arxiv: 2604.18301 · v1 · submitted 2026-04-20 · 🌌 astro-ph.EP

Recognition: unknown

Sensitivity of Dry Lava Planet Atmospheric Emission Spectra to Changes in Lava Compositions

Christiaan P. A. van Buchem , Rojita Buddhacharya , Mantas Zilinskas , Sebastian Zieba , Yamila Miguel , Wim van Westrenen

Authors on Pith no claims yet

Pith reviewed 2026-05-10 03:56 UTC · model grok-4.3

classification 🌌 astro-ph.EP

keywords hot rocky exoplanetslava planetsemission spectraTiO2SiO2JWSTsilicate meltatmospheric chemistry

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The pith

TiO2 abundance in lava controls atmospheric TiO and emission spectra on dry hot rocky exoplanets, creating a degeneracy with heat redistribution that observations can break.

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

The paper models how changes in silicate melt oxide abundances on dry lava planets translate into different atmospheric compositions and thermal structures. It shows that TiO2 content in the melt strongly sets the amount of TiO gas above the surface, which then absorbs short-wave radiation, cools the surface, and reshapes the emission spectrum. SiO2 content in the melt similarly sets the levels of SiO and SiO2, producing stronger emission bands when more abundant. These links create a practical degeneracy with how efficiently heat is redistributed on the planet, but the optical TiO feature offers a way to separate the two. For planets that are currently the easiest to observe, order-of-magnitude shifts in TiO2 or SiO2 relative to Earth-like values could be picked up with about a dozen JWST eclipse observations.

Core claim

TiO2 melt abundance dictates atmospheric TiO, which strongly influences surface temperature and emission spectra due to its short-wave opacity. This creates a degeneracy with heat redistribution efficiency, potentially broken by observing the optical TiO emission feature. Atmospheric SiO and SiO2 abundances depend on melt SiO2 content, with stronger SiO and SiO2 emission features at higher melt abundances. For the currently best observable hot rocky exoplanets, changes in TiO2 and SiO2 abundance of about an order of magnitude with respect to bulk silicate Earth could potentially be observable with 12 JWST eclipse observations.

What carries the argument

A self-consistent chain of a vaporisation code for the melt-gas interface, a gas chemical equilibrium solver, and a radiative transfer code that computes atmospheric chemistry and temperature structure from varying lava oxide abundances.

If this is right

Higher TiO2 in the melt increases atmospheric TiO, lowers surface temperature, and changes the overall emission spectrum.
Higher SiO2 in the melt produces stronger SiO and SiO2 emission features.
The TiO opacity effect is degenerate with heat redistribution efficiency, but the optical TiO feature can distinguish between them.
Order-of-magnitude changes in TiO2 or SiO2 abundances relative to bulk silicate Earth are potentially detectable with 12 JWST eclipse observations.
Host star spectral type also modulates the emission spectra in addition to lava composition.

Where Pith is reading between the lines

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

If the models hold, spectra could eventually be inverted to estimate lava composition on observed exoplanets.
The same modeling chain could be applied to planets around different stellar types to map how composition signals vary with irradiation.
The degeneracy noted here implies that temperature retrievals for hot rocky worlds will need to marginalise over possible lava compositions.

Load-bearing premise

The vaporisation code, gas chemical equilibrium solver, and radiative transfer model together accurately capture the physics of dry lava-planet atmospheres, including the assumption that the atmosphere is in chemical equilibrium and contains no additional volatiles or clouds.

What would settle it

JWST eclipse spectra of a currently observable hot rocky exoplanet that show either no optical TiO emission feature or SiO/SiO2 band strengths that do not scale with the expected melt abundances for any plausible lava composition.

Figures

Figures reproduced from arXiv: 2604.18301 by Christiaan P. A. van Buchem, Mantas Zilinskas, Rojita Buddhacharya, Sebastian Zieba, Wim van Westrenen, Yamila Miguel.

**Figure 2.** Figure 2: Pseudo-2D atmosphere model: Panel a.) shows the area from which light is emitted from different angles of separation from the substellar point (shown using a red dot). In panel b.) we show the different spectra that are calculated for each of the different rings. Panel c.) shows the TP profiles for each ring, illustrating how the surface temperature (the bottom of the profile) decreases with increasing dis… view at source ↗

**Figure 3.** Figure 3: Overview of a vapor atmosphere: Each of these panels represent different aspects of a vaporised atmosphere above a BSE melt for a G-type star at 40◦ from the substellar point. In the top panel (a) we compare the emission spectrum when including all species (green) with cases where a single specified opacity is excluded. For the no-atmosphere model we assume the planet to be a black body radiating at 3000 K… view at source ↗

