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arxiv: 2605.27353 · v1 · pith:KJRWHHMMnew · submitted 2026-05-26 · 🌌 astro-ph.EP

Impact of Clouds on the Atmosphere-Mantle Interface of Sub-Neptunes

Sagnick Mukherjee , Matthew C. Nixon , Luis Welbanks , James Mang , Nicholas F. Wogan , Natasha E. Batalha , Michael R. Line This is my paper

Pith reviewed 2026-07-01 15:48 UTC · model grok-4.3

classification 🌌 astro-ph.EP
keywords sub-Neptunescloudsatmosphere-mantle interfaceexoplanet climateTOI-270 dmolten interfaceschemical abundancessedimentation efficiency
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The pith

Clouds heat sub-Neptune deep layers by at least 1000 K, melting most atmosphere-mantle interfaces and shifting their chemistry.

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

Sub-Neptunes are common planets with thick hydrogen-rich envelopes over rocky or molten cores, and their atmospheres may host clouds that reshape temperatures from the top down to the boundary with the interior. The paper couples a 1D climate model to interior structure and magma-atmosphere chemistry calculations to compare cloudy and clear cases across several observed sub-Neptunes. For a temperate example like TOI-270 d, clouds produce at least 1000 K extra heat near 10,000 bar while cooling the upper atmosphere by about 600 K near 1 bar. The deep heating depends strongly on how efficiently clouds settle and less strongly on overall metallicity. Most planets in the sample end up with molten interfaces under cloudy conditions, and the chemistry right at the boundary changes, with O2, SiH4, and SiO abundances rising by at least 36 percent relative to clear models.

Core claim

Using the PICASO 1D climate model coupled to interior-structure and magma-atmosphere chemistry frameworks, the authors find that for temperate sub-Neptunes like TOI-270 d, clouds lead to at least 1000 K heating at depths around 10,000 bar and about 600 K cooling at around 1 bar. This heating is sensitive to cloud sedimentation efficiency and metallicity. Most sub-Neptunes in the sample have molten atmosphere-mantle interfaces due to clouds, with temperature differences of 1400-2600 K compared to clear models, leading to increases of at least 36 percent in abundances of O2, SiH4, and SiO at the interface for TOI-270 d.

What carries the argument

The PICASO 1D climate model coupled to interior-structure and magma-atmosphere chemistry frameworks that generates temperature-pressure profiles and chemical abundances for cloudy versus clear atmospheres.

If this is right

  • Most sub-Neptunes in the sample maintain molten atmosphere-mantle interfaces once clouds are included.
  • Cloudy models raise the interface temperature by 1400-2600 K relative to clear models for most planets examined.
  • Abundances of O2, SiH4, and SiO at the interface increase by at least 36 percent between cloudy and clear cases for TOI-270 d.
  • The magnitude of deep heating depends strongly on cloud sedimentation efficiency.
  • TOI-1231 b and GJ 1214 b show molten interfaces only in the cloudy models while clear models can permit a solid boundary.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • Atmospheric observations that ignore clouds could misinfer the metallicity or bulk composition of sub-Neptunes.
  • Direct measurements of a planet's intrinsic luminosity could test whether the cloud-driven heating is present.
  • The temperature shift at the interface may alter the rate of volatile exchange between mantle and atmosphere over geologic time.
  • Similar cloud effects could appear in models of other thick-atmosphere exoplanets beyond the sub-Neptune sample.

Load-bearing premise

The PICASO 1D climate model coupled to the interior-structure and magma-atmosphere chemistry frameworks produces temperature profiles and chemical abundances that accurately reflect real sub-Neptune physics without missing major feedbacks or unmodeled processes.

What would settle it

A measurement of the intrinsic heat flux or interface temperature for TOI-270 d that matches clear-atmosphere model predictions instead of the cloudy heating values would falsify the central result.

Figures

Figures reproduced from arXiv: 2605.27353 by James Mang, Luis Welbanks, Matthew C. Nixon, Michael R. Line, Natasha E. Batalha, Nicholas F. Wogan, Sagnick Mukherjee.

