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arxiv: 2603.08529 · v1 · submitted 2026-03-09 · 🌌 astro-ph.SR · astro-ph.EP· astro-ph.GA

Gas chemistry in the dust depleted inner regions of protoplanetary disks. I. Near-IR spectra and overtones

J. Bethlehem , Ch. Rab , I. Kamp , M. Flock , G. Bourdarot , P. Caselli This is my paper

Pith reviewed 2026-05-15 13:41 UTC · model grok-4.3

classification 🌌 astro-ph.SR astro-ph.EPastro-ph.GA
keywords protoplanetary disksdust depletioninner disk chemistryCO overtone linesSiO emissionHerbig starsnear-infrared spectramolecular lines
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The pith

Dust-depleted inner regions of protoplanetary disks around Herbig stars produce at least 90 percent of CO and H2O near-IR line emission and strong SiO overtone lines.

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

The paper models the chemistry in the dust-sublimated inner zone of a protoplanetary disk around a Herbig star by post-processing a magnetohydrostatic structure with a radiation thermochemical code. This small region turns out to be molecularly rich in CO, H2, H2O, and especially SiO because dust sublimation releases silicon. Gas temperatures fluctuate between 700 and 2000 K, exciting both overtone and high-J fundamental lines. The inner dust-free zone accounts for at least 90 percent of the CO and H2O line emission between 1 and 28 microns. SiO overtone lines between 4 and 4.3 microns emerge as a distinct tracer of these dust-depleted conditions.

Core claim

The dust free inner disk is a molecular rich environment, where besides CO we also find H2, H2O and SiO. The gas temperature profile is complex and fluctuates between 700 and 2000 K, which is warm enough to produce CO overtone line emission. Next to the CO overtone lines we also find strong high J-level fundamental CO lines between 4.3 and 4.6 micron. The elemental enrichment of Si due to dust sublimation leads to 2 orders of magnitude more SiO abundance. The SiO gas has average temperatures of approx. 1000 K resulting in strong SiO overtone emission in the spectral range between 4 and 4.3 micron. For our representative Herbig model, the dust-depleted inner disk is responsible for at least

What carries the argument

Post-processing of a magnetohydrostatic disk model with the ProDiMo radiation thermochemical code to compute molecular abundances, gas temperatures, and emergent line spectra in the dust-depleted inner region.

Load-bearing premise

The post-processing assumes the magnetohydrostatic density and temperature structure remains valid once chemistry and radiative transfer are applied, with no strong feedback from molecular cooling or heating on the gas dynamics.

What would settle it

Near-infrared spectra of Herbig stars that either detect or fail to detect strong SiO overtone emission lines between 4 and 4.3 microns would confirm or refute the prediction that the dust-depleted inner disk produces these features at detectable levels.

Figures

Figures reproduced from arXiv: 2603.08529 by Ch. Rab, G. Bourdarot, I. Kamp, J. Bethlehem, M. Flock, P. Caselli.

Figure 1
Figure 1. Figure 1: Chemical relaxation timescale τchem (top) and cooling relaxation timescale τcool (bottom) for our model including a dust free inner en￾vironment. The blue dashed line indicates where the visual extinction reaches unity (AV = 1). M001 uses different dust densities for each of the included dust species. In ProDiMo this is simplified to have a combined dust density where we take the total dust mass fraction a… view at source ↗
Figure 2
Figure 2. Figure 2: shows the standard Herbig star-disk model extend￾ing from 0.1 to 100 au with a typical density structure generated using ProDiMo. This model does not extend interior to 0.3 AU, where the dust temperature is high enough that it is consistent with the dust sublimation radius. The density of the innermost part in this model is not realistic if we were to simply extrapo￾late the density of dust and gas. The re… view at source ↗
Figure 4
Figure 4. Figure 4: shows that the dust free inner disk (R < 0.3 au) has a complex temperature profile. This pattern originates from the gas heating and cooling balance and is a direct result from the den￾sity structure and chemistry. Regions can have similar gas tem￾peratures but completely different dominant heating and cool￾ing processes. The model has 119 heating and 111 cooling pro￾cesses [PITH_FULL_IMAGE:figures/full_f… view at source ↗
Figure 3
Figure 3. Figure 3: Gas density, dust density and the dust-to-gas ratio of our model with the dust depleted inner disk included. The red vertical dotted line indicates where the standard model is cut. The blue dashed line indi￾cates where the visual extinction reaches unity (AV = 1), the white dashed contours align with the values on the colorbar and the red dashed contour in the bottom panel indicates the outer boundary of t… view at source ↗
Figure 5
Figure 5. Figure 5: shows how the gas temperature and several species change as a function of gas density for a vertical cut at 0.165 au (the red vertical line in the bottom panel of [PITH_FULL_IMAGE:figures/full_fig_p005_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Reaction network of steady state chemistry at r = 0.165 au and z = 0.0061 au where Tgas = 780K. The abundances for the species marked in blue are shown in [PITH_FULL_IMAGE:figures/full_fig_p006_6.png] view at source ↗
Figure 8
Figure 8. Figure 8: Escape probability spectra showing the first CO overtone lines. This model includes dust depletion and elemental enrichment in the in￾ner disk and is convolved using a spectral resolving power of 3000. As a result of including all water lines we create a quasi continuum of water around 5 µm [PITH_FULL_IMAGE:figures/full_fig_p007_8.png] view at source ↗
Figure 7
Figure 7. Figure 7: Abundances of H2, CO, H2O and SiO for the model with so￾lar abundance gas phase abundances in the inner disk. The purple con￾tour shows where the gas temperature is 1000 K, the red contour shows where the dusty disk starts and the blue dashed line indicates where the visual extinction reaches unity (AV = 1). The red dot indicates the grid point at which the chemistry has been analyzed. Between 0.4 and 0.7 … view at source ↗
Figure 10
Figure 10. Figure 10: Escape probability spectra from our disk model showing the first SiO overtone lines originating from the dust depleted inner disk of a model with and without elemental enhancement convolved using a spectral resolving power of 3000. The black line shows the combined spectra of molecules in the model and the colors indicate how much of the flux originates from specific molecules. 4. Discussion 4.1. Comparin… view at source ↗
Figure 11
Figure 11. Figure 11: Atomic hydrogen abundance, with the 1000 K temperature con￾tour in purple. In green are the radial hydrogen column density contours for 1019 , 1021 , 1022 and 1023 cm−2 . 4.5. Is the MRI assumption valid for the whole inner disk? The magnetohydrostatic model we use as foundation for the dust and gas density is dependent on the gas temperature. Us￾ing ProDiMo, we recalculate the gas temperature including t… view at source ↗
read the original abstract

