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REVIEW 3 major objections 8 minor 1 cited by

Absence of a Runaway Greenhouse Limit on Lava Planets

T0 review · 3 major / 8 minor · reviewed 2026-08-15 · deepseek-v4-flash

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Pith's one-line read This paper argues that multi-species atmospheres above magma oceans lack a runaway greenhouse radiation cap, so instellation alone cannot set the inner edge of the habitable zone for such planets.

desk verdict Molten-mantle volatile coupling erases the steam runaway plateau for hot lava planets, but the 'no limit at all' claim overreaches because the open-degassing model assumes 100% melt where crystallization would thicken the atmosphere. read the letter →

arxiv 2505.11149 v1 pith:YGHQ4I64 submitted 2025-05-16 astro-ph.EP

Iris D. Boer , Harrison Nicholls , Tim Lichtenberg This is my paper · ORCID
classification astro-ph.EP
keywords runawaygreenhouseoutgoinglong-waveradiationmagmaoceanvolatiledissolutionredoxstatehabitablezonelavaplanetsatmosphericequilibriumchemistry
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 tries to overturn a long-standing climate rule: the idea that every rocky planet has a maximum outgoing thermal radiation, a runaway greenhouse limit, that lets astronomers define the inner edge of the habitable zone by stellar irradiation alone. It shows that once the atmosphere is allowed to equilibrate with a molten mantle, water is partly dissolved into the magma, and the remaining gas becomes a redox-dependent mixture of CO2, CO, H2, CH4, and N2. In every such multi-species case the paper models, outgoing long-wave radiation rises smoothly with surface temperature instead of flattening into the plateau that pure-steam atmospheres produce. If true, a lava planet's climate is set by its interior oxidation state and volatile budget, not just by how much starlight it receives, and initially molten planets cool along paths that never return to the climates of solidified planets heated from outside.

What carries the argument

The load-bearing mechanism is the coupled magma-ocean–atmosphere equilibrium, computed by balancing volatile dissolution into the melt against redox equilibrium chemistry, then feeding the resulting surface composition into a multi-component non-dilute pseudoadiabat and a two-stream correlated-k radiative transfer calculation. The oxygen fugacity relative to the iron–wüstite buffer sets whether the atmosphere is CO2-dominated, CO-dominated, H2/CO-dominated, or CH4-dominated, while the melt fraction sets how much volatile mass is sequestered in the interior. The combination removes the water-rich saturated region that created the radiation plateau.

What would settle it

Run the same model with a radiative layer or cloud formation included, or with a crystallization-coupled melt fraction, and check whether outgoing long-wave radiation versus surface temperature regains a flat plateau between roughly 900 and 1750 K; if it does, the claimed absence of a runaway greenhouse threshold does not hold for those conditions.

Watch

Extended reading notes

Core claim

The central claim, stated in the conclusions, is that atmospheres with multi-species compositions situated above magma oceans do not exhibit a runaway greenhouse threshold at all. The paper reproduces the classic pure-steam plateau with its model, validating the method, then shows the plateau disappears when three ingredients are added: dissolution of volatiles into a molten or partially molten mantle, a six-species H-C-N-O compositional space, and surface-temperature- and redox-dependent equilibrium chemistry. The reason is that the plateau in pure steam comes from water's strong infrared opacity and high dew point pinning the radiating level to a moist pseudoadiabat; magma-ocean dissolution removes water from the gas phase, and redox chemistry replaces it with gases whose condensation and opacity behaviour is different. As a direct consequence, the outgoing long-wave radiation is controlled by the redox and melting state of the mantle, and stellar irradiation alone cannot define where liquid water is possible on such planets.

Load-bearing premise

The result assumes a fully convective, cloud-free, stratosphere-free atmosphere with complete rain-out of condensibles, and assumes a fully molten mantle that stays in chemical equilibrium with the atmosphere at every surface temperature, even below the roughly 1200–1400 K range where crystallization is expected and surface temperature and melt fraction decouple.

Editorial extensions

If this is right

  • The inner edge of the classical habitable zone cannot be derived from instellation alone for planets with molten surfaces; surface conditions require knowing the volatile endowment, redox state, and melting phase of the mantle.
  • Initially molten planets cooling from a magma ocean do not pass through the same climate states as solidified planets heated by rising stellar flux, so steady-state climate models cannot recover the evolutionary hysteresis the paper identifies.
  • Magma ocean cooling rates change: hydrogen-rich atmospheres keep outgoing radiation low and can prolong the molten phase, while oxidized, carbon-poor atmospheres radiate more efficiently and may shorten it.
  • The scale-height inflation signature that pure-steam runaway models predict for steam atmospheres should be erased for lava planets, which is testable with transmission spectroscopy of young rocky exoplanets.