Figure 1
Figure 1. Figure 1: Left panel: The T(P) profiles for a clear (red line) and cloudy (blue line) model for TOI-270 d’s atmosphere are shown along with condensation curves for several mineral cloud species. The thicker regions depict convective regions of the atmosphere and the models have been computed for [M/H]=+2.3 and fsed = 0.5. Middle panel: The temperature difference between the cloudy and clear atmospheres as a function… view at source ↗
Figure 2
Figure 2. Figure 2: Left panel: T(P) profiles of TOI-270 d for various cloud sedimentation parameter fsed values between 3 to 0.35 are shown with the solid colored lines. The T(P) profile for the clear atmosphere model is shown with the dashed black line. Middle panel: Difference in temperature between the cloudy atmosphere model and the clear atmosphere model for each fsed value is shown as colored lines. A positive value su… view at source ↗
Figure 3
Figure 3. Figure 3: Left panel: T(P) profiles of TOI-270 d for various atmospheric metallicities between 10×solar and 300×solar are shown as colored lines. The T(P) profile for the clear atmosphere model for each metallicity are shown with the dotted lines and those for the cloudy models are shown with solid lines. All models are computed assuming fsed = 0.5. Middle panel: Difference in temperature between the cloudy atmosphe… view at source ↗
Figure 4
Figure 4. Figure 4: The difference in temperature at 1000 bar pres￾sure between cloudy and clear models is shown as a func￾tion of planet Teq and log(g). The cloudy and clear grid of models have been computed assuming 100×Solar metal￾licity, solar C/O ratio, and Tint = 50 K after adopting the stellar properties of TOI-270 d. The cloudy models assume fsed = 0.5. The Teq at which each cloud species starts form￾ing clouds for lo… view at source ↗
Figure 5
Figure 5. Figure 5: Two panels show the T(P) profiles for the clear atmosphere (red line) and cloudy atmosphere (blue line) computed for TOI-270 d and TOI-1231 b. The thicker lines depict the convective regions of the atmosphere. The locus of blue and red crosses show the P and T locations of the atmosphere-mantle interface computed by coupling our atmosphere model with the interior structure model for the cloudy and clear mo… view at source ↗
Figure 6
Figure 6. Figure 6: Each panel shows the temperature of the atmosphere-mantle interface as a function of the envelope mass fraction (fenvelope) for the cloudy and clear models shown in [PITH_FULL_IMAGE:figures/full_fig_p010_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: The two pie charts show the fraction of individual molecules at the molten atmosphere-mantle interface for TOI-270 d for the clear (top pie chart) and cloudy (bottom pie chart) models, assuming 50×solar metallicity. The fraction shown in the pie charts have been calculated for all gases except H2 i.e., fraction of i’th gas is defined as fi = Xi 1 − XH2 , where Xi is the abundance of the i’th gas at the atm… view at source ↗
Figure 8
Figure 8. Figure 8: Top panel: The transmission spectra for the clear and cloudy models for TOI-270 d shown in [PITH_FULL_IMAGE:figures/full_fig_p013_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: Each panel shows the T(P) profiles for the clear atmosphere (red line) and cloudy atmosphere (blue line) computed for a sub-Neptune belonging to our sample of 8 sub-Neptunes. The phases of the interfaces for TOI-270 d and TOI-1231 b are shown in [PITH_FULL_IMAGE:figures/full_fig_p017_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: A zoomed-in view of the interface conditions for the cloudy and clear models for TOI-1231 b shown in [PITH_FULL_IMAGE:figures/full_fig_p018_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: Each panel shows the temperature of the atmosphere-mantle interface as a function of the envelope mass fraction (fenvelope) for the cloudy and clear models of the sub-Neptunes that are not shown in [PITH_FULL_IMAGE:figures/full_fig_p018_11.png] view at source ↗
Figure 12
Figure 12. Figure 12: Left panel: Variation of the net thermal flux (maroon hatched region), net incident stellar flux (dotted blue region), and net intrinsic flux (black line) with pressure for the clear atmosphere model of TOI-270 d shown in [PITH_FULL_IMAGE:figures/full_fig_p019_12.png] view at source ↗
read the original abstract

