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arxiv: 2605.22926 · v1 · pith:MRTTF5TCnew · submitted 2026-05-21 · 🌌 astro-ph.EP · astro-ph.SR

JWST-DECO: The Impact of Accretion on Mid-Infrared Observable Water in Planet-forming Disks

Jenny K. Calahan , Tarisai Dziire , Karin \"Oberg , Andrea Banzatti , L. Ilsedore Cleeves , Felipe Alarc\'on , Geoffrey A. Blake , Mar\'ia Jos\'e Colmenares
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Camilo Gonz\'alez-Ruilova Aashish Gupta Claudio Hern\'andez-Vera Till Kaeufer Sebastiaan Krijt Charles J. Law Tamara Molyarova Joe Williams
This is my paper

Pith reviewed 2026-05-25 02:03 UTC · model grok-4.3

classification 🌌 astro-ph.EP astro-ph.SR
keywords protoplanetary diskswater linesaccretion luminositymid-infrared spectroscopyJWSTthermo-chemical modelingplanet formation
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The pith

Accretion luminosity enlarges the mid-infrared water emitting area in protoplanetary disks, increasing the observable water mass.

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

The paper adds an accretion module to the DALI thermo-chemical code to model how viscous accretion and central luminosity affect the 2D temperature and water chemistry in planet-forming disks. It reproduces the observed rise in water line flux with accretion rate, strongest for hot water and weaker for warm and cool water. The increase stems from a larger emitting area caused by higher central luminosity, while midplane viscous heating leaves observable water mass unchanged. At higher accretion rates some cool and warm water becomes hidden under an optically thick dust surface and is confined to smaller volumes. This directly informs how JWST mid-IR spectra trace the water available during planet formation.

Core claim

Incorporating accretion luminosity into disk models reproduces the trend of increasing observed water mass with accretion rate. The trend arises because accretion raises central luminosity and thereby expands the emitting area; viscous heating confined to the midplane produces no change in observable water. The correlation is strongest for hot water, intermediate for warm water, and weakest for cool water because part of the cooler populations is obscured by increased dust optical depth.

What carries the argument

DALI thermo-chemical code with added accretion module that computes 2D temperature structure, water chemistry, and observable line fluxes under varying accretion rates and luminosities.

If this is right

  • Observed water mass increases with accretion rate, with the correlation strongest for hot water, weaker for warm water, and weakest for cool water.
  • The trend is produced entirely by the accretion-driven rise in central luminosity that enlarges the emitting area.
  • Viscous heating localized to the midplane has no measurable effect on the observable water mass.
  • At higher accretion rates some cool and warm water populations are hidden beneath an optically thick dust surface and restricted to a smaller disk volume.

Where Pith is reading between the lines

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

  • Mid-IR water-line interpretations of total disk water content will require correction for the accretion state of each system.
  • Higher-accretion disks may deliver a larger effective water reservoir to the inner planet-forming zone because the emitting region expands.
  • Comparing water lines across disks that share similar luminosities but differ in accretion rate would directly test whether central luminosity is the controlling variable.

Load-bearing premise

The DALI code with the accretion module accurately captures the 2D temperature structure, water chemistry, and observable line fluxes without dominant contributions from unmodeled processes such as dust evolution or non-viscous heating.

What would settle it

Observations of water line fluxes in disks with matched central luminosity but differing accretion rates that show no corresponding increase in water mass, or models omitting the central-luminosity term that still reproduce the observed trend.

Figures

Figures reproduced from arXiv: 2605.22926 by Aashish Gupta, Andrea Banzatti, Camilo Gonz\'alez-Ruilova, Charles J. Law, Claudio Hern\'andez-Vera, Felipe Alarc\'on, Geoffrey A. Blake, Jenny K. Calahan, Joe Williams, Karin \"Oberg, L. Ilsedore Cleeves, Mar\'ia Jos\'e Colmenares, Sebastiaan Krijt, Tamara Molyarova, Tarisai Dziire, Till Kaeufer.