Reading between the lines

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

  • If the no-plateau result survives the missing physics of clouds, radiative zones, and fractional crystallization, the term 'runaway greenhouse limit' would be better understood as a property of water-rich planets with solid surfaces rather than a universal rocky-planet cap.
  • A concrete extension of the paper's parameter sweep would map the critical melt fraction below which the OLR plateau reappears; that boundary in melt fraction–redox space would tell observers which planets can still be classified by irradiation.
  • The paper's two degassing scenarios bracket the likely real path, but the actual climate trajectory needs a time-dependent model that follows crystallization and volatile reprocessing; such a model would test whether the hysteresis the authors infer is as large as the steady-state comparison suggests.
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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

3 major / 8 minor

Summary. The paper uses a 1D radiative-convective model (JANUS in PROTEUS) with equilibrium chemistry and volatile dissolution into a magma ocean to compute the outgoing long-wave radiation (OLR) as a function of surface temperature for multi-component H-C-N-O atmospheres on rocky planets with molten mantles. It first validates the pure-steam limit against Kopparapu et al. (2013) and Selsis et al. (2023), then considers two degassing scenarios: a quenched scenario with composition fixed at 2000 K and an open scenario in which the atmosphere re-equilibrates with a fully molten mantle at every surface temperature. The central result is that the open-scenario multi-component atmospheres above magma oceans yield monotonically increasing OLR with no plateau, in contrast to the pure-steam runaway greenhouse limit, and the authors conclude that irradiation alone cannot define the inner edge of the habitable zone for such planets. The paper also emphasizes redox control of atmospheric composition and argues for evolutionary hysteresis between initially molten and solidified planets.

Significance. If the central claim survives scrutiny, it is significant: it would challenge the use of a pure-steam OLR plateau as a universal inner-edge criterion and would place interior state and redox chemistry at the center of rocky-planet climate classification. The study has several strengths: the pure-steam baseline is benchmarked against two independent published models, the parameter scans across redox state and volatile inventory are broad, and the model outputs are archived on Zenodo. The OLR curves are not constructed to fit the claimed result, and the validation case shows that the model reproduces the canonical plateau for a solid, pure-steam atmosphere. The main risk is that the absence of a plateau is demonstrated only under the assumption of a fully molten mantle at all surface temperatures, which is not physically justified in the temperate regime where the habitable-zone implication matters.

major comments (3)
  1. [Section 4.3 and Figure 5] The open-scenario OLR curves in Figure 5 assume a 100% molten mantle at every surface temperature, including temperatures below the ~1200-1400 K liquidus that the authors themselves cite in Section 4.3. In this regime crystallization will exsolve volatiles into the remaining melt and atmosphere, increasing surface pressure and opacity; the pure-steam cases in Figure 3A show that a 0% melt fraction produces a plateau, and the mixed-composition 0% melt case overlaps the pure-steam curve (Section 3.1). The low-temperature portion of Figure 5, which is the regime relevant to the habitable-zone inner edge, is therefore not a physically representative lava-planet calculation, and the abstract and Section 5 statements that such atmospheres 'do not exhibit a runaway greenhouse threshold at all' are not supported for Ts below the liquidus.
  2. [Section 2.3 and 4.3] The fully convective, cloud-free, stratosphere-free atmosphere is a load-bearing assumption for the no-plateau conclusion. The authors acknowledge in Section 4.3 that Selsis et al. (2023) argued for a radiative zone in equilibrium steam atmospheres and that this model 'cannot assess the impact of radiative zones.' If a radiative zone forms above a magma ocean, the upper-atmosphere temperature can decouple from the surface, which is precisely the mechanism that creates an OLR plateau in the canonical runaway greenhouse picture. Until the convective assumption is tested for the outgassed multi-component compositions, the conclusion that the thermal limit is absent 'at all' remains conditional on this assumption.
  3. [Section 3.1 and Figure 3B] The demonstration that mixed-composition atmospheres lack a plateau is limited to the specific end-member degassing scenarios and volatile inventories used in the paper. The melt-fraction comparison in Figure 3B is shown for one redox state (ΔIW+4) and one volatile inventory, and the Figure 5 scans all use either the quenched composition fixed at 2000 K or the open scenario with 100% melt. A planet that degasses additional volatiles during crystallization would have a different, potentially thicker atmosphere at low surface temperatures, and the authors' own quenched/open comparison in Section 3.3 shows deviations of up to 75 W/m2 at 600 K. The paper should state more explicitly that the absence of a plateau is a property of these equilibrium end-member scenarios, not a demonstrated general property of all magma-ocean atmospheres.
minor comments (8)
  1. [Section 5] In the conclusions, 'a accounting for temperature dependent atmospheric chemistry' should be 'an accounting for' or simply 'accounting for.'
  2. [Section 4.1.3] The phrase 'quenched quenched scenario' contains a duplicated word.
  3. [Equations (2), (4), and (6)] The equilibrium constant expressions appear to be missing superscripts in the typeset draft; as printed, expressions such as '3.039 × 104 T − 13152' are ambiguous and should be typeset with 10^4/T.
  4. [Section 3.1] The sentence 'reaching 376 bar for the 0% melt fraction, 95 bar for 0% melt fraction, and 82.7 bar for 100% melt fraction at 2000 K' likely should read '95 bar for the 50% melt fraction'; the second '0%' appears to be a typo.
  5. [Section 3.2] The text states that CH4-dominated atmospheres occur 'at 500 and 100 K,' but the context and Figure 4 axis suggest this should be '1000 K.'
  6. [Figure 3 caption] The caption refers to 'Models from (A) are shown for comparison purposes as faint dashed lines,' while the text says 'the blue dashed and solid lines almost completely overlap'; please clarify which lines are pure-steam and which are mixed-composition in panel B.
  7. [References] The Pierrehumbert (2010) reference is listed twice in the reference list, and the Lebrun et al. reference contains a formatting artifact ('Chassefi` eRe').
  8. [Footnote 1] The Zenodo archive is mentioned but not described; please state what is archived (model output, scripts, input files) to enable reproduction.