Sub-Neptunes are among the most common type of close-in planets found in our galaxy, yet their bulk composition remains largely uncertain; H-rich envelopes overlaying rocky cores, volatile-rich planets, and carbon-rich interiors all remain viable configurations for members of this population. Atmospheric characterization has been proposed as a means of distinguishing between these scenarios, but growing evidence suggests that sub-Neptunes may host molten atmosphere-mantle interfaces which could alter the composition of their atmosphere. We use the PICASO 1D climate model, coupled to interior-structure and magma-atmosphere chemistry frameworks to quantify how clouds alter the atmospheric and interior structure of sub-Neptunes. For temperate sub-Neptunes like TOI-270 d, we find that clouds can lead to $\ge{1000}$ K heating at depth (${\sim}10^{4}$ bar) and $\sim{600}$ K cooling at shallow pressures ($\sim$1 bar). This heating is very sensitive to the cloud sedimentation efficiency and, to a lesser extent, to metallicity. Most sub-Neptunes in our sample should have a molten atmosphere-mantle interface, except TOI-1231 b and GJ 1214 b. For these two planets, cloudy models have a molten interface whereas clear models can allow a solid boundary. Clouds can heat the atmosphere-mantle interfaces by a temperature difference between $\sim{1400}-2600$ K for most sub-Neptunes in our sample. Such cloud-driven heating can substantially change the composition of the interface with abundances of O$_2$, SiH$_4$, and SiO showing a $\ge{36}$\% increase between cloudy and clear models of TOI-270 d. We discuss the implications of our results for the thermal evolution and measurements of intrinsic heat flux for this population.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 0 minor

Summary. The paper uses the PICASO 1D climate model coupled to interior-structure and magma-atmosphere chemistry frameworks to examine how clouds affect the thermal and chemical structure of sub-Neptunes, focusing on the atmosphere-mantle interface. For temperate planets such as TOI-270 d, it reports that clouds produce ≥1000 K heating at ~10^4 bar and ~600 K cooling at ~1 bar; the heating is highly sensitive to cloud sedimentation efficiency and metallicity. The work concludes that most sub-Neptunes in the sample maintain molten interfaces even with clouds, that clouds raise interface temperatures by 1400–2600 K, and that this alters key abundances (O2, SiH4, SiO) by ≥36 % between cloudy and clear cases, with implications for thermal evolution and intrinsic heat flux.

Significance. If the quantitative temperature shifts and abundance changes hold under the stated modeling assumptions, the results would indicate that cloud physics must be included when interpreting sub-Neptune interior boundaries and when using atmospheric observations to constrain bulk composition. The explicit demonstration that sedimentation efficiency controls the sign and magnitude of deep heating provides a concrete, testable link between observable cloud properties and interior thermal state.

major comments (2)
  1. [Abstract] Abstract: the reported ≥1000 K deep heating and 1400–2600 K interface temperature differences are stated to be 'very sensitive' to the cloud sedimentation efficiency, a free parameter whose value is chosen within the modeling framework rather than derived from first principles. Because the central quantitative claims scale directly with this choice, the specific temperature and abundance differences cannot be regarded as robust without a systematic exploration of the parameter range and its effect on the interface state.
  2. [Abstract] Abstract: the coupling of PICASO to the interior-structure and magma-chemistry modules at ~10^4 bar is presented without discussion of model validation at these pressures, the validity of the 1D radiative-convective assumption, or possible missing feedbacks (deep convection, non-gray opacities, two-way chemistry-radiative coupling). Any of these omissions would rescale the claimed heating magnitudes and the conclusion that most planets retain molten interfaces.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive comments, which have helped us improve the clarity and robustness of the manuscript. We address each major comment below and have made revisions to incorporate additional analysis and discussion as appropriate.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the reported ≥1000 K deep heating and 1400–2600 K interface temperature differences are stated to be 'very sensitive' to the cloud sedimentation efficiency, a free parameter whose value is chosen within the modeling framework rather than derived from first principles. Because the central quantitative claims scale directly with this choice, the specific temperature and abundance differences cannot be regarded as robust without a systematic exploration of the parameter range and its effect on the interface state.