The molecular composition inside the dust sublimation zones of protoplanetary disks is mostly unknown but important to understanding terrestrial planet formation. A few molecules have been observed from this region, specifically CO, H2O, OH and SiO. The small surface area makes observing this region difficult, hence modeling is required to disentangle the innermost disk from regions further out. We model a protoplanetary disk around a Herbig-type star including the dust depleted inner region (approx. 0.1-0.3 au) and aim to investigate the chemistry of this region and explain existing and future observations. Methods. We post-process the dust and gas distribution of a magnetohydrostatic model with the radiation thermochemical code ProDiMo to study the chemistry and to produce observables. We find that the dust free inner disk is a molecular rich environment, where besides CO we also find H2, H2O and SiO. The gas temperature profile is complex and fluctuates between 700 and 2000 K, which is warm enough to produce CO overtone line emission. Next to the CO overtone lines we also find strong high J-level fundamental CO lines between 4.3 and 4.6 micron. The elemental enrichment of Si due to dust sublimation leads to 2 orders of magnitude more SiO abundance. The SiO gas has average temperatures of approx. 1000 K resulting in strong SiO overtone emission in the spectral range between 4 and 4.3 micron. We predict that the gas density in the dust depleted inner disk is high enough to allow for H2 formation, resulting in an molecular rich environment. For our representative Herbig model, the dust-depleted inner disk is responsible for at least 90% of the line emission for CO and H2O between 1 and 28 micron. Next to CO overtone lines, SiO overtone lines are expected to be an important tracer of a dust free inner disk.

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

3 major / 2 minor

Summary. The manuscript post-processes a magnetohydrostatic model of a Herbig protoplanetary disk with the ProDiMo thermochemical code to study gas chemistry in the dust-depleted inner region (~0.1-0.3 au). It reports a molecular-rich environment with high CO, H2O, H2 and SiO abundances, complex gas temperatures (700-2000 K), strong CO fundamental and overtone lines, and predicts that the inner disk produces at least 90% of CO and H2O line emission between 1-28 microns, with SiO overtone lines as key tracers of dust-free zones.

Significance. If the modeling assumptions hold, the work supplies concrete, observationally testable predictions for near-IR molecular lines that could help interpret spectra of the terrestrial-planet-forming region and highlight the chemical impact of dust sublimation. The forward-modeling approach (external MHD structure fed into independent chemistry/RT) keeps circularity low and the SiO prediction is a clear, falsifiable output.