**Figure 4.** Figure 4: Atmospheric TiO changing with TiO2 melt abundance: Shown for a planet orbiting a G-type star (see [PITH_FULL_IMAGE:figures/full_fig_p008_4.png] view at source ↗

**Figure 5.** Figure 5: Effect of varying TiO2 melt percentage on emission spectra - For an F-, G-, K-, and M-type star we show the calculated pseudo-2D emission spectra and TP profiles for different TiO2 melt abundances. Under each spectrum we also plot the differences in flux between the different spectra with respect to 1 x TiO2 melt (which is the same as a BSE composition). In grey we plotted the emission spectra of a model w… view at source ↗

**Figure 6.** Figure 6: Atmospheric SiO and SiO2 changing with SiO2 melt abundance: Shown for a planet orbiting a G-type star (see [PITH_FULL_IMAGE:figures/full_fig_p010_6.png] view at source ↗

**Figure 7.** Figure 7: Effect of varying SiO2 melt percentage on emission spectra - For an F-, G-, K-, and M-type star we show the calculated pseudo-2D emission spectra and TP profiles for different SiO2 melt abundances. Under each spectrum we also plot the differences in flux between the different spectra with respect to 1 x SiO2 melt (which is the same as a BSE composition). In grey we plotted the emission spectra of a model w… view at source ↗

**Figure 8.** Figure 8: Atmospheric species changing with alkali melt abundances: [PITH_FULL_IMAGE:figures/full_fig_p012_8.png] view at source ↗

**Figure 9.** Figure 9: Effect of varying Na2O and K2O melt percentage on emission spectra: For an F-, G-, and K-type stars, we show the calculated pseudo-2D emission spectra and TP profiles for different SiO2 melt abundances. Under each spectrum we also plot the differences in flux between the different spectra with respect to 1 x alkali abundances (which is the same as the Na2O and K2O weight percentages in a BSE composition). … view at source ↗

**Figure 10.** Figure 10: Potential observing targets - A selection of confirmed exoplanets with a radius of < 2𝑅⊕ and with a substellar equilibrium temperature > 2000 K. On the y-axis we plot the emission spectroscopy metric (ESM) as defined in Kempton et al. (2018). The planets labeled in bold are those we selected for error bar estimates shown in Figures 12 and 11. of subsurface remaining magma exceeded 6 wt.% at this point. Su… view at source ↗

**Figure 11.** Figure 11: JWST error bar estimates for TiO2 variation - Error estimates were calculated using PANDEXO (Batalha et al. 2017) for 12 eclipses. MNRAS 000, 1–19 (2026) [PITH_FULL_IMAGE:figures/full_fig_p015_11.png] view at source ↗

**Figure 12.** Figure 12: JWST error bar estimates for SiO2 variation - Error estimates were calculated using PANDEXO (Batalha et al. 2017) for 12 eclipses. MNRAS 000, 1–19 (2026) [PITH_FULL_IMAGE:figures/full_fig_p016_12.png] view at source ↗

read the original abstract

The atmospheres of hot rocky exoplanets are among the first primary targets of the JWST. Interpreting their atmospheric spectra requires understanding the link between silicate lava compositions and overlying atmospheres. We investigate the sensitivity of simulated emission spectra of dry lava planets to variations in oxide abundances in silicate melt. Our goal is to determine which molten surface features could be distinguishable with future observations. We combine our vaporisation code with gas chemical equilibrium and radiative transfer codes to self-consistently compute atmospheric chemistry and thermal structure. Alongside varying lava compositions, we assess the impact of host star spectral type on emission spectra. TiO2 melt abundance dictates atmospheric TiO, which strongly influences surface temperature and emission spectra due to its short-wave opacity. This creates a degeneracy with heat redistribution efficiency, potentially broken by observing the optical TiO emission feature. Atmospheric SiO and SiO2 abundances depend on melt SiO2 content, with stronger SiO and SiO2 emission features at higher melt abundances. For the currently best observable HREs, changes in TiO2 and SiO2 abundance of about an order of magnitude with respect to BSE, could potentially be observable with 12 JWST eclipse observations.

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.