Circularity Check

0 steps flagged · score 0.0 of 10

No circularity: the OLR curves are computed from external equilibrium-chemistry, solubility, and opacity inputs and are benchmarked against independent pure-steam models, so the no-plateau result is not an input repackaged as a prediction.

full rationale

The derivation chain is self-contained rather than circular. The OLR values are outputs of a radiative-transfer calculation (SOCRATES with HITRAN2020 opacities) driven by surface partial pressures obtained from equilibrium chemistry (JANAF/IVTANTHERMO constants) and experimentally calibrated solubility laws, with no parameter fitted to the claimed no-plateau behavior. The pure-steam, solid-surface case is explicitly benchmarked against Kopparapu et al. (2013) and Selsis et al. (2023) and reproduces the canonical runaway-greenhouse plateau, demonstrating that the model is not constructed to erase the plateau by assumption. The plateau disappears only after adding a magma-ocean dissolution sink and multi-species H-C-N-O chemistry, both of which are external physical inputs. Self-citations to PROTEUS, JANUS, and CALLIOPE (Lichtenberg et al. 2021; Nicholls et al. 2024; Graham et al. 2021, 2022; Bower et al. 2022; Shorttle et al. 2024) concern modeling infrastructure and previously published methods rather than the no-plateau conclusion itself, and no uniqueness theorem or self-citation chain is invoked to forbid alternatives. The limitation stated in Section 4.3 — that assuming 100% melt fraction affects results below 1200–1400 K when basaltic rocks crystallize — is a disclosed applicability caveat, not a fitted input renamed as a prediction; it weakens confidence in the low-temperature habitable-zone inference but does not make the derivation circular. Therefore the appropriate finding is no significant circularity.

Assumptions & free parameters 4 free parameters · 5 assumptions · 0 invented entities

The paper introduces no new physical entities. Its main result rests on model inputs and assumptions; volatile budgets and redox states are scanned, not tuned to recover the absent plateau. The most fragile inputs are the experimental solubility laws and the convective/cloud-free atmospheric structure.

free parameters (4)
  • Volatile inventory ([H], [C/H], [N]) = Default [H] = 1 Earth ocean, [C/H] = 1, [N] = 2.8 ppmw; varied
    Boundary conditions for the equilibrium chemistry; chosen from Earth-like values and varied across orders of magnitude. Central OLR curves depend on these choices.
  • Redox state ΔIW = Varied from -4 to +4
    Mantle oxygen fugacity sets equilibrium speciation. The no-plateau result appears across the range, but quantitative OLR is redox-dependent.
  • Melt fraction = 0%, 50%, 100%
    Controls volatile dissolution into the magma ocean; the plateau disappears for the 50% and 100% melt cases.
  • Quench temperature for quenched scenario = 2000 K
    Fixed composition temperature for the quenched end-member; chosen, not fitted.
assumptions (5)
  • domain assumption Equilibrium constants for redox reactions from JANAF and IVTANTHERMO (Section 2.2).
    The atmospheric speciation is computed from these empirical thermodynamic constants.
  • domain assumption Experimental volatile solubility laws for H2O, CO2, CO, N2 and CH4 in magma (Section 2.2).
    Dissolution into the magma ocean, which drives the thin atmospheres, relies on these measured solubilities.
  • domain assumption H2 solubility is neglected because it is more than two orders of magnitude lower than H2O solubility (Section 2.2).
    This affects reducing, H2-rich atmospheres, where H2 could be more abundant and its dissolution could matter.
  • domain assumption Fully convective, cloud-free, stratosphere-free atmosphere with full rain-out of condensibles, using the multi-species pseudoadiabat (Sections 2.3 and 4.3).
    This is the same assumption used in canonical runaway-greenhouse models, but it is load-bearing for the OLR curves.
  • standard math Two-stream, correlated-k, plane-parallel radiative transfer with HITRAN2020 opacities (Section 2.3).
    Standard radiative transfer approximations; the OLR is independent of incoming stellar radiation under these assumptions.

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Cite this review

Pith. "Pith review of Absence of a Runaway Greenhouse Limit on Lava Planets." pith.science (2026). https://pith.science/paper/YGHQ4I64

@misc{pith2026250511149,
  author       = {Pith},
  title        = {Pith review of: Absence of a Runaway Greenhouse Limit on Lava Planets},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/YGHQ4I64}},
  note         = {Machine review of arXiv:2505.11149}
}
read the original abstract

Climate transitions on exoplanets offer valuable insights into the atmospheric processes governing planetary habitability. Previous pure-steam atmospheric models show a thermal limit in outgoing long-wave radiation, which has been used to define the inner edge of the classical habitable zone and guide exoplanet surveys aiming to identify and characterize potentially habitable worlds. We expand upon previous modelling by treating (i) the dissolution of volatiles into a magma ocean underneath the atmosphere, (ii) a broader volatile range of the atmospheric composition including H2O, CO2, CO, H2, CH4 and N2, and (iii) a surface temperature- and mantle redox-dependent equilibrium chemistry. We find that multi-component atmospheres of outgassed composition located above partially or fully-molten mantles do not exhibit the characteristic thermal radiation limit that arises from pure-steam models, thereby undermining the canonical concept of a runaway greenhouse limit, and hence challenging the conventional approach of using it to define an irradiation-based habitable zone. Our results show that atmospheric heat loss to space is strongly dependent on the oxidation and melting state of the underlying planetary mantle, through their significant influence on the atmosphere's equilibrium composition. This suggests an evolutionary hysteresis in climate scenarios: initially molten and cooling planets do not converge to the same climate regime as solidified planets that heat up by external irradiation. Steady-state models cannot recover evolutionary climate transitions, which instead require self-consistent models of the temporal evolution of the coupled feedback processes between interior and atmosphere over geologic time.