Figure 1
Figure 1. Figure 1: The stellar spectra of a star with the same stellar mass, luminosity, and effective temperature as AS 209 [black] and the addition of differing levels of accretion rate [brown through yellow]. average, as these are also found around Class II proto￾planetary disks, and one step above, as anything beyond 10−7 M⊙/yr would be in line with an active protostar or outbursting source (L. Hartmann & S. J. Kenyon 19… view at source ↗
Figure 2
Figure 2. Figure 2: Left: The gas temperature profile of a model with no accretion, and contour lines at 155 and 80 K. Middle: The factor representing the increase in gas temperature with the addition of viscous heating originating at the midplane with 10−8 M⊙/yr . Right: The factor representing the increase in gas temperature due to the accretion luminosity component to the stellar spectrum. 0 2 4 radius [au] 0.0 0.5 1.0 1.5… view at source ↗
Figure 3
Figure 3. Figure 3: 2D temperature plots across different accretion rates, with both viscous heating and Lacc implemented. The temperature contours of 155 K and 80 K approximately trace the H2O and CO2 sublimation fronts, respectively. All plots are shown with the same color-scale. the highest accretion rate (now at 1 au at 10−7 M⊙/yr), atoms dominate the gas component z/r⪆0.3. The change in disk temperature due to differing … view at source ↗
Figure 4
Figure 4. Figure 4: The radial temperature of the disk across the midplane (top) and z/r=0.36 (bottom), with each line corre￾sponding to a different accretion rate. Water is the most abundant volatile species frozen-out onto dust grains in disk, and its snow surface has been shown to alter different aspects of planet formation (e.g. F. J. Ciesla & J. N. Cuzzi 2006; A. J. Cridland et al. 2016; J. Dra˙zkowska & Y. Alibert 2017)… view at source ↗
Figure 5
Figure 5. Figure 5: Top: The location of the water snowline, as defined by where the gas-phase H2O abundances is equal to the ice-phase H2O. Middle: The associated gas density along each of the water snow surfaces for each accretion rate. Bot￾tom: The temperature along each water snowline for each accretion rate. The snowline intersects the midplane at dif￾ferent temperatures for each accretion rate. From lowest to highest ac… view at source ↗
Figure 6
Figure 6. Figure 6: 2D number densities of gas-phase water throughout the disk (top). The yellow, orange, and red contours correspond to 200, 400, and 900 K, delineating the cool, warm, and hot reservoirs respectively. The black contour follows where the disk is optically thick to IR wavelengths (10 µm). The bottom plot shows the total mass of water surrounding each of these contours ±20% in units of Earth’s Oceans, and the t… view at source ↗
Figure 7
Figure 7. Figure 7: The gas-phase water number density in our model with an accretion rate of 10−8 M⊙/yr, with different defini￾tions of the snow surface. Black corresponds to the isother￾mal contour of 155 K, orange to the theoretical freeze-out temperature (see Equation 1), and blue is where the abun￾dance of gas-phase and ice-phase water are equal. trace amounts of O2. The spatial difference between the theoretical water-i… view at source ↗
Figure 8
Figure 8. Figure 8: Observable water mass found in disks around M and K stars in Lupus and Taurus, as calculated from C. Romero-Mirza (2025), and their corresponding Lacc [L⊙]. Fits to the data with 95% confidence intervals are in teal. Dashed line is the observable water mass from the DALI K-star model in from this work for the cold, warm, and hot populations. it is the total central luminosity that alters the tempera￾ture a… view at source ↗
Figure 9
Figure 9. Figure 9: The observed water mass (in Earth’s Oceans) versus accretion rate in the DALI models, with the dashed line showing the evolution with only heating due to midplane accretion, and the solid line as our final results with both midplane and illuminated contribution from Lacc. • Molecular snow surfaces will be pushed outward to larger radii with increasing accretion rate. The freeze-out temperature at the midpl… view at source ↗
read the original abstract

The inner few au of a protoplanetary disk hosts the majority of observed exoplanets and is the primary planet-forming zone of the disk. The mid-IR spectra of disks, with its rich forest of water lines, provides key insights into the composition of forming planets. One of the strongest trends seen with data from Spitzer and now JWST is a correlation between the increase in water line flux and accretion luminosity of a system. We set out to reproduce and understand this trend by adding an accretion module to the thermo-chemical code DALI, and explore how viscous accretion heating and the addition of accretion luminosity impacts the 2D temperature structure and the observable water reservoir. We reproduce the trend that the observed water mass increases with accretion rate, with hot, warm, and cool water being more to less strongly correlated, respectively. Our model suggests that these trends are due to an increased emitting area with accretion rate, with some of the cool and warm population becoming hidden underneath an optically thick dust surface and being constrained to a smaller disk volume. This trend is driven by the accretion-related increase in central luminosity, while viscous heating centralized to the midplane has no impact on observed water mass.

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 / 2 minor

Summary. The manuscript augments the DALI thermo-chemical code with an accretion module to explore how viscous heating and accretion luminosity affect the 2D temperature structure, water chemistry, and mid-IR observable water reservoir in protoplanetary disks. It reports reproducing the observed positive correlation between water line flux and accretion rate (strongest for hot water, weaker for warm and cool components) and attributes the trend to an accretion-driven increase in emitting area, with some cool/warm water hidden beneath an optically thick dust surface, while finding no effect from midplane viscous heating.