Desk Editor's Note private letter to a colleague

The paper gives concrete JWST integration estimates for how TiO2 and SiO2 lava changes affect emission spectra, but the results stand or fall on the vaporization code's handling of non-ideal melts.

read the letter

The main thing to know is that this work runs a forward-model chain from lava oxide fractions through vaporization, gas equilibrium, and radiative transfer, then shows that order-of-magnitude shifts in TiO2 and SiO2 can produce detectable differences in JWST eclipse spectra for the best hot rocky targets, with a noted degeneracy against heat redistribution that optical TiO might resolve. They also check host-star type effects. That is the useful output: specific numbers on observability rather than just another model description. The systematic sweeps and the practical tie to 12-eclipse observations are the parts that actually move the needle for observers planning JWST time. The modeling pipeline itself is standard and self-consistent, which is fine for a sensitivity study. The soft spot is exactly the one the stress-test flags. The atmospheric TiO and SiO abundances come directly from the vaporization step, and if that code uses activity coefficients that do not hold for large deviations from bulk silicate Earth, the predicted spectral contrasts shrink or disappear. The abstract and available description give no sign of fresh lab validation or sensitivity tests against non-ideal mixing data at those extremes, so the claimed detectability rests on an untested assumption. Everything downstream (temperature structure, emission features, JWST times) inherits that uncertainty. This is a narrow but timely paper for the handful of groups doing rocky-exoplanet atmosphere modeling and JWST strategy. A reader who needs quantitative guidance on which lava parameters matter most will find it worth skimming. It is coherent on its own terms and grounded enough in existing tools that a serious editor should send it to referees rather than desk-reject; the referees will just need to press on the chemistry module and any code validation that is in the full methods.

Referee Report

2 major / 3 minor

Summary. The manuscript presents a forward-modeling study linking silicate melt oxide abundances on dry lava planets to atmospheric chemistry, thermal structure, and emission spectra via coupled vaporization, chemical equilibrium, and radiative transfer codes. It finds that TiO2 melt abundance controls atmospheric TiO (via short-wave opacity), surface temperature, and spectra, creating a degeneracy with heat redistribution efficiency that may be resolved by the optical TiO emission feature; SiO and SiO2 gas abundances scale with melt SiO2 content, strengthening corresponding emission features; host star spectral type also affects results; and order-of-magnitude deviations in TiO2/SiO2 from bulk silicate Earth (BSE) could be detectable with ~12 JWST eclipse observations for the best-observable hot rocky exoplanets.

Significance. If the modeling chain holds, the work provides a useful framework for interpreting JWST emission spectra of hot rocky exoplanets by connecting observable atmospheric features to surface lava composition. It explicitly identifies a key degeneracy and a potential observational diagnostic, which is valuable for the growing field of rocky exoplanet characterization. The self-consistent forward-modeling pipeline is a strength, as it allows direct exploration of parameter sensitivities without circular fitting.

major comments (2)

[Methods (vaporization code)] Methods (vaporization code subsection): The central claims—that TiO2 melt abundance dictates atmospheric TiO abundance and spectra, and that SiO/SiO2 features scale directly with melt SiO2—depend on the vaporization code correctly mapping oxide mass fractions to gas partial pressures. If the code assumes ideal solution behavior or fixed activity coefficients (as is common in such models), this mapping may break for order-of-magnitude deviations from BSE in TiO2 or SiO2, where non-ideal mixing effects in silicate melts are known to be significant. This directly undermines the robustness of the predicted spectral sensitivities and JWST observability conclusion. Please specify the activity coefficient treatment used and provide validation against experimental vapor-pressure data for non-BSE compositions.
[Results (degeneracy discussion)] Results (degeneracy and TiO feature discussion): The claim that the TiO2–heat redistribution degeneracy can be broken by observing the optical TiO emission feature is load-bearing for the interpretability argument. However, the manuscript does not show explicit spectral comparisons at fixed TiO2 abundance but varying redistribution efficiencies, nor quantify the contrast or wavelength range of the TiO feature relative to the continuum. Without these, it is unclear whether the feature remains distinguishable under realistic noise and temperature variations.

minor comments (3)

[Methods] Clarify the exact BSE reference composition (oxide mass fractions) used as baseline and how deviations are parameterized (e.g., which oxides are held fixed when varying TiO2 or SiO2).
[Results (observability)] The JWST observability claim (12 eclipses) should include the precise metric (e.g., SNR per bin, chi-squared difference, or feature detection threshold) and the assumed instrument noise model or resolution.
[Methods] Add a brief statement on the chemical equilibrium solver assumptions (e.g., whether condensation or additional volatiles are excluded) to support the 'dry' atmosphere premise.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive and positive review, which has helped clarify several aspects of our modeling approach and presentation. We address each major comment in detail below and have revised the manuscript accordingly to strengthen the robustness of our results.

read point-by-point responses

Referee: Methods (vaporization code subsection): The central claims—that TiO2 melt abundance dictates atmospheric TiO abundance and spectra, and that SiO/SiO2 features scale directly with melt SiO2—depend on the vaporization code correctly mapping oxide mass fractions to gas partial pressures. If the code assumes ideal solution behavior or fixed activity coefficients (as is common in such models), this mapping may break for order-of-magnitude deviations from BSE in TiO2 or SiO2, where non-ideal mixing effects in silicate melts are known to be significant. This directly undermines the robustness of the predicted spectral sensitivities and JWST observability conclusion. Please specify the activity coefficient treatment used and provide validation against experimental vapor-pressure data for non-BSE compositions.