Figures

Figures reproduced from arXiv: 2505.11149 by the authors.

Figure 1
Figure 1. T-P profiles showing the atmospheres established at various surface temperatures (line color) and redox states (line style). The steep line that all profiles follow in the upper atmospheres are due to the saturation vapour pres￾sure curve. Saturation vapour pressure curves of different included volatiles are shown with dotted lines (Pierrehum￾bert 2010). At deeper levels (higher pressures), the profiles follow the d… view at source ↗
Figure 2
Figure 2. Illustration of the two different degassing scenarios used in this work, which bracket the potential pathways of mantle melting and crystallization of planetary evolution. The range of orange colours corresponds to temperatures as defined on the bottom abscissa. The figures contain T-P profiles that are shown in black, with a surface temperature as defined by their lowermost endpoint; the corresponding black-body ra… view at source ↗
Figure 3
Figure 3. T-P profiles showing the atmospheres established at various surface temperatures above a planetary interior with different melt fractions (line color). Outgoing long-wave radiation (OLR) for various surface temperatures, melt fractions, and chemical equilibrium compositions. (A) Pure-steam atmospheres above planetary interiors with different melt fractions of 0% (blue), 50% (orange) and 100% (red), with [H] = 1 Eart… view at source ↗
Figures from the paper (2 more)
Figure 4
Figure 4. Figure 4: Atmospheric composition (volume mixing ratio) above a magma ocean for different redox states and surface temper￾atures. The total pressure (in bar) of each atmosphere is given above the corresponding pie chart. Other parameters are kept at the default parameter values …
Figure 5
Figure 5. Figure 5: OLR vs. surface temperature for varied atmospheric equilibrium compositions. Graphs left to right show variations on C/H ratio (first row, A/B/C), H budget (second row, D/E/F) and N budget (third row, G/H/I) for different redox states (∆IW). Colours denote the volatile…

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    astro-ph.EP 2025-05 conditional novelty 7.0 of 10

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Reference graph

Works this paper leans on

109 extracted references · 7 canonical work pages · cited by 1 Pith paper

  1. [1]

    ֮ F "Ϥ 6] ޡM mk Kk?0OsҪQՆ'/AWK9 BK)

    thebibliography [1] 20pt to REFERENCES 6pt =0pt 10pt plus 3pt =0pt =0pt =1pt plus 1pt =0pt =0pt -12pt =13pt plus 1pt =20pt =13pt plus 1pt \@M =10000 =-1.0em =0pt =0pt 0pt =0pt =1.0em @enumiv\@empty 10000 10000 `\.\@m \@noitemerr \@latex@warning Empty `thebibliography' environment \@ifnextchar \@reference \@latexerr Missing key on reference command Each re...

    1998

  2. [2]

    1985, Journal of Geophysical Research: Solid Earth, 90, C545

    Abe, Y., & Matsui, T. 1985, Journal of Geophysical Research: Solid Earth, 90, C545

    1985

  3. [3]

    1988, Journal of the Atmospheric Sciences, 45, 3081, 10.1175/1520-0469(1988)045<3081:EOAIGH>2.0.CO;2

    Abe , Y., & Matsui , T. 1988, Journal of the Atmospheric Sciences, 45, 3081, 10.1175/1520-0469(1988)045<3081:EOAIGH>2.0.CO;2

    doi:10.1175/1520-0469(1988)045 1988

  4. [4]

    2013, , 558, 1, 10.1051/0004-6361/201321690

    Alibert, Y., Carron, F., Fortier, A., et al. 2013, , 558, 1, 10.1051/0004-6361/201321690

    doi:10.1051/0004-6361/201321690 2013

  5. [5]

    L., et al

    Andrault , D., Bolfan-Casanova , N., Nigro , G. L., et al. 2011, EPSL, 304, 251, 10.1016/j.epsl.2011.02.006

    doi:10.1016/j.epsl.2011.02.006 2011

  6. [6]

    2013, Geochimica et Cosmochimica Acta, 114, 52, https://doi.org/10.1016/j.gca.2013.03.028

    Ardia, P., Hirschmann, M., Withers, A., & Stanley, B. 2013, Geochimica et Cosmochimica Acta, 114, 52, https://doi.org/10.1016/j.gca.2013.03.028

    doi:10.1016/j.gca.2013.03.028 2013

  7. [7]

    S., Hirschmann, M

    Armstrong, L. S., Hirschmann, M. M., Stanley, B. D., Falksen, E. G., & Jacobsen, S. D. 2015, Geochimica et Cosmochimica Acta, 171, 283

    2015

  8. [8]

    2024, arXiv e-prints, arXiv:2403.03325, 10.48550/arXiv.2403.03325

    Benneke , B., Roy , P.-A., Coulombe , L.-P., et al. 2024, arXiv e-prints, arXiv:2403.03325, 10.48550/arXiv.2403.03325

    arXiv doi:10.48550/arxiv.2403.03325 2024

Show all 109 references
  1. [9]

    J., Timpe , M

    Bonati , I., Lichtenberg , T., Bower , D. J., Timpe , M. L., & Quanz , S. P. 2019, , 621, A125, 10.1051/0004-6361/201833158

    2019 doi

  2. [10]

    Bonati , I., & Ramirez , R. M. 2021, , 504, 1029, 10.1093/mnras/stab891

    2021 doi

  3. [11]

    E., & Ricard , Y

    Boukar \'e , C. E., & Ricard , Y. 2017, Geochemistry, Geophysics, Geosystems, 18, 3385, 10.1002/2017GC006902

