CO2-rich protoplanetary discs as a probe of dust radial drift & trapping

Andrew D. Sellek; Ewine F. van Dishoeck; Marissa Vlasblom

REVIEW 1 major objections 4 minor 5 cited by

CO2-rich protoplanetary discs as a probe of dust radial drift & trapping

T0 review · 1 major / 4 minor · reviewed 2026-08-12 · deepseek-v4-flash

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Pith's one-line read Drifting ice grains make planet-forming discs turn CO2-rich on million-year timescales, and the CO2/H2O ratio marks where dust traps sit.

desk verdict Solid modeling paper with a useful new tracer, but the headline correlation rests on an explicitly flagged pure-CO2 ice assumption that the authors never test. read the letter →

arxiv 2412.01895 v2 pith:PPV7YD5F submitted 2024-12-02 astro-ph.EP

Andrew D. Sellek , Marissa Vlasblom , Ewine F. van Dishoeck This is my paper · ORCID

classification astro-ph.EP

keywords protoplanetarydiscsdustradialdrifttrappingsnowlinesCO2/H2Oratiomid-infraredspectroscopyicesublimationdiscchemicalevolution

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

This paper argues that the chemical diversity seen in the inner regions of planet-forming discs—some dominated by water vapour, others by carbon dioxide—can arise from the inward drift of dust grains carrying ices, and that the ratio of CO2 to H2O is a practical tracer of where dust trapping occurs. Using a 1D disc evolution model, the authors show that discs first become water-rich as water ice sublimates at its snow line, then turn CO2-rich as the water vapour drains onto the star and CO2 ice drifts inward from its more distant snow line. Dust traps—pressure bumps created by gaps in the gas disc—interrupt this delivery, speed up the transition, and raise CO2/H2O, with the size of the effect depending on the gap's radius and formation time. Synthetic mid-infrared spectra analysed with standard slab models show that the CO2/H2O column-density ratio is far less affected by dust obscuration than either molecule's absolute column density, making it the more reliable observable. If the picture is right, the ratio offers a way to read both the age of a disc and the location of its dust traps from JWST spectra.

What carries the argument

The load-bearing mechanism is the snow-line sequence, in which each ice sublimates at a characteristic radius set by its binding energy—H2O closest to the star, CO2 further out—and the released vapour is then drained onto the star on a viscous timescale proportional to that radius. The models implement this with a 1D viscous evolution code using the two-population dust model, and represent dust traps as Gaussian perturbations to the effective viscosity that create pressure bumps. The paper's central diagnostic is the CO2/H2O column-density ratio $N_{\mathrm{CO_2}}/N_{\mathrm{H_2O}}$: because the dust that delivers H2O also adds continuum opacity that hides the water, absolute columns are unreliable, whereas the ratio largely cancels this obscuration and tracks the underlying chemistry.

What would settle it

A population survey combining ALMA gap radii with JWST MIRI-MRS measurements of CO2/H2O column-density ratios could settle the claim: if discs at 1–3 Myr show no positive correlation between the ratio and gap radius, the predicted dependence fails. The mechanism would also collapse if experiments or observations show that the majority of CO2 desorbs at the H2O sublimation temperature rather than at its pure-phase temperature.

Watch

Extended reading notes

Core claim

The central claim is that inward-drifting pebbles deliver H2O and CO2 ices to the inner disc in a volatility-ordered sequence: H2O sublimates closest to the star and briefly dominates, then its vapour is accreted onto the star on a viscous timescale of roughly 0.25 Myr, while CO2 continues to arrive from its snow line further out, leaving the inner disc CO2-rich on Myr timescales. Introducing a dust trap cuts off the pebble flux, and because H2O is drained faster than CO2, traps raise the CO2/H2O vapour ratio; close-in or early-opening gaps block more of the CO2 ice and therefore produce smaller increases. The paper further claims this behaviour survives in observable form: the CO2/H2O column-density ratio retrieved from 0D LTE slab fits to synthetic MIR spectra mirrors the underlying vapour-mass ratio and depends only weakly on dust continuum obscuration, so it can serve as a tracer of radial drift and trapping in real discs.

Load-bearing premise

The predicted separation of the water-rich and CO2-rich phases—and therefore the diagnostic power of the CO2/H2O ratio—rests on the assumption that CO2 ice is pure and sublimates at its own snow line; if most CO2 is trapped in polar water ice and released together with water, the two delivery episodes would merge and the ratio would lose its sensitivity to gap location.

