Communications] 10.1038/s41467-024-52642-6 , 15, 8374

    Krissansen-Totton J., Wogan N., Thompson M., Fortney J. J., 2024, @doi [Nature Communications] 10.1038/s41467-024-52642-6 , 15, 8374

    2024 doi

  75. [84]

    Lebrun T., Massol H., Chassefière E., Davaille A., Marcq E., Sarda P., Leblanc F., Brandeis G., 2013, @doi [Journal of Geophysical Research: Planets] 10.1002/jgre.20068 , 118, 1155

    2013 doi

  76. [85]

    Lee E. K. H., Tan X., Tsai S.-M., 2024, @doi [Monthly Notices of the Royal Astronomical Society] 10.1093/mnras/stae537 , 529, 2686

    2024 doi

  77. [86]

    Lichtenberg T., 2021, @doi [The Astrophysical Journal Letters] 10.3847/2041-8213/ac0146 , 914, L4

    2021 doi

  78. [87]

    Lichtenberg T., Miguel Y., 2025, @doi [Treatise on Geochemistry] 10.1016/B978-0-323-99762-1.00122-4 , https://ui.adsabs.harvard.edu/abs/2025TrGeo...7...51L 7, 51

    2025 doi

  79. [88]

    J., Hammond M., Boukrouche R., Sanan P., Tsai S., Pierrehumbert R

    Lichtenberg T., Bower D. J., Hammond M., Boukrouche R., Sanan P., Tsai S., Pierrehumbert R. T., 2021, @doi [Journal of Geophysical Research: Planets] 10.1029/2020JE006711 , 126

    2021 doi

  80. [89]

    Lodders K., Fegley B., 1998, The planetary scientist's companion / Katharina Lodders, Bruce Fegley

    1998

  81. [90]

    S., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2409.16270 , https://ui.adsabs.harvard.edu/abs/2024arXiv240916270L p

    Loftus K., Luo Y., Fan B., Kite E. S., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2409.16270 , https://ui.adsabs.harvard.edu/abs/2024arXiv240916270L p. arXiv:2409.16270

    2024 doi arXiv

  82. [91]

    Malik M., et al., 2017, @doi [The Astronomical Journal] 10.3847/1538-3881/153/2/56 , 153, 56

    2017 doi

  83. [92]

    Met Office, Exeter, UK

    Manners J., et al., 2017, Technical report, SOCRATES Technical Guide: Suite Of Community RAdiative Transfer Codes Based on Edwards and Slingo. Met Office, Exeter, UK

    2017

  84. [93]

    N., Steinke T., Nimmo F., 2022, @doi [Elements] 10.2138/gselements.18.6.374 , 18, 374

    Matsuyama I. N., Steinke T., Nimmo F., 2022, @doi [Elements] 10.2138/gselements.18.6.374 , 18, 374

    2022 doi

  85. [94]

    G., Bower D

    Meier T. G., Bower D. J., Lichtenberg T., Hammond M., Tackley P. J., 2023, @doi [ ] 10.1051/0004-6361/202346950 , https://ui.adsabs.harvard.edu/abs/2023A&A...678A..29M 678, A29

    2023 doi

  86. [95]

    J., Payne V

    Mlawer E. J., Payne V. H., Moncet J. L., Delamere J. S., Alvarado M. J., Tobin D. C., 2012, @doi [Philosophical Transactions of the Royal Society of London Series A] 10.1098/rsta.2011.0295 , https://ui.adsabs.harvard.edu/abs/2012RSPTA.370.2520M 370, 2520

    2012

  87. [96]

    J., Cady-Pereira K

    Mlawer E. J., Cady-Pereira K. E., Mascio J., Gordon I. E., 2023, @doi [Journal of Quantitative Spectroscopy and Radiative Transfer] 10.1016/j.jqsrt.2023.108645 , https://ui.adsabs.harvard.edu/abs/2023JQSRT.30608645M 306, 108645

    2023

  88. [97]

    Namur O., Charlier B., Holtz F., Cartier C., McCammon C., 2016, @doi [Earth and Planetary Science Letters] https://doi.org/10.1016/j.epsl.2016.05.024 , 448, 102

    2016 doi

  89. [98]

    Nicholls H., 2024, Convective shutdown in the atmospheres of lava worlds, @doi 10.5281/zenodo.14273352 , https://doi.org/10.5281/zenodo.14273352

    2024 doi

  90. [99]

    Nicholls H., Hébrard E., Venot O., Drummond B., Evans E., 2023, @doi [Monthly Notices of the Royal Astronomical Society] 10.1093/mnras/stad1734 , 523, 5681

    2023 doi

  91. [100]