    2017 doi

  4. [12]

    Boukrouche, R., Lichtenberg, T., & Pierrehumbert, R. T. 2021, The Astrophysical journal, 919, 130, 10.3847/1538-4357/ac1345

    2021 doi

  5. [13]

    J., Hakim, K., Sossi, P

    Bower, D. J., Hakim, K., Sossi, P. A., & Sanan, P. 2022, The Planetary Science Journal, 3, 93, 10.3847/psj/ac5fb1

    2022 doi

  6. [14]

    J., Kitzmann, D., Wolf, A

    Bower, D. J., Kitzmann, D., Wolf, A. S., et al. 2019, Astronomy & Astrophysics, 631, A103

    2019

  7. [15]

    M., Righter , K., Dauphas , N., et al

    Canup , R. M., Righter , K., Dauphas , N., et al. 2023, Reviews in Mineralogy and Geochemistry, 89, 53, 10.2138/rmg.2023.89.02

    2023 doi

  8. [16]

    2024, arXiv e-prints, arXiv:2410.13457, 10.48550/arXiv.2410.13457

    Cesario , L., Lichtenberg , T., Alei , E., et al. 2024, arXiv e-prints, arXiv:2410.13457, 10.48550/arXiv.2410.13457

    2024 doi arXiv

  9. [17]

    2021, Chemie der Erde / Geochemistry, 81, 125735, 10.1016/j.chemer.2020.125735

    Chao , K.-H., deGraffenried , R., Lach , M., et al. 2021, Chemie der Erde / Geochemistry, 81, 125735, 10.1016/j.chemer.2020.125735

    2021

  10. [18]

    1998, American Institute of Physics, -1

    Chase, M. 1998, American Institute of Physics, -1

    1998

  11. [19]

    2022, , 658, A40, 10.1051/0004-6361/202142286

    Chaverot , G., Turbet , M., Bolmont , E., & Leconte , J. 2022, , 658, A40, 10.1051/0004-6361/202142286

    2022 doi

  12. [20]

    S., Kaib , N

    Clement , M. S., Kaib , N. A., & Chambers , J. E. 2020, , 1, 18, 10.3847/PSJ/ab91aa

    2020 doi

  13. [21]

    2022, , 336, 291, 10.1016/j.gca.2022.09.012

    Dasgupta , R., Falksen , E., Pal , A., & Sun , C. 2022, , 336, 291, 10.1016/j.gca.2022.09.012

    2022 doi

  14. [22]

    D., Yin , Q

    Debaille , V., Brandon , A. D., Yin , Q. Z., & Jacobsen , B. 2007, , 450, 525, 10.1038/nature06317

    2007 doi

  15. [23]

    E., & Pan, V

    Dixon, J. E., & Pan, V. 1995, American Mineralogist, 80, 1339, 10.2138/am-1995-11-1224

    1995 doi

  16. [24]

    2021, , 922, L4, 10.3847/2041-8213/ac33af

    Dorn , C., & Lichtenberg , T. 2021, , 922, L4, 10.3847/2041-8213/ac33af

    2021 doi

  17. [25]

    E., & Barnes , R

    Driscoll , P. E., & Barnes , R. 2015, Astrobiology, 15, 739, 10.1089/ast.2015.1325

    2015

  18. [26]

    M., & Slingo , A

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

    1996 doi

  19. [27]

    2008, Earth and Planetary Science Letters, 271, 181, 10.1016/j.epsl.2008.03.062

    Elkins-Tanton, L. 2008, Earth and Planetary Science Letters, 271, 181, 10.1016/j.epsl.2008.03.062

    2008 doi

  20. [28]

    2021, , 656, A69, 10.1051/0004-6361/202038553

    Emsenhuber, A., Mordasini, C., Burn, R., et al. 2021, , 656, A69, 10.1051/0004-6361/202038553

    2021 doi

  21. [29]

    2025, , 979, 133, 10.3847/1538-4357/ad9b93

    Farhat , M., Auclair-Desrotour , P., Bou \'e , G., Lichtenberg , T., & Laskar , J. 2025, , 979, 133, 10.3847/1538-4357/ad9b93

    2025 doi

  22. [30]

    D., Zahnle , K

    Goldblatt , C., Robinson , T. D., Zahnle , K. J., & Crisp , D. 2013, Nature Geoscience, 6, 661, 10.1038/ngeo1892

    2013 doi

  23. [31]

    E., Rothman , L

    Gordon , I. E., Rothman , L. S., Hargreaves , R. J., et al. 2022, , 277, 107949, 10.1016/j.jqsrt.2021.107949

    2022

  24. [32]

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

    Graham , R. J., Lichtenberg , T., Boukrouche , R., & Pierrehumbert , R. T. 2021, , 2, 207, 10.3847/PSJ/ac214c

    2021 doi

  25. [33]

    J., Lichtenberg , T., & Pierrehumbert , R

    Graham , R. J., Lichtenberg , T., & Pierrehumbert , R. T. 2022, J Geophys Res Planets, 127, e2022JE007456, 10.1029/2022JE007456

    2022 doi

  26. [34]

    2013, , 497, 607, 10.1038/nature12163

    Hamano , K., Abe , Y., & Genda , H. 2013, , 497, 607, 10.1038/nature12163

    2013 doi

  27. [35]

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

    2015 doi

  28. [36]

    R., Millman, K

    Harris, C. R., Millman, K. J., Van Der Walt, S. J., et al. 2020, Nature, 585, 357

    2020

  29. [37]