Editorial extensions

If this is right

CO2-dominated inner-disc spectra should be a common late stage of disc evolution, appearing on ~1–3 Myr timescales even without gaps, as H2O drains onto the star faster than CO2 arrives.
Dust traps should raise the CO2/H2O ratio, and in discs with early-formed traps the ratio should increase with gap radius during the 1–3 Myr window, offering a direct observational test with ALMA gap catalogues.
Traps opened close to the star or very early block more CO2 ice and produce smaller ratio increases, so the ratio can constrain both the location and formation time of substructure.
Because the ratio is only weakly sensitive to dust continuum obscuration, retrieving it from weak features such as CO2 hot bands or 13CO2 should trace the bulk delivered chemistry better than absolute water or CO2 column densities.
Trap formation delayed beyond roughly 0.1 Myr weakens or reverses the ratio–gap-location trend, so the observed strength of the correlation constrains when substructures formed.

Reading between the lines

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

A null result in the predicted correlation would independently point to CO2 being largely locked in polar water ice, or to surface-layer chemistry resetting delivered abundances; 2D thermochemical models could distinguish these.
If the correlation is confirmed, it would favour early-forming, non-planetary dust traps such as MHD zonal flows, because planets struggle to open gaps before ~0.1 Myr.
The time at which a disc switches from water-dominated to CO2-dominated encodes the viscous timescale at the water snow line, so the ratio could serve as a chemical age indicator for individual discs.
The paper's 'traffic jam' scenario implies water column densities are fixed by the ice-to-dust ratio rather than by delivered water mass; unusually high observed water columns would therefore signal dust loss or decoupling inside the snow line.

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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Desk Editor's Note

read the letter

Bottom line: this is a careful, useful modeling study. It gives JWST observers a new diagnostic—the CO2/H2O column density ratio—that may connect inner-disc chemistry to outer-disc dust traps. The central claim is well argued within the model's assumptions, and the paper is honest about the main caveat, but that caveat is more load-bearing than the authors let on.

What's new: Booth, Kalyaan, and Mah did H2O and C/O effects of traps; this paper adds explicit CO2, a systematic grid of gap radii and formation times, and forward modeling into synthetic MIRI-MRS spectra with slab-model retrieval. That last step is valuable: it tests what an observer would actually measure, and the finding that the ratio survives dust-obscuration effects is the strongest part. The code is released at a tagged version, the initial ice abundances come from independent protostellar ice observations, and the binding energies from lab experiments; the comparison to observed discs is made after the models are run. No circularity problem.

The weakest spot is exactly what the authors flag in §2.3.3: they assume pure, layered ices with single desorption temperatures, and then note that pure CO2 ice is never more than ~20% of the CO2 ice budget, usually <10%. If most CO2 is in polar H2O ice and is released near the H2O snowline, the H2O-rich then CO2-rich phase separation weakens, and the NCO2/NH2O vs Rgap correlation loses its diagnostic power. The authors argue for volcano desorption and segregation, but they also call their choice the 'most extreme scenario.' A mixed-ice model variant would have settled this; its absence leaves the domain of validity unclear. A second soft spot is scenario dependence: the positive correlation at 1–3 Myr appears in Scenarios 1 and 3, but in Scenario 2 the ratio behaves differently and column densities overshoot observations by orders of magnitude. The paper acknowledges this, but it means the diagnostic is only as good as the assumption that the dust dynamics are in the Scenario 1/3 regime.

The observational comparison is appropriately cautious—small, heterogeneous sample, different fitting methods—and they don't overclaim. The discussion of what could produce CO2-dominated spectra is balanced.

Who this is for: anyone interpreting MIRI-MRS spectra of T Tauri discs, or trying to connect ALMA substructure to inner-disc chemistry. It deserves a serious referee; I'd send it out. I'd also suggest the authors add a mixed-ice run in revision, because it directly tests the headline prediction.

Referee Report

1 major / 4 minor

Summary. The manuscript uses a 1D protoplanetary disc evolution code with a two-population dust model and molecular ice tracers to model how radially drifting dust and dust traps in gas gaps shape the inner-disc H2O and CO2 vapour abundances, and it post-processes the resulting structures with 0D LTE slab spectral models to predict observable MIR column densities. The central claims are that discs evolve through an H2O-rich phase into a CO2-rich phase as H2O vapour is accreted and CO2 is advected inward from its snowline, that dust traps hasten this transition and raise CO2/H2O, and that the retrieved NCO2/NH2O ratio is a more robust tracer of drift/trapping than individual column densities and may correlate with gap location at 1–3 Myr. The model predictions are compared qualitatively to a small sample of JWST MIRI-MRS discs, and the code is released at a tagged version.

