Burned to ashes: How the thermal decomposition of refractory organics in the inner protoplanetary disc impacts the gas-phase C/O ratio

Adrien Houge; Anders Johansen; Bertram Bitsch; Edwin Bergin; Fred J. Ciesla; Giulia Perotti; Michiel Lambrechts; Thomas Henning

REVIEW 2 major objections 6 minor 1 cited by

Burned to ashes: How the thermal decomposition of refractory organics in the inner protoplanetary disc impacts the gas-phase C/O ratio

T0 review · 2 major / 6 minor · reviewed 2026-08-07 · deepseek-v4-flash

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Pith's one-line read Irreversible thermal decomposition of refractory organics in the inner protoplanetary disc creates a long-lived, outward-diffusing reservoir of carbon-rich gas that raises the gas-phase C/O ratio to super-stellar and even super-unity…

desk verdict A clean numerical experiment showing irreversible decomposition of refractory organics can redistribute carbon outward, but the headline C/O>1 result hangs on Sc=1/3 and C2H2 as sole product. read the letter →

arxiv 2505.20427 v1 pith:6FGG7PQJ submitted 2025-05-26 astro-ph.EP

Adrien Houge , Anders Johansen , Edwin Bergin , Fred J. Ciesla , Bertram Bitsch , Michiel Lambrechts , Thomas Henning , Giulia Perotti This is my paper

classification astro-ph.EP

keywords protoplanetarydiscsC/OratiorefractoryorganicsthermaldecompositionC2H2dustevolutionicelinesSchmidtnumber

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

The paper argues that the irreversibility of thermal decomposition changes how the largest carbon reservoir in protoplanetary discs behaves. Refractory organics, which carry roughly 60% of the carbon, are usually destroyed so close to the star that the released gas is assumed to be quickly accreted and irrelevant. The authors show that if, as laboratory experiments indicate, these organics break apart into volatile molecules such as C2H2 rather than sublimating and recondensing, the organics line becomes permeable: carbon-rich gas can diffuse outward to the C2H2 iceline at about 7 au around a solar-mass star and survive for much longer. In their 1D evolution model this raises the gas-phase carbon reservoir by about an order of magnitude and markedly changes the C/O ratio, with values above unity outside the water iceline for most of the disc lifetime. If correct, this gives a new path for carbon enrichment of the inner disc that does not rely on large CH4 abundances, and a new way to read Spitzer and JWST observations of C2H2-rich discs.

What carries the argument

The mechanism is the permeable organics line, produced by irreversible thermal decomposition. In ordinary iceline chemistry, vapor that diffuses outward across its sublimation line recondenses onto grains (the cold-finger effect), trapping the volatile inside the iceline; for refractory organics, decomposition into simpler molecules such as C2H2 makes that return path impossible, so the line does not hold carbon back. The argument is carried quantitatively by the 1D evolution of gas and dust: a two-population grain-growth scheme sets pebble drift, and each gas species is advected and diffused according to a viscous disc model in which the Schmidt number (ratio of viscosity to gas diffusivity) is $Sc = 1/3$ in the standard setup, giving diffusion three times the reach of inward advection. With that transport, C2H2 released at roughly 0.3 au spreads to its own iceline at about 7 au, and the longer viscous timescale there keeps the carbon-rich gas in the disc for millions of years instead of accreting onto the star.

What would settle it

Run the paper's model with a Schmidt number of 1 instead of 1/3, or measure the turbulent Schmidt number in the inner disc with non-ideal MHD simulations; either would show whether the outward C2H2 flux survives. A direct observational test: in a solar-mass disc still delivering pebbles, spatially resolve C2H2 (or the gas-phase C/O ratio) between the water iceline and about 7 au; absence of the predicted order-of-magnitude carbon-rich reservoir there would falsify the central claim in its fiducial setup.

Watch

Extended reading notes

Core claim

The central claim is that thermally decomposing refractory organics release carbon into the gas phase in a form that cannot return to the solid phase, and that this one-way valve redistributes carbon through the inner disc. The paper's model takes refractory organics to decompose at 350 K into gaseous C2H2 (sublimation temperature 70 K). Because C2H2 does not recondense at the organics line, the usual cold-finger trapping that holds vapor just inside an iceline is absent; instead the organics line lets carbon-rich vapor diffuse outward against the accretion flow. The result is a reservoir of C2H2-rich gas extending out to the C2H2 iceline at roughly 7 au, where the viscous accretion timescale is about 1.5 Myr compared with 0.06 Myr at the organics line, and a total carbon-rich gas mass about an order of magnitude larger than in models without irreversible decomposition. The gas-phase C/O ratio consequently becomes super-stellar inside the water iceline and exceeds unity outside it in the fiducial model, with the detailed outcome depending on turbulence, pebble flux lifetime, and the partitioning of carbon.

Load-bearing premise

The model's outspread of carbon-rich gas assumes a Schmidt number of 1/3, meaning gas diffuses three times more efficiently than it is dragged inward; if the real value is 0.7 or higher, the paper itself finds the C2H2 reaching 7 au drops by about a factor of 5 and the C/O rise outside the water iceline disappears.