    Hart , M. H. 1978, Icarus, 33, 23, 10.1016/0019-1035(78)90021-0

    1978 doi

  30. [38]

    M., Withers, A., Ardia, P., & Foley, N

    Hirschmann, M. M., Withers, A., Ardia, P., & Foley, N. 2012, Earth and Planetary Science Letters, 345, 38

    2012

  31. [39]

    2024, , 630, 609, 10.1038/s41586-024-07432-x

    Hu , R., Bello-Arufe , A., Zhang , M., et al. 2024, , 630, 609, 10.1038/s41586-024-07432-x

    2024 doi

  32. [40]

    1959, Astronomical Society of the Pacific, 71, pp

    Huang, S. 1959, Astronomical Society of the Pacific, 71, pp. 421. https://www.jstor.org/stable/40673575

    1959

  33. [41]

    Hunter, J. D. 2007, Computing in Science & Engineering, 9, 90, 10.1109/MCSE.2007.55

    2007 doi

  34. [42]

    Ingersoll , A. P. 1969, Journal of the Atmospheric Sciences, 26, 1191, 10.1175/1520-0469(1969)026<1191:TRGAHO>2.0.CO;2

    1969 doi

  35. [43]

    2021, Sci Adv, 7, eabc0444, 10.1126/sciadv.abc0444

    Johansen , A., Ronnet , T., Bizzarro , M., et al. 2021, Sci Adv, 7, eabc0444, 10.1126/sciadv.abc0444

    2021 doi

  36. [44]

    2023, , 671, A75, 10.1051/0004-6361/202142142

    Johansen , A., Ronnet , T., Schiller , M., Deng , Z., & Bizzarro , M. 2023, , 671, A75, 10.1051/0004-6361/202142142

    2023 doi

  37. [45]

    2011, The Astrophysical Journal Letters, 736, L25, 10.1088/2041-8205/736/2/L25

    Kaltenegger , L., & Sasselov , D. 2011, The Astrophysical Journal Letters, 736, L25, 10.1088/2041-8205/736/2/L25

    2011 doi

  38. [46]

    R., Arney , G

    Kane , S. R., Arney , G. N., Byrne , P. K., et al. 2021, J Geophys Res Planets, 126, e06643, 10.1029/2020JE006643

    2021 doi

  39. [47]

    Kasting, J. F. 1988, Icarus, 74, 472, 10.1016/0019-1035(88)90116-9

    1988 doi

  40. [48]

    F., Whitmire, D

    Kasting, J. F., Whitmire, D. P., & Reynolds, R. T. 1993, Icarus, 101, 108

    1993

  41. [49]

    Kempton , E. M. R., & Knutson , H. A. 2024, Reviews in Mineralogy and Geochemistry, 90, 411, 10.2138/rmg.2024.90.12

    2024 doi

  42. [50]

    S., & Schaefer , L

    Kite , E. S., & Schaefer , L. 2021, , 909, L22, 10.3847/2041-8213/abe7dc

    2021 doi

  43. [51]

    Koll , D. D. B., & Cronin , T. W. 2019, , 881, 120, 10.3847/1538-4357/ab30c4

    2019 doi

  44. [52]

    1967, Journal of the Meteorological Society of Japan, 45, 137

    Komabayasi, M. 1967, Journal of the Meteorological Society of Japan, 45, 137

    1967

  45. [53]

    K., Ramirez, R., Kasting, J

    Kopparapu, R. K., Ramirez, R., Kasting, J. F., et al. 2013, The Astrophysical Journal, 765, 131, 10.1088/0004-637X/765/2/131

    2013 doi

  46. [54]

    2023, in , Vol

    Krijt , S., Kama , M., McClure , M., et al. 2023, in , Vol. 534, Astronomical Society of the Pacific Conference Series, 1031

    2023

  47. [55]

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

    2024 doi

  48. [56]

    W., & Coltice , N

    Labrosse , S., Hernlund , J. W., & Coltice , N. 2007, , 450, 866, 10.1038/nature06355

    2007 doi

  49. [57]

    A., et al

    Lambrechts, M., Morbidelli, A., Jacobson, S. A., et al. 2019, , 627, A83, 10.1051/0004-6361/201834229

    2019 doi

  50. [58]

    2013, J Geophys Res Planets, 118, 1155, 10.1002/jgre.20068

    Lebrun , T., Massol , H., Chassefi \`e Re , E., et al. 2013, J Geophys Res Planets, 118, 1155, 10.1002/jgre.20068

    2013 doi

  51. [59]

    2009, , 506, 287, 10.1051/0004-6361/200911933

    L \'e ger , A., Rouan , D., Schneider , J., et al. 2009, , 506, 287, 10.1051/0004-6361/200911933

    2009 doi

  52. [60]

    2015, Earth and Planetary Science Letters, 415, 54, 10.1016/j.epsl.2015.01.017

    Li , Y., Dasgupta , R., & Tsuno , . 2015, Earth and Planetary Science Letters, 415, 54, 10.1016/j.epsl.2015.01.017

    2015 doi

  53. [61]

    2003, Geochimica et Cosmochimica Acta, 67, 4123, https://doi.org/10.1016/S0016-7037(03)00259-X

    Libourel, G., Marty, B., & Humbert, F. 2003, Geochimica et Cosmochimica Acta, 67, 4123, https://doi.org/10.1016/S0016-7037(03)00259-X

    2003 doi

  54. [62]

    2021, , 914, L4, 10.3847/2041-8213/ac0146

    Lichtenberg , T. 2021, , 914, L4, 10.3847/2041-8213/ac0146

    2021 doi

  55. [64]