Significance. If the predicted relationship between inner-disc CO2/H2O and the presence/location of dust traps holds, it would offer a new population-level observational diagnostic for the role of radial drift and substructure formation in setting the volatile chemistry available to planet formation. The paper’s strengths are its clear model specification, the explicit exploration of three dust-evolution scenarios, the careful treatment of continuum obscuration in the synthetic spectra, and the release of the model code. The authors are also candid about limitations that they do not model, such as vertical thermal structure and chemical reprocessing. The main risk to the central claim is the assumption of pure, successively layered CO2 ice, which is acknowledged in the text but not subject to a sensitivity test.

major comments (1)

[§2.3.3 and Figs. 9–10] The central prediction—an H2O-rich phase followed by a CO2-rich phase, and the positive NCO2/NH2O–Rgap trend at 1–3 Myr—relies on the assumption stated in §2.3.3 that CO2 ice is pure and has a single desorption temperature at its own snowline (about 2.2 au in the model). The text immediately notes that protostellar ice observations imply pure CO2 is never more than about 20% of CO2 ice (usually <10%), with the polar, H2O-rich phase most abundant, and that the paper assumes the most extreme scenario. If a substantial fraction of CO2 is trapped in polar H2O ice and released near the H2O snowline at about 0.47 au, both molecules would enter the same inner reservoir and be advected on the same short viscous timescale (Eq. 19), so the CO2/H2O ratio would tend to track the initial ice abundance ratio and lose the dependence on Rgap shown in Figs. 9 and 10. The qualitative arguments for volcano desorption and segregation are plausible but do not provide a quantitative bound on the polar-phase fraction needed to preserve the correlation. I request a sensitivity test with a mixed-ice prescription—for example, a parametrized fraction of CO2 that co-desorbs with H2O—or an equivalent demonstration that the predicted ratio and its trend with gap location survive for observationally motivated ice-phase distributions.

minor comments (4)

[§4.3.3] The statement that 'the trends with respect to H2O are lost' is too absolute, since Fig. 9 shows a weak late-time negative trend in the H2O column density for the most distant gaps; please qualify the sentence.
[§2.2.2] Equation (12) contains a factor (1−b) in the denominator, so the special case b = 1 is singular; please either exclude it explicitly or comment on the limiting behaviour.
[Fig. 3 caption] The markers labeled 'RM24 Compact' and 'RM24 Extended' are not described in the caption; please add one sentence explaining the observational estimates they represent.
[Throughout] The manuscript uses both 'snowline' and 'snow line'; please unify the spelling for consistency.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the model predictions are generated from independent physical inputs and are compared with observations only after the models are run.

full rationale

The derivation chain is self-contained rather than circular. Initial ice abundances (Table 4) are set from independent protostellar ice observations and elemental abundance references (Öberg et al. 2011; Boogert et al. 2015; McClure et al. 2023; Minissale et al. 2022); binding energies and desorption prefactors come from laboratory TPD experiments, and the transport code advects ices and vapour with the standard viscous and drift velocities (Eqs. 3-5). No model parameter is fitted to the observed N_CO2/N_H2O values in Table 5; indeed the models generally overpredict absolute column densities, which the authors explicitly note in Section 4.2.1, the opposite of a tuned fit. The predicted correlation with gap location is produced by the trap interrupting the pebble flux, and the numerical trends are checked against analytical scalings (Eqs. 23 and 27) rather than assumed. The pure-ice assumption in Section 2.3.3 is explicitly flagged by the authors as 'the most extreme scenario', and is a domain-of-validity caveat: if CO2 co-desorbs from polar H2O ice, the phase separation would weaken and the predicted ratio would change, but this does not mean the model's output is defined in terms of its input. The only self-citations are to the publicly available DiscEvolution code and to the authors' earlier code-development papers; these are reproducible implementation references, not a load-bearing uniqueness theorem. No circular step can be exhibited from the paper's own equations.

Assumptions & free parameters 8 free parameters · 7 assumptions · 0 invented entities

The central predictions rest on a chain of modeling choices, including dust growth prescriptions, chemistry neglect, pure-ice desorption, and vertical isothermality. Most are drawn from prior literature or experiments and are explicitly discussed; the pure-ice and no-chemistry assumptions are the most consequential for the claimed H2O-to-CO2 sequence.