Editorial extensions

If this is right

The carbon-rich gas reservoir produced by refractory organics is roughly ten times more massive and survives far longer in the disc than in models where the released carbon is trapped inside the organics line.
Gas-phase C/O is significantly enhanced: super-stellar values appear just inside the water iceline, and values above unity appear outside it, with the pattern persisting through most of the disc lifetime for alpha >= 1e-3.
The usual anti-correlation between gas and solid composition breaks down: carbon-rich gas and carbon-rich solids can coexist at the same radius, changing how planetesimals and planets sample carbon relative to oxygen.
The model can produce hydrocarbon-rich inner discs and a colder, more extended C2H2 component without requiring a large volatile CH4 reservoir, offering an alternative explanation for Spitzer and JWST spectra.
Giant planets migrating in the inner few au have a wider window to accrete carbon-rich gas, which alters the heavy-element content they inherit.

Reading between the lines

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

Because the paper's own $Sc = 0.7$ run reduces C2H2 at 7 au by about a factor of 5 and drops gas-phase C/O below unity outside the water iceline, the headline result is conditional on turbulent diffusion being genuinely stronger than advection; pinning down the Schmidt number observationally or with non-ideal MHD simulations would decide how far the effect extends.
The same one-way-valve logic applies to any refractory carrier whose decomposition products are volatile: if organics decompose into CH4 (30 K) rather than C2H2, the carbon-rich gas would reach roughly 40 au, making the C/O footprint much more extended.
Coupling this mechanism with FUor-type outbursts, which push the organics line outward to several au, suggests that the gas-phase C/O enhancement could outlast the outburst by hundreds of kyr and serve as a chemical fossil of past accretion events.
A testable separation: in discs where pebble drift is still ongoing, spatially resolved C2H2 emission (or C/O mapping) beyond the water iceline would distinguish this decomposition-driven reservoir from the alternative late-stage CH4 inflow scenario, which operates only after the pebble flux has died.

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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

Quick take: this is a well-posed 1D disk evolution study with a genuinely new mechanism — irreversible thermal decomposition of refractory organics into C2H2 turns the soot line from a trap into a one-way valve for carbon. The modeling is transparent, the sensitivity runs are honest, and they modified chemcomp to free the Schmidt number and tested the new implementation against the standard one. Credit where due: the paper clearly shows that if decomposition is irreversible and the product is as volatile as C2H2, carbon-rich gas can diffuse outward and survive far longer than in models with reversible sublimation, with order-of-magnitude increases in the carbon-rich gas mass. That reframes how inner-disk C/O and C/H are set.

The soft spots are real and mostly internal. The headline claim that C/O exceeds unity outside the water iceline out to ~7 au depends on Sc=1/3. Their own Section 4.4 shows that at Sc=0.7 — within the published MHD range, including their cited Johansen & Klahr 0.85 — the C2H2 reaching 7 au drops by a factor ~5 and C/O outside the water iceline falls below unity. The abstract does not qualify this. To recover C/O>1 at Sc=0.7 they lower CO2 from 10% to 1% of carbon, which is a parameter adjustment, not an empirical constraint. So the single most load-bearing quantitative implication is hostage to a poorly constrained number. The alternative decomposition product CH4 pushes the effect further out, which helps, but the default assumption of pure C2H2 is itself a guess, acknowledged in the text.

It is also worth saying what is not broken: the qualitative behavior — irreversible decomposition plus outward diffusion redistributes carbon over several au — is not an artifact of one parameter choice, and the paper's own discussion is unusually candid about the sensitivities. They flag the Schmidt number issue in Section 4.4 and in the conclusions. But candor does not remove the uncertainty; the abstract as written overstates robustness.

Who is this for? Disk chemical evolution modelers, planet formation people interested in C/O ratios and giant planet enrichment, and anyone interpreting Spitzer or JWST C2H2 observations. It deserves a serious referee. I would send it out with a request to qualify the abstract and make the Sc dependence front-and-center, not buried in Section 4.4. If the authors reframe the claims as conditional on Sc<~0.5 and treat the beyond-water-iceline C/O>1 as illustrative rather than robust, this is a solid contribution.

Referee Report

2 major / 6 minor

Summary. The paper presents a 1D dust/gas evolution model (based on chemcomp) that treats the thermal decomposition of refractory organics as an irreversible process producing gaseous C2H2 at the organics line (~0.3 au for a solar-mass star). Unlike the standard treatment in which sublimated vapor recondenses at the iceline, the decomposition product C2H2 has a much lower sublimation temperature (70 K), so the carbon-rich gas diffuses outward to the C2H2 iceline at ~7 au, where it eventually freezes out. The authors find that this outward transport increases the gas-phase C/H by factors of 2–5 and can raise the gas-phase C/O above unity outside the water iceline, depending on turbulence, stellar mass, and the CO2 abundance. They argue this process could explain JWST/Spitzer observations of hydrocarbon-rich inner disks and affect the heavy-element budgets of giant planets.