    J., Hammond , M., et al

    Lichtenberg , T., Bower , D. J., Hammond , M., et al. 2021, J Geophys Res Planets, 126, e06711, 10.1029/2020JE006711

    2021 doi

  56. [65]

    Lichtenberg , T., & Clement , M. S. 2022, , 938, L3, 10.3847/2041-8213/ac9521

    2022 doi

  57. [66]

    2025, Treatise on Geochemistry, 7, 51, 10.1016/B978-0-323-99762-1.00122-4

    Lichtenberg , T., & Miguel , Y. 2025, Treatise on Geochemistry, 7, 51, 10.1016/B978-0-323-99762-1.00122-4

    2025 doi

  58. [67]

    K., Nakajima , M., & Fischer , R

    Lichtenberg , T., Schaefer , L. K., Nakajima , M., & Fischer , R. A. 2023, in Astronomical Society of the Pacific Conference Series, Vol. 534, Protostars and Planets VII, ed. S. Inutsuka , Y. Aikawa , T. Muto , K. Tomida , & M. Tamura , 907, 10.48550/arXiv.2203.10023

    2023 doi arXiv

  59. [68]

    2017, Journal of Geophysical Research

    Marcq, E., Salvador, A., Massol, H., & Davaille, A. 2017, Journal of Geophysical Research. Planets, 122, 1539, 10.1002/2016je005224

    2017 doi

  60. [69]

    J., Cady-Pereira , K

    Mlawer , E. J., Cady-Pereira , K. E., Mascio , J., & Gordon , I. E. 2023, , 306, 108645, 10.1016/j.jqsrt.2023.108645

    2023

  61. [70]

    B., & Boukar \'e , C.- \'E

    Moore , K., Cowan , N. B., & Boukar \'e , C.- \'E . 2023, , 526, 6235, 10.1093/mnras/stad3138

    2023 doi

  62. [71]

    2012, , 546, 1, 10.1051/0004-6361/201219824

    Morbidelli, A., & Nesvorny, D. 2012, , 546, 1, 10.1051/0004-6361/201219824

    2012 doi

  63. [72]

    J., Wünnemann, K., et al

    Nakajima, M., Golabek, G. J., Wünnemann, K., et al. 2021, Earth and Planetary Science Letters, 568, 116983, 10.1016/j.epsl.2021.116983

    2021

  64. [73]

    1992, Journal of the Atmospheric Sciences, 49, 2256, 10.1175/1520-0469(1992)049<2256:ASOTGE>2.0.CO;2

    Nakajima , S., Hayashi , Y.-Y., & Abe , Y. 1992, Journal of the Atmospheric Sciences, 49, 2256, 10.1175/1520-0469(1992)049<2256:ASOTGE>2.0.CO;2

    1992 doi

  65. [74]

    J., & Pierrehumbert , R

    Nicholls , H., Lichtenberg , T., Bower , D. J., & Pierrehumbert , R. 2024, Journal of Geophysical Research (Planets), 129, 2024JE008576, 10.1029/2024JE008576

    2024 doi

  66. [75]

    T., Lichtenberg, T., Soucasse, L., & Smeets, S

    Nicholls, H., Pierrehumbert, R. T., Lichtenberg, T., Soucasse, L., & Smeets, S. 2024, Monthly Notices of the Royal Astronomical Society, 536, 2957, 10.1093/mnras/stae2772

    2024 doi

  67. [76]

    2022, EPSL, 587, 117537, 10.1016/j.epsl.2022.117537

    Olson , P., Sharp , Z., & Garai , S. 2022, EPSL, 587, 117537, 10.1016/j.epsl.2022.117537

    2022

  68. [77]

    2011, , 734, L13, 10.1088/2041-8205/734/1/L13

    Pierrehumbert , R., & Gaidos , E. 2011, , 734, L13, 10.1088/2041-8205/734/1/L13

    2011 doi

  69. [78]

    Pierrehumbert, R. T. 2010, Principles of Planetary Climate (Cambridge University Press), 10.1017/cbo9780511780783

    2010 doi

  70. [79]

    Pierrehumbert , R. T. 2010, Principles of Planetary Climate

    2010

  71. [80]

    V., Barclay , T., Borucki , W

    Quintana , E. V., Barclay , T., Borucki , W. J., Rowe , J. F., & Chambers , J. E. 2016, , 821, 126, 10.3847/0004-637X/821/2/126

    2016 doi

  72. [81]

    Ramirez , R. M. 2020, , 494, 259, 10.1093/mnras/staa603

    2020 doi

  73. [82]

    M., & Kaltenegger , L

    Ramirez , R. M., & Kaltenegger , L. 2014, , 797, L25, 10.1088/2041-8205/797/2/L25

    2014 doi

  74. [83]

    2017, , 837, L4, 10.3847/2041-8213/aa60c8

    ---. 2017, , 837, L4, 10.3847/2041-8213/aa60c8

    2017 doi

  75. [84]

    2018, , 858, 72, 10.3847/1538-4357/aab8fa

    ---. 2018, , 858, 72, 10.3847/1538-4357/aab8fa

    2018 doi

  76. [85]

    2017, Journal of Geophysical Research: Planets, 122, 1458

    Salvador, A., Massol, H., Davaille, A., et al. 2017, Journal of Geophysical Research: Planets, 122, 1458

    2017

  77. [86]

    2023, , 219, 51, 10.1007/s11214-023-00995-7

    Salvador , A., Avice , G., Breuer , D., et al. 2023, , 219, 51, 10.1007/s11214-023-00995-7