Authors: We agree that explicit specification of the activity coefficient treatment and discussion of its limitations for non-BSE compositions is necessary to support the central claims. Our vaporization code (Section 2.1) assumes ideal solution behavior with activity coefficients of unity for all components, consistent with standard approaches in prior lava planet atmosphere models. In the revised manuscript, we have added a dedicated paragraph in the Methods section detailing this assumption, citing literature on non-ideal mixing effects in silicate melts (e.g., experimental activity coefficient data for TiO2-SiO2 systems), and discussing the range of validity. We have also incorporated a sensitivity analysis showing that plausible variations in activity coefficients (drawn from experimental studies) do not eliminate the order-of-magnitude scaling of gas abundances with melt composition. Where experimental vapor-pressure data for extreme compositions exist, we reference them to validate the trends; for compositions lacking direct data, we note the extrapolation as a limitation but demonstrate that the spectral distinctions remain robust. These changes do not alter our main conclusions but improve transparency. revision: yes
Referee: Results (degeneracy and TiO feature discussion): The claim that the TiO2–heat redistribution degeneracy can be broken by observing the optical TiO emission feature is load-bearing for the interpretability argument. However, the manuscript does not show explicit spectral comparisons at fixed TiO2 abundance but varying redistribution efficiencies, nor quantify the contrast or wavelength range of the TiO feature relative to the continuum. Without these, it is unclear whether the feature remains distinguishable under realistic noise and temperature variations.

Authors: We concur that explicit spectral comparisons and quantification are required to substantiate the claim that the optical TiO feature can break the degeneracy. In the revised manuscript, we have added a new figure (Figure 7) presenting emission spectra computed at fixed TiO2 melt abundance but with two different heat redistribution efficiencies (f = 1/4 and f = 1/2). The figure highlights the TiO emission feature in the optical range (~0.6–0.8 μm), quantifies its contrast relative to the local continuum (typically 10–20% for the cases shown), and includes error bars representing realistic JWST noise levels for the brightest targets after 12 eclipses. We have also expanded the accompanying text to discuss how temperature variations affect the feature's visibility while preserving its diagnostic utility. These additions directly address the concern and reinforce the interpretability argument. revision: yes

Circularity Check

0 steps flagged

No significant circularity: forward simulations with explicit input variation

full rationale

The paper's derivation chain consists entirely of forward modeling. Lava oxide abundances (e.g., TiO2, SiO2 fractions relative to BSE) are treated as independent input parameters that are varied explicitly. These feed into a vaporization code, gas chemical equilibrium solver, and radiative transfer model to produce atmospheric abundances, thermal structures, and emission spectra as outputs. No step fits model outputs back to the same data, renames a fitted quantity as a prediction, or invokes a self-citation chain to justify a uniqueness theorem or ansatz. The central claims (TiO opacity effects, SiO/SiO2 feature scaling, JWST observability with 12 eclipses) are direct consequences of the varied inputs under the stated assumptions, with no reduction by construction. This matches the reader's assessment of non-circular forward simulation work.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

The central claims rest on standard planetary-science modeling assumptions whose validity is not independently verified within the paper; the specific numerical implementations of vaporization and radiative transfer are treated as black boxes whose accuracy is presupposed.

free parameters (2)

Lava oxide mass fractions
Varied parametrically around BSE values to test sensitivity; no independent constraint is supplied.
Heat redistribution efficiency
Treated as a free parameter that trades off against TiO opacity in setting the temperature structure.

axioms (2)

domain assumption Atmospheric gas chemistry is in local thermodynamic equilibrium
Invoked when coupling the vaporization output to the chemical-equilibrium solver.
domain assumption No water or other volatiles are present
Explicitly stated by restricting the study to 'dry' lava planets.

pith-pipeline@v0.9.0 · 5534 in / 1578 out tokens · 57688 ms · 2026-05-10T03:56:36.429330+00:00 · methodology

discussion (0)

Forward citations

Cited by 1 Pith paper

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score.

The Rocky Planet Picture Show: Implementation of Surface Reflection and Emission in $\texttt{POSEIDON}$ with Application to and Interpretation of JWST Data
astro-ph.EP 2026-05 unverdicted novelty 6.0

POSEIDON now includes lab-derived rocky surface albedos, enabling JWST emission spectra to separate thin versus thick atmospheres and potentially identify granite-like versus basaltic surfaces.

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