Significance. If the modeled mechanism holds, the work supplies a physical explanation for a key JWST/Spitzer trend in disk water emission, with direct implications for interpreting mid-IR spectra and linking accretion to the conditions in the planet-forming zone. The explicit separation of central-luminosity versus midplane-viscous-heating effects is a useful diagnostic contribution.

major comments (2)
  1. [Abstract] Abstract: the statement that the model 'reproduces the trend' that observed water mass increases with accretion rate is not accompanied by any quantitative metrics (correlation coefficients, slope comparisons, or residuals against the Spitzer/JWST data points), which is load-bearing for the central claim of successful reproduction.
  2. [Results (model runs)] The attribution of the trend solely to central-luminosity-driven changes in emitting area (with viscous heating having 'no impact') rests on the assumption that the added accretion module correctly updates the 2D temperature and dust optical-depth structure; no explicit test or figure isolating the luminosity versus viscous-heating contributions is referenced to confirm this separation.
minor comments (2)
  1. [Methods] Clarify the exact implementation of the accretion luminosity (e.g., how it is added to the central source spectrum and whether it affects the stellar radius or effective temperature) so readers can assess consistency with standard accretion prescriptions.
  2. [Abstract] The abstract mentions 'hot, warm, and cool water' populations but does not define the temperature or radial boundaries used to classify them; this notation should be made explicit early in the text.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive comments, which help clarify the presentation of our results. We respond to each major comment below and indicate the revisions that will be incorporated.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the statement that the model 'reproduces the trend' that observed water mass increases with accretion rate is not accompanied by any quantitative metrics (correlation coefficients, slope comparisons, or residuals against the Spitzer/JWST data points), which is load-bearing for the central claim of successful reproduction.

    Authors: We agree that the abstract would benefit from quantitative support for the reproduction claim. The manuscript already shows the trend via the modeled water-mass increase with accretion rate and the relative strengths (hot strongest, then warm, then cool). We will revise the abstract to report the model-derived correlation coefficients for each water component and note their consistency with the observed direction and ordering of the Spitzer/JWST trends. revision: yes

  2. Referee: [Results (model runs)] The attribution of the trend solely to central-luminosity-driven changes in emitting area (with viscous heating having 'no impact') rests on the assumption that the added accretion module correctly updates the 2D temperature and dust optical-depth structure; no explicit test or figure isolating the luminosity versus viscous-heating contributions is referenced to confirm this separation.

    Authors: The separation was performed by dedicated model suites: one with accretion luminosity added only to the central source (viscous heating term disabled) and one with only the midplane viscous-heating term active. These runs confirm that only the central-luminosity change alters the observable water reservoir. We will add explicit references to these configurations in the results section and include a new figure (or supplementary panel) that directly compares the two cases to make the isolation transparent. revision: yes

Circularity Check

0 steps flagged

No significant circularity detected

full rationale

The paper adds an accretion module to the established DALI thermo-chemical code and runs simulations to reproduce the observed water-accretion correlation; the claimed mechanism (central luminosity increasing emitting area while midplane viscous heating has no effect) is an output of those simulations rather than a fitted parameter or self-referential definition. No load-bearing self-citation, ansatz smuggling, or renaming of known results is indicated in the abstract or claim text, and the derivation remains self-contained within the independent physical model.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The central claim rests on the validity of the base DALI code and the implementation details of the accretion module, neither of which are specified in the abstract; no free parameters or invented entities are identifiable from the given text.

axioms (1)
  • domain assumption The DALI thermo-chemical code correctly computes 2D disk temperatures and water abundances under added accretion luminosity
    Invoked when the paper states that the model reproduces the observed trend and isolates the role of central luminosity.

pith-pipeline@v0.9.0 · 5836 in / 1265 out tokens · 48315 ms · 2026-05-25T02:03:56.514407+00:00 · methodology

discussion (0)

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Lean theorems connected to this paper

Citations machine-checked in the Pith Canon. Every link opens the source theorem in the public Lean library.

  • IndisputableMonolith/Cost/FunctionalEquation.lean washburn_uniqueness_aczel unclear
    ?
    unclear

    Relation between the paper passage and the cited Recognition theorem.

    We set out to reproduce and understand this trend by adding an accretion module to the thermo-chemical code DALI, and explore how viscous accretion heating and the addition of accretion luminosity impacts the 2D temperature structure and the observable water reservoir.

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Reference graph

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