    J., Pierrehumbert R., 2024, Magma ocean evolution at arbitrary redox state ( @eprint arXiv 2411.19137 ), https://arxiv.org/abs/2411.19137

    Nicholls H., Lichtenberg T., Bower D. J., Pierrehumbert R., 2024, Magma ocean evolution at arbitrary redox state ( @eprint arXiv 2411.19137 ), https://arxiv.org/abs/2411.19137

    2024 arXiv

  92. [101]

    T., 2025, submitted to the Journal of Open Source Software

    Nicholls H., Lichtenberg T., Pierrehumbert R. T., 2025, submitted to the Journal of Open Source Software

    2025

  93. [102]

    W., Puchtel I

    Nicklas R. W., Puchtel I. S., Ash R. D., 2018, @doi [Geochimica et Cosmochimica Acta] https://doi.org/10.1016/j.gca.2017.11.002 , 222, 447

    2018 doi

  94. [103]

    A., Lee E

    Noti P. A., Lee E. K. H., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2409.17101 , https://ui.adsabs.harvard.edu/abs/2024arXiv240917101N p. arXiv:2409.17101

    2024 doi arXiv

  95. [104]

    E., 2019, @doi [Annual Review of Earth and Planetary Sciences] https://doi.org/10.1146/annurev-earth-053018-060246 , 47, 67

    Owen J. E., 2019, @doi [Annual Review of Earth and Planetary Sciences] https://doi.org/10.1146/annurev-earth-053018-060246 , 47, 67

    2019 doi

  96. [105]

    Parc L., Bouchy F., Venturini J., Dorn C., Helled R., 2024, @doi [ ] 10.1051/0004-6361/202449911 , https://ui.adsabs.harvard.edu/abs/2024A&A...688A..59P 688, A59

    2024 doi

  97. [106]

    Parmentier V., Showman A., Lian Y., 2013, @doi [A&A] 10.1051/0004-6361/201321132 , 558, A91

    2013 doi

  98. [107]

    A., et al., 2024, @doi [A&A] 10.1051/0004-6361/202450748 , 690, A159

    Patel J. A., et al., 2024, @doi [A&A] 10.1051/0004-6361/202450748 , 690, A159

    2024 doi

  99. [108]

    A., Kasting J

    Pavlov A. A., Kasting J. F., 2002, @doi [Astrobiology] 10.1089/153110702753621321 , https://ui.adsabs.harvard.edu/abs/2002AsBio...2...27P 2, 27

    2002 doi

  100. [109]

    Cambridge University Press, p

    Perryman M., 2011, Imaging. Cambridge University Press, p. 149–180

    2011

  101. [110]

    Cambridge University Press, Cambridge New York

    Pierrehumbert R., 2010, Principles of planetary climate. Cambridge University Press, Cambridge New York

    2010

  102. [111]

    T., Hammond M., 2019, @doi [Annual Review of Fluid Mechanics] 10.1146/annurev-fluid-010518-040516 , 51, 275

    Pierrehumbert R. T., Hammond M., 2019, @doi [Annual Review of Fluid Mechanics] 10.1146/annurev-fluid-010518-040516 , 51, 275

    2019 doi

  103. [112]

    Piette A. A. A., Gao P., Brugman K., Shahar A., Lichtenberg T., Miozzi F., Driscoll P., 2023, Rocky planet or water world? Observability of low-density lava world atmospheres, http://arxiv.org/abs/2306.10100

    2023 arXiv

  104. [113]

    D., Marley M

    Robinson T. D., Marley M. S., 2014, @doi [The Astrophysical Journal] 10.1088/0004-637X/785/2/158 , 785, 158

    2014 doi

  105. [114]

    C., Nimmo F., Melosh J., 2007, in Schubert G., ed., , Vol

    Rubie D. C., Nimmo F., Melosh J., 2007, in Schubert G., ed., , Vol. 9, Evolution of the Earth. pp 51--90, @doi 10.1016/B978-044452748-6.00140-1

    2007 doi

  106. [115]

    Salvador A., Massol H., Davaille A., Marcq E., Sarda P., Chassefi \`e re E., 2017, @doi [Journal of Geophysical Research (Planets)] 10.1002/2017JE005286 , https://ui.adsabs.harvard.edu/abs/2017JGRE..122.1458S 122, 1458

    2017 doi

  107. [116]

    Salvador A., et al., 2023, @doi [Space Sci Rev] 10.1007/s11214-023-00995-7 , https://ui.adsabs.harvard.edu/abs/2023SSRv..219...51S 219, 51

    2023 doi

  108. [117]

    Scarsdale N., et al., 2024, @doi [The Astronomical Journal] 10.3847/1538-3881/ad73cf , 168, 276

    2024 doi

  109. [118]