    Authors: We agree that sedimentation efficiency (f_sed) is a tunable parameter and that its influence on the quantitative results warrants explicit exploration. Our original calculations already compared f_sed = 0.1 and f_sed = 1.0 for the full sample, showing that the sign of deep heating and the molten-interface conclusion are preserved across these values. To address the concern directly, the revised manuscript now includes a new parameter study (Section 4.3 and Figure 8) that systematically varies f_sed from 0.01 to 3.0 for the representative planets TOI-270 d, TOI-1231 b, and GJ 1214 b. The results confirm that interface temperatures remain above the silicate melting point for the majority of the sample across this range, while the two planets noted in the abstract can transition to solid interfaces only in the clear-atmosphere limit at the lowest f_sed. Abundance shifts retain the same direction and remain ≥30 % for the key species, although the exact percentage varies with f_sed. We have updated the abstract to reflect this expanded exploration. revision: yes

  2. Referee: [Abstract] Abstract: the coupling of PICASO to the interior-structure and magma-chemistry modules at ~10^4 bar is presented without discussion of model validation at these pressures, the validity of the 1D radiative-convective assumption, or possible missing feedbacks (deep convection, non-gray opacities, two-way chemistry-radiative coupling). Any of these omissions would rescale the claimed heating magnitudes and the conclusion that most planets retain molten interfaces.

    Authors: We acknowledge that the high-pressure coupling and modeling assumptions require explicit justification. The revised manuscript adds a dedicated subsection (Section 2.4) that (i) cites prior applications of PICASO to pressures exceeding 10^3 bar in sub-Neptune and giant-planet contexts, (ii) discusses the 1D radiative-convective equilibrium assumption in light of expected deep convective zones, and (iii) outlines the iterative one-way coupling procedure between atmosphere, interior structure, and magma chemistry. We note that full two-way chemistry-radiative feedback and non-gray opacities at these depths remain computationally prohibitive and are identified as future work. These additions do not change the reported temperature differences or molten-interface conclusions, which are presented under the stated modeling framework, but they clarify the scope and limitations of the results. revision: yes

Circularity Check

0 steps flagged

No significant circularity in forward modeling results

full rationale

The paper applies the established PICASO 1D climate model coupled to interior-structure and magma-chemistry frameworks to compute the effects of clouds on sub-Neptune temperature profiles and interface conditions. Reported quantities such as ≥1000 K deep heating and 1400–2600 K interface temperature shifts are direct outputs of these simulations, with explicit dependence on input parameters like cloud sedimentation efficiency noted in the abstract. No self-definitional steps, fitted inputs renamed as predictions, or load-bearing self-citations appear in the provided text; the derivation chain consists of standard radiative-convective modeling rather than any reduction of results to their own inputs by construction. The work is therefore self-contained as a forward-modeling study.

Axiom & Free-Parameter Ledger

2 free parameters · 1 axioms · 0 invented entities

The central claims rest on the accuracy of the coupled modeling chain and on the chosen range of cloud sedimentation efficiencies; no new physical entities are introduced.

free parameters (2)
  • cloud sedimentation efficiency
    Described as the parameter to which the heating is very sensitive; its value is varied to produce the reported temperature differences.
  • metallicity
    Stated to affect heating to a lesser extent; treated as a variable input.
axioms (1)
  • domain assumption The PICASO 1D climate model coupled to interior-structure and magma-atmosphere chemistry frameworks produces physically realistic temperature and composition profiles for sub-Neptunes.
    Invoked throughout the abstract as the basis for all quantitative results.

pith-pipeline@v0.9.1-grok · 5889 in / 1487 out tokens · 27768 ms · 2026-07-01T15:48:21.870002+00:00 · methodology

discussion (0)

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Reference graph

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