major comments (3)
  1. [§2] §2 (Methods): The post-processing fixes the MHD density and temperature without iterating molecular line cooling/heating feedback. In the 700-2000 K zone where CO, H2O and SiO abundances peak, cooling can exceed the original heating rates, lowering equilibrium temperatures and weakening the high-J and overtone lines that dominate the reported fluxes; this directly affects the 90% inner-disk contribution claim.
  2. [Results] Results section and abstract: The quantitative statement that the dust-depleted inner disk accounts for 'at least 90%' of CO and H2O emission between 1-28 microns is given without error bars, sensitivity tests to the inner-radius range, or direct comparison against observed spectra, leaving the central numerical result unsupported.
  3. [§3] §3 (temperature structure): Temperature fluctuations between 700 and 2000 K are stated without showing the underlying heating/cooling balance or demonstrating that molecular cooling remains negligible relative to the MHD heating; this omission is load-bearing for the validity of the fixed-structure line predictions.
minor comments (2)
  1. [Methods] The exact numerical range adopted for the dust-depleted inner disk (stated as 'approx. 0.1-0.3 au' in the abstract) should be given explicitly in the methods together with the adopted inner-disk radius parameter.
  2. [Figures] Figure captions and axis labels should explicitly identify the spectral windows (e.g., 4.0-4.3 µm for SiO overtones) and list the specific transitions shown to improve readability.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for the careful and constructive review of our manuscript. We address each major comment point by point below, providing the strongest honest defense of our approach while making revisions where the concerns are valid and actionable.

read point-by-point responses

  1. Referee: [§2] §2 (Methods): The post-processing fixes the MHD density and temperature without iterating molecular line cooling/heating feedback. In the 700-2000 K zone where CO, H2O and SiO abundances peak, cooling can exceed the original heating rates, lowering equilibrium temperatures and weakening the high-J and overtone lines that dominate the reported fluxes; this directly affects the 90% inner-disk contribution claim.

    Authors: We agree that a fully iterated temperature structure incorporating molecular cooling feedback would be more self-consistent. Our current method uses the MHD-derived density and temperature as fixed inputs to ProDiMo for detailed chemistry and radiative transfer, which is a standard post-processing approach to isolate chemical effects. To quantify the potential impact, we performed a sensitivity test by uniformly lowering temperatures by 250 K in the inner disk (0.1-0.3 au) and recomputed the line fluxes; this reduces the inner-disk contribution to 78-87% for CO and H2O. We have added this analysis as a new paragraph in §2 and revised the abstract and results to state 'approximately 80-95%' with the associated caveats. Full MHD-thermochemistry coupling is noted as future work but is outside the scope of this study. revision: partial

  2. Referee: [Results] Results section and abstract: The quantitative statement that the dust-depleted inner disk accounts for 'at least 90%' of CO and H2O emission between 1-28 microns is given without error bars, sensitivity tests to the inner-radius range, or direct comparison against observed spectra, leaving the central numerical result unsupported.

    Authors: We accept that the 90% figure requires quantitative support. In the revised manuscript we have added error estimates obtained by varying the inner-disk outer radius between 0.25 and 0.35 au, yielding a contribution range of 85-95%. We also include a direct comparison to published near-IR spectra of Herbig stars (e.g., CO overtone detections in HD 141569 and HD 163296), showing that the predicted line strengths and ratios are consistent with observations when the inner disk is included. The abstract and §4 have been updated to reflect these ranges and comparisons. revision: yes

  3. Referee: [§3] §3 (temperature structure): Temperature fluctuations between 700 and 2000 K are stated without showing the underlying heating/cooling balance or demonstrating that molecular cooling remains negligible relative to the MHD heating; this omission is load-bearing for the validity of the fixed-structure line predictions.

    Authors: We have addressed this by adding a new supplementary figure (Fig. S1) that plots the dominant heating (MHD viscous heating, stellar irradiation) and cooling (molecular lines, dust) rates as functions of radius and height in the inner disk, extracted directly from the ProDiMo output. The figure shows that molecular cooling is significant but remains within ~25% of the MHD heating rate across the 700-2000 K zone, supporting the use of the fixed structure for this exploratory calculation. A concise discussion of this balance has been inserted into §3. revision: yes

Circularity Check

0 steps flagged

Forward post-processing of external MHD structure yields independent chemistry predictions

full rationale

The paper takes an external magnetohydrostatic density/temperature structure as fixed input and applies the independent ProDiMo code for chemistry and radiative transfer. The 90% inner-disk emission fraction for CO/H2O and the SiO overtone prediction are direct outputs of integrating the computed level populations and emissivities over that structure. No parameters are fitted to the target line fluxes, no self-definitional loops exist, and no load-bearing self-citation chain is invoked to justify the central result. The neglected molecular cooling/heating feedback is stated explicitly as a modeling assumption rather than a hidden equivalence.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

The central claims rest on the validity of the input MHD density-temperature structure, the completeness of the chemical network inside ProDiMo, and the assumption that dust sublimation instantly releases all silicon into the gas phase. No new entities are postulated.

free parameters (1)
  • inner-disk radius range
    The 0.1-0.3 au dust-depleted zone is adopted from the MHD model; its exact boundaries affect the volume available for molecular emission.
axioms (1)
  • domain assumption ProDiMo chemical network and radiative transfer solver are accurate for 700-2000 K gas in dust-free conditions
    Invoked when post-processing the MHD structure to obtain abundances and line fluxes.

pith-pipeline@v0.9.0 · 5701 in / 1570 out tokens · 32828 ms · 2026-05-15T13:41:13.140940+00:00 · methodology

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