    T., 2018, @doi [Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences] 10.1098/rsta.2018.0109 , 376, 20180109

    Schaefer L., Elkins-Tanton L. T., 2018, @doi [Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences] 10.1098/rsta.2018.0109 , 376, 20180109

    2018

  110. [119]

    D., Berta-Thompson Z., Sasselov D., 2016, @doi [ ] 10.3847/0004-637X/829/2/63 , https://ui.adsabs.harvard.edu/abs/2016ApJ...829...63S 829, 63

    Schaefer L., Wordsworth R. D., Berta-Thompson Z., Sasselov D., 2016, @doi [ ] 10.3847/0004-637X/829/2/63 , https://ui.adsabs.harvard.edu/abs/2016ApJ...829...63S 829, 63

    2016 doi

  111. [120]

    Z., et al., 2024, @doi [The Astrophysical Journal] 10.3847/1538-4357/ad0b82 , 961, 22

    Seligman D. Z., et al., 2024, @doi [The Astrophysical Journal] 10.3847/1538-4357/ad0b82 , 961, 22

    2024 doi

  112. [121]

    Selsis F., Leconte J., Turbet M., Chaverot G., Bolmont A., 2023, @doi [Nature] 10.1038/s41586-023-06258-3 , 620, 287

    2023 doi

  113. [122]

    E., et al., 2023, @doi [Geoscientific Model Development] 10.5194/gmd-16-5601-2023 , 16, 5601

    Sergeev D. E., et al., 2023, @doi [Geoscientific Model Development] 10.5194/gmd-16-5601-2023 , 16, 5601

    2023 doi

  114. [123]

    Elsevier, Amsterdam, pp 91--119, @doi https://doi.org/10.1016/B978-044452748-6.00141-3 , https://www.sciencedirect.com/science/article/pii/B9780444527486001413

    Solomatov V., 2007, in Schubert G., ed., , Treatise on Geophysics. Elsevier, Amsterdam, pp 91--119, @doi https://doi.org/10.1016/B978-044452748-6.00141-3 , https://www.sciencedirect.com/science/article/pii/B9780444527486001413

    2007 doi

  115. [124]

    A., Burnham A

    Sossi P. A., Burnham A. D., Badro J., Lanzirotti A., Newville M., O’Neill H. S., 2020, @doi [Science Advances] 10.1126/sciadv.abd1387 , 6, eabd1387

    2020 doi

  116. [125]

    C., Sills A., 2013, @doi [The Astrophysical Journal] 10.1088/0004-637X/776/2/87 , 776, 87

    Spada F., Demarque P., Kim Y. C., Sills A., 2013, @doi [The Astrophysical Journal] 10.1088/0004-637X/776/2/87 , 776, 87

    2013 doi

  117. [126]

    W., Kitzmann D., Patzer A

    Stock J. W., Kitzmann D., Patzer A. B. C., Sedlmayr E., 2018, @doi [Monthly Notices of the Royal Astronomical Society] 10.1093/mnras/sty1531

    2018 doi

  118. [127]

    W., Kitzmann D., Patzer A

    Stock J. W., Kitzmann D., Patzer A. B. C., 2022, @doi [ ] 10.1093/mnras/stac2623 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.517.4070S 517, 4070

    2022 doi

  119. [128]

    S., Dalou C., Lichtenberg T., 2023, @doi [Frontiers in Earth Science] 10.3389/feart.2023.1159412 , https://ui.adsabs.harvard.edu/abs/2023FrEaS..1159412S 11, 1159412

    Suer T.-A., Jackson C., Grewal D. S., Dalou C., Lichtenberg T., 2023, @doi [Frontiers in Earth Science] 10.3389/feart.2023.1159412 , https://ui.adsabs.harvard.edu/abs/2023FrEaS..1159412S 11, 1159412

    2023

  120. [129]

    W., Hunten D

    Taylor F. W., Hunten D. M., 2014, in Spohn T., Breuer D., Johnson T. V., eds, , Encyclopedia of the Solar System (Third Edition), third edition edn, Elsevier, Boston, pp 305--322, @doi https://doi.org/10.1016/B978-0-12-415845-0.00014-1 , https://www.sciencedirect.com/science/a...