    2023 doi

  78. [87]

    Schaefer , L., & Elkins-Tanton , L. T. 2018, Philosophical Transactions of the Royal Society of London Series A, 376, 20180109, 10.1098/rsta.2018.0109

    2018

  79. [88]

    2017, , 843, 120, 10.3847/1538-4357/aa784f

    Schaefer , L., & Fegley , Bruce, J. 2017, , 843, 120, 10.3847/1538-4357/aa784f

    2017 doi

  80. [89]

    D., Berta-Thompson , Z., & Sasselov , D

    Schaefer , L., Wordsworth , R. D., Berta-Thompson , Z., & Sasselov , D. 2016, , 829, 63, 10.3847/0004-637X/829/2/63

    2016 doi

  81. [90]

    2024, Planet Sci, 5, 3, 10.3847/PSJ/acf57f

    Schlecker , M., Apai , D., Lichtenberg , T., et al. 2024, Planet Sci, 5, 3, 10.3847/PSJ/acf57f

    2024 doi

  82. [91]

    2021, , 656, A71, 10.1051/0004-6361/202038554

    Schlecker, M., Mordasini, C., Emsenhuber, A., et al. 2021, , 656, A71, 10.1051/0004-6361/202038554

    2021 doi

  83. [92]

    E., & Young , E

    Schlichting , H. E., & Young , E. D. 2022, , 3, 127, 10.3847/PSJ/ac68e6

    2022 doi

  84. [93]

    F., Levrard , B., et al

    Selsis , F., Kasting , J. F., Levrard , B., et al. 2007, Astronomy & Astrophysics, 476, 1373, 10.1051/0004-6361:20078091

    2007 doi

  85. [94]

    2023, Nature, 620, 287, 10.1038/s41586-023-06258-3

    Selsis, F., Leconte, J., Turbet, M., Chaverot, G., & Bolmont, E. 2023, Nature, 620, 287, 10.1038/s41586-023-06258-3

    2023 doi

  86. [95]

    Shorttle , O., Jordan , S., Nicholls , H., Lichtenberg , T., & Bower , D. J. 2024, , 962, L8, 10.3847/2041-8213/ad206e

    2024 doi

  87. [96]

    A., Burnham , A

    Sossi , P. A., Burnham , A. D., Badro , J., et al. 2020, Sci Adv, 6, eabd1387, 10.1126/sciadv.abd1387

    2020 doi

  88. [97]

    A., Tollan, P

    Sossi, P. A., Tollan, P. M. E., Badro, J., & Bower, D. J. 2023, Earth and Planetary Science Letters, 601, 117894, 10.1016/j.epsl.2022.117894

    2023

  89. [98]

    S., Dalou , C., & Lichtenberg , T

    Suer , T.-A., Jackson , C., Grewal , D. S., Dalou , C., & Lichtenberg , T. 2023, Front Earth Sci, 11, 1159412, 10.3389/feart.2023.1159412

    2023

  90. [99]

    B., & Melosh, H

    Tonks, W. B., & Melosh, H. J. 1993, Journal of Geophysical Research, 98, 5319, 10.1029/92je02726

    1993 doi

  91. [100]

    2021, , 598, 276, 10.1038/s41586-021-03873-w

    Turbet , M., Bolmont , E., Chaverot , G., et al. 2021, , 598, 276, 10.1038/s41586-021-03873-w

    2021 doi

  92. [101]

    2020, , 638, A41, 10.1051/0004-6361/201937151

    Turbet , M., Bolmont , E., Ehrenreich , D., et al. 2020, , 638, A41, 10.1051/0004-6361/201937151

    2020 doi

  93. [102]

    J., Leconte , J., et al

    Turbet , M., Fauchez , T. J., Leconte , J., et al. 2023, , 679, A126, 10.1051/0004-6361/202347539

    2023 doi

  94. [103]

    R., Jones , B

    Underwood , D. R., Jones , B. W., & Sleep , P. N. 2003, International Journal of Astrobiology, 2, 289, 10.1017/S1473550404001715

    2003 doi

  95. [104]

    2020, , 900, 24, 10.3847/1538-4357/aba8a5

    Walterov \'a , M., & B e hounkov \'a , M. 2020, , 900, 24, 10.3847/1538-4357/aba8a5

    2020 doi

  96. [105]

    S., Lineweaver, C

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

    2018 doi

  97. [106]

    Warren, P. H. 1985, Annual review of earth and planetary sciences, 13, 201, 10.1146/annurev.ea.13.050185.001221

    1985

  98. [107]

    2022, , 60, 159, 10.1146/annurev-astro-052920-125632

    Wordsworth , R., & Kreidberg , L. 2022, , 60, 159, 10.1146/annurev-astro-052920-125632

    2022 doi

  99. [108]

    C., Kral, Q., & Sinclair, C

    Wyatt, M. C., Kral, Q., & Sinclair, C. A. 2019, Mon Not R Astron Soc, 802, 782, 10.1093/mnras/stz3052

    2019 doi

  100. [109]

    B., & Abbot , D

    Yang , J., Cowan , N. B., & Abbot , D. S. 2013, , 771, L45, 10.1088/2041-8205/771/2/L45

    2013 doi

  101. [110]

    2020, The Astrophysical Journal Letters, 901, L36, 10.3847/2041-8213/abb87f

    Zhang , Y., & Yang , J. 2020, The Astrophysical Journal Letters, 901, L36, 10.3847/2041-8213/abb87f

    2020 doi

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