free parameters (8)

alpha (viscosity) = 10^-3 (Scenarios 1 and 3); 10^-4 (Scenario 2)
Chosen, not fitted. Sets the gas advection timescale and the timing of the H2O-to-CO2 transition (Equation 19).
alpha_t (turbulence) = 10^-3, 10^-4, 10^-5
Chosen. Sets the dust fragmentation equilibrium and the St/alpha coupling; controls the traffic jam and dust leakage.
u_frag,ice (icy grain fragmentation velocity) = 10 m/s (Scenario 1); 1 m/s (Scenarios 2 and 3)
From experimental ranges; determines whether icy grains decouple and create a traffic jam inside the H2O snowline.
f_small (small dust mass fraction) = 0.25 (fragmentation-limited); 0.03 (drift-limited)
Calibrated from Birnstiel et al. (2012); controls the small-dust continuum opacity and the diffusive trap leakage.
Initial H2O ice abundance = 0.2 x O/H = 1.1e-4
Chosen intermediate between protostellar ice observations and chemical models; sets the H2O column density benchmark.
Initial CO2 ice abundance = 0.09 x C/H = 2.1e-5
From ice observations toward protostellar envelopes; sets the CO2 reservoir and the late-time CO2/H2O ratio.
Gap depth A and width factor = A = 10; w_gap = sqrt(2) H
Chosen to be in the effective trapping regime while keeping computation feasible; affects dust leakage and the gap-location trends.
Trap growth parameters = b_grow = 2/3; t_grow,f = 10^4 yr
From pebble accretion growth scaling; sets the formation-time dependence explored in Figure 10.

assumptions (7)

domain assumption The two-population dust model of Birnstiel et al. (2012) with fixed small-dust fraction f_small.
Invoked in Section 2; determines how much dust is coupled to the gas and sets the continuum opacity and trap leakiness. The fixed f_small is acknowledged as an approximation that underpredicts diffusive leaking through gaps.
domain assumption No chemical reactions between species; only transport and freeze-out/desorption change tracer abundances.
Stated in Section 2.3; validated in Appendix A for midplane timescales, but surface-layer photochemistry is not modeled and could alter the observable ratio.
domain assumption Ices are pure and successively layered with a single desorption temperature, with CO2 not trapped in polar H2O ice.
Section 2.3.3; this assumption produces well-separated H2O and CO2 snowlines and is load-bearing for the sequential H2O-then-CO2 phase evolution.
domain assumption Vertically isothermal temperature profile and vertically well-mixed molecules for the synthetic spectra.
Section 3.2; the visible column density N_vis depends on the vertical Gaussian distribution of molecules and the MIR tau = 1 surface. The paper calls the isothermal assumption its most major limitation.
domain assumption 0D LTE slab models are adequate to retrieve column densities from the synthetic spectra and to compare with observed MIRI-MRS fits.
Section 3.3; used to define the observable CO2/H2O column density ratio, with the caveat that real spectra contain multiple temperature components.
domain assumption The Gaussian gap perturbation parametrizes a planet-carved dust trap with width w_gap = sqrt(2) H and depth A = 10.
Section 2.2.1; the trap properties control how much dust and ice are blocked and how much leaks. The authors note real gaps are leakier than the fixed-f_small model captures.
domain assumption Initial volatile abundances follow Booth et al. (2017) Case 2, updated with experimental binding energies.
Section 2.3.2; the initial H2O and CO2 ice abundances set the absolute column densities and the late-time ratio.

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Cite this review

Pith. "Pith review of CO2-rich protoplanetary discs as a probe of dust radial drift & trapping." pith.science (2026). https://pith.science/paper/PPV7YD5F

@misc{pith2026241201895,
  author       = {Pith},
  title        = {Pith review of: CO2-rich protoplanetary discs as a probe of dust radial drift & trapping},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/PPV7YD5F}},
  note         = {Machine review of arXiv:2412.01895}
}

read the original abstract

MIR spectra imply considerable chemical diversity in the inner regions of protoplanetary discs: some are H2O-dominated, others by CO2. Sublimating ices from radially drifting dust grains are often invoked to explain some of this diversity, particularly the H2O-rich discs. We use a 1D protoplanetary disc evolution code to model how radially drifting dust grains that transport ices inwards to snowlines impact the chemistry of the inner regions of protoplanetary discs. We explore differences between smooth discs and those where radial drift is impeded by dust trapping outside gas gaps and quantify the effects of gap location and formation time. Discs evolve through an initial H2O-rich phase due to sublimating ices, followed by a CO2-rich phase as H2O vapour advects onto the star and CO2 advects into the inner disc from its snowline. The inclusion of traps hastens the transition between the phases, raising the CO2/H2O ratio; gaps opened early or close-in produce lower increases by blocking more CO2 ice from reaching the inner disc. This leads to a potential correlation between CO2/H2O and gap location that occurs on Myr timescales for fiducial parameters. We produce synthetic spectra from the models which we analyse with 0D LTE slab models to understand how this evolution may be expressed observationally. Whether the evolution can be retrieved depends on the contribution of dust grains to the optical depth: dust that couples to the gas after crossing the H2O snowline can add to the continuum optical depth and obscure the delivered H2O, largely hiding the evolution in its visible column density. However, the CO2/H2O visible column density ratio is only weakly sensitive to dust continuum obscuration. This suggests it may be a clearer tracer of the impact of transport on chemistry than individual column densities for spectra that show weak features probing deep enough in the disc. (Abridged)

Figures

Figures reproduced from arXiv: 2412.01895 by the authors.