    2014 doi

  121. [130]

    B., Melosh H

    Tonks W. B., Melosh H. J., 1993, @doi [Journal of Geophysical Research: Planets] https://doi.org/10.1029/92JE02726 , 98, 5319

    1993 doi

  122. [131]

    B., Turco R

    Toon O. B., Turco R. P., Pollack J. B., 1982, @doi [ ] 10.1016/0019-1035(82)90089-6 , https://ui.adsabs.harvard.edu/abs/1982Icar...51..358T 51, 358

    1982 doi

  123. [132]

    B., Tailby N

    Trail D., Watson E. B., Tailby N. D., 2011, @doi [Nature] 10.1038/nature10655 , 480, 79

    2011 doi

  124. [133]

    E., 1992, Climate system modeling

    Trenberth K. E., 1992, Climate system modeling. Cambridge University Press

    1992

  125. [134]

    R., Fateev A., Lee E., Heng K., 2021, @doi [The Astrophysical Journal] 10.3847/1538-4357/ac29bc , 923, 264

    Tsai S.-M., Malik M., Kitzmann D., Lyons J. R., Fateev A., Lee E., Heng K., 2021, @doi [The Astrophysical Journal] 10.3847/1538-4357/ac29bc , 923, 264

    2021 doi

  126. [135]

    Turbet M., Bolmont E., Chaverot G., Ehrenreich D., Leconte J., Marcq E., 2021, @doi [Nature] 10.1038/s41586-021-03873-w , 598, 276

    2021 doi

  127. [136]

    H., Henning W

    Tyler R. H., Henning W. G., Hamilton C. W., 2015, @doi [The Astrophysical Journal Supplement Series] 10.1088/0067-0049/218/2/22 , 218, 22

    2015 doi

  128. [137]

    S., Tennyson J., Yurchenko S

    Underwood D. S., Tennyson J., Yurchenko S. N., Huang X., Schwenke D. W., Lee T. J., Clausen S., Fateev A., 2016, @doi [Monthly Notices of the Royal Astronomical Society] 10.1093/mnras/stw849 , 459, 3890

    2016 doi

  129. [138]

    Van Buchem C. P. A., Miguel Y., Zilinskas M., van Westrenen W., 2023, LavAtmos : An open source chemical equilibrium vaporisation code for lava worlds, http://arxiv.org/abs/2210.10463

    2023 arXiv

  130. [139]

    Wagner W., Pru A., 2002, @doi [Journal of Physical and Chemical Reference Data] 10.1063/1.1461829 , https://ui.adsabs.harvard.edu/abs/2002JPCRD..31..387W 31, 387

    2002 doi

  131. [140]

    S., Lineweaver C

    Wang H. S., Lineweaver C. H., Ireland T. R., 2018, @doi [Icarus] https://doi.org/10.1016/j.icarus.2017.08.024 , 299, 460

    2018 doi

  132. [141]

    H., 1985, @doi [Annual Review of Earth and Planetary Sciences] https://doi.org/10.1146/annurev.ea.13.050185.001221 , 13, 201

    Warren P. H., 1985, @doi [Annual Review of Earth and Planetary Sciences] https://doi.org/10.1146/annurev.ea.13.050185.001221 , 13, 201

    1985

  133. [142]

    J., Del Genio A

    Way M. J., Del Genio A. D., Kiang N. Y., Sohl L. E., Grinspoon D. H., Aleinov I., Kelley M., Clune T., 2016, @doi [ ] 10.1002/2016GL069790 , https://ui.adsabs.harvard.edu/abs/2016GeoRL..43.8376W 43, 8376

    2016 doi

  134. [143]

    J., et al., 2021, @doi [The Astrophysical Journal] 10.3847/1538-4357/abe771 , 911, 18

    Wilson D. J., et al., 2021, @doi [The Astrophysical Journal] 10.3847/1538-4357/abe771 , 911, 18

    2021 doi

  135. [144]

    Yoshida T., Terada N., Kuramoto K., 2024, @doi [Progress in Earth and Planetary Science] 10.1186/s40645-024-00666-3 , 11, 59

    2024 doi

  136. [145]

    J., Kasting J

    Zahnle K. J., Kasting J. F., 2023, @doi [Geochimica et Cosmochimica Acta] https://doi.org/10.1016/j.gca.2023.09.023 , 361, 228

    2023 doi

  137. [146]

    Zhang M., et al., 2022, @doi [ ] 10.3847/1538-3881/ac3f3b , https://ui.adsabs.harvard.edu/abs/2022AJ....163...68Z 163, 68

    2022 doi

  138. [147]

    Zieba S., et al., 2023, @doi [Nature] 10.1038/s41586-023-06232-z

    2023 doi

  139. [148]

    Zilinskas M., Miguel Y., van Buchem C. P. A., Snellen I. A. G., 2023, @doi [A&A] 10.1051/0004-6361/202245521 , 671

    2023 doi

  140. [149]

    write newline

    " write newline "" before.all 'output.state := FUNCTION fin.entry write newline FUNCTION new.block output.state before.all = 'skip after.block 'output.state := if FUNCTION new.sentence output.state after.block = 'skip output.state before.all = 'skip after.sentence 'output.stat...

Pith tools

Reviewed August 11, 2026 · model on record in the stance chip above.