**Figure 1.** Cartoon depicting the three scenarios explored in this work. The thickness of the yellow arrows connecting the disc and star represents the magnitude of α controlling the gas evolution and accretion. The turbulence strength is indicated by the thickness and size of the circular arrow in the bottom right. The speckled region represents the dust with the brown colour indicating dry dust and the light blue colour indic… view at source ↗

**Figure 2.** Example surface density profiles of gas (solid, initial value only) and (small+large) dust (dashed, at different times) for each of the three scenarios, illustrating the changing dust surface density distribution due to radial drift. The dip in the gas surface density signifies the gap, in this case at Rgap = 30 au and after 0.1 Myr (red), dust has begun to accumulate in the trap at its outer edge. The traffic jam t… view at source ↗

**Figure 3.** Evolution of the pebble component of the disc. Right: Total dust mass (including that which has crossed the inner disc boundary and accreted onto the star) inside the initial locations of the H2O (solid) and CO2 (dashed) snow lines (right). Left: Pebble flux across the H2O snow line. Included for reference are the values from [PITH_FULL_IMAGE:figures/full_fig_p009_3.png] view at source ↗

Figures from the paper (7 more)

**Figure 4.** Figure 4: Radial distribution of the H2O (blue), CO2 (bright green), and CH4 (olive green) after 1 kyr of evolution (left) and 0.1 Myr of evolution in a smooth disc in Scenario 1. Solid lines indicate molecules in the solid (ice) phase, and dashed lines molecules in the gas (vap…

**Figure 5.** Figure 5: Evolution of the vapour mass of H2O (blue), CO2 (bright green), and CH4 (olive green) normalised to their initial values for a smooth disc in Scenario 1. The vertical dotted lines mark the times that each molecule reaches its peak vapour mass and the rightward arrows i…

**Figure 6.** Figure 6: Example of the construction of a synthetic spectrum and the retrieval of parameters using 0D LTE slab model fits. The top panels show the temperature profile (left) and the column density profiles after 104 yr (right) for small dust (black) and total (solid) and visibl…

**Figure 7.** Figure 7: Relationships between the vapour mass and the column density measured using slab fits for H2O (left) and CO2 (right) for a smooth disc model in Scenarios 1 (purple), 2 (gold), and 3 (red). The curves shown are traversed anticlockwise. the same inside the snow line as w…

**Figure 8.** Figure 8: Evolution of the vapour mass (left) and column density (right) for CO2 (top row), H2O (middle row), and their ratio (bottom row) for discs with traffic jams inside the water snow line (Scenario 1). The grey line represents a smooth disc with no traps, while the blues l…

**Figure 9.** Figure 9: Trends of CO2 (top) and H2O (middle) vapour masses (left) and column densities (right) and their ratio (bottom) with Rgap at different stages of evolution for discs with traffic jams inside the water snow line (Scenario 1). The initial condition is in grey, while incre…

**Figure 10.** Figure 10: Dependence of the CO2/H2O column density ratio on gap location at different snapshots in the disc evolution. The panels show models in which the traps are fully developed at successively later times. 4.3.4. Dependence on trap formation time Having identified the CO2/…

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Forward citations

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Pith tools

Reviewed August 12, 2026 · model on record in the stance chip above.

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, " * write output.state after.block = add.period write newline

ENTRY address archiveprefix author booktitle chapter edition editor howpublished institution eprint journal key month note number organization pages publisher school series title type volume year label extra.label sort.label short.list INTEGERS output.state before.all mid.sentence after.sentence after.block FUNCTION init.state.consts #0 'before.all := #1 ...

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write newline

" write newline "" before.all 'output.state := FUNCTION n.dashify 't := "" t empty not t #1 #1 substring "-" = t #1 #2 substring "--" = not "--" * t #2 global.max substring 't := t #1 #1 substring "-" = "-" * t #2 global.max substring 't := while if t #1 #1 substring * t #2 global.max substring 't := if while FUNCTION word.in bbl.in " " * FUNCTION format....

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