Significance. The mechanism proposed is physically plausible and distinct from previous treatments: irreversible decomposition turns a large solid carbon reservoir into a mobile gas-phase reservoir that is not trapped at the organics line. The paper is transparent about its assumptions and provides a thorough parameter study (turbulence, stellar mass, fragmentation velocity, viscous heating, carbon partitioning, product species, and Schmidt number). The authors are also candid about the limitations of their fiducial choices, especially in §4.4. If the fiducial parameters hold, the work identifies a new route to sustain C/O > 1 in the outer inner disk (several au), with observable consequences for C2H2 emission. However, the headline quantitative result is conditional on Sc = 1/3 and on C2H2 being the sole decomposition product; both assumptions are acknowledged in the text but not fully reflected in the abstract and conclusions.

major comments (2)

[§4.4, Fig. 8] The quantitative headline claim in the Abstract and Conclusions — that carbon-rich gas survives out to 7 au with an order-of-magnitude abundance increase and that C/O exceeds unity outside the water iceline — is obtained with Sc = 1/3 as fixed in Eq. (3). Figure 8 shows that at Sc = 0.7, a value within the published MHD range (Johansen & Klahr 2005; Carballido et al. 2005), the C2H2 surface density at 7 au drops by a factor of ~5 and the gas-phase C/O outside the water iceline falls below unity. The abstract presents the 7 au/order-of-magnitude result without qualification, while the paper's own §4.4 shows this result is not robust to plausible Sc values. The suggested mitigation of lowering CO2 from 10% to 1% of carbon is a parameter adjustment, not an empirical constraint. This is load-bearing because the abstract and conclusion 3 explicitly claim C/O > 1 outside the water iceline for the fiducial model. I recommend revising the abstract and conclusions to state the Sc dependence, or providing a more empirically grounded argument for Sc = 1/3.
[§2.1 and §4.3] The choice that 100% of the decomposed refractory carbon is released as C2H2 (T_sub = 70 K) sets the extent of outward diffusion (to the 7 au C2H2 iceline) and therefore the entire radial scale of the claimed effect. The paper acknowledges this in §4.3 and shows the CH4 end-member case, but the fiducial result is not bracketed by a realistic product distribution: the decomposition of macromolecular organics likely yields a mixture of species, some of which (e.g., benzene, T_sub comparable to ammonia as noted in §4.3) have higher binding energies and would freeze out closer in. Such a mixture would reduce the effective outward transport distance. Because the 7 au distance is essentially set by the assumed product's sublimation temperature, I ask the authors to either treat the product speciation more explicitly, or explicitly reframe the result as an upper limit on the outward extent.

minor comments (6)

[Abstract] The phrase 'allowing gaseous carbon to diffuse outward without returning to the solid phase' is imprecise because C2H2 does recondense at its own iceline at ~7 au; suggest 'without returning to the solid phase at the organics line' or similar.
[§2.2] The sentence 'We set up chemcomp over a discretised grid of 500 radial cells log-spaced between either 0.01 au or 0.1 au to 1000 au' is ambiguous; please specify which inner boundary is used for which stellar mass (0.01 au for the 0.1 M_sun case, 0.1 au for the solar-mass case, as elsewhere in the text).
[Fig. 8 caption] The phrase 'to show that it allows to obtain C/O ratios greater than unity' is awkward; suggest 'to show that C/O ratios greater than unity can be obtained'.
[References] The chemcomp code is cited as Schneider & Bitsch (2023, arXiv:2401.15686); if the code has since been published or a DOI is available, please update the reference.
[§4.4] The text quantifies the drop at Sc = 0.7 but not at Sc = 1 or Sc = 3, although these cases are shown in Fig. 8; adding a sentence quantifying the reduction at Sc = 1 would help the reader.
[Throughout] The notation for sublimation temperature is inconsistent (Tsub vs. T_sub); please unify, and likewise use a consistent subscript style for the Schmidt number (Sc vs. Sc_g).

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the central C/O and carbon-reservoir results are integrated outputs of stated transport inputs, and the key Schmidt-number sensitivity is transparently reported in Section 4.4.

full rationale

The paper's derivation chain is self-contained: it inputs irreversible thermal decomposition of refractory organics into C2H2 (Tsub=70 K), a fixed organics-line temperature, solar abundances, a carbon partitioning, and the chemcomp advection-diffusion equations, and then integrates the coupled gas/solid transport to obtain the C2H2 surface density and gas-phase C/O profiles. The 'out to 7 au' extent is the C2H2 iceline implied by the assumed Tsub=70 K and the adopted temperature profile; this is a stated boundary of the model, not a fitted prediction, and the nontrivial outputs are the order-of-magnitude enhancement of the C2H2 reservoir and the radial C/O structure, which emerge from solving Eq. (3) rather than being imposed. The Schmidt number is fixed at Sc=1/3 by the standard chemcomp implementation, and the paper explicitly tests this assumption in Section 4.4, showing that at Sc=0.7 the C2H2 reaching 7 au drops by a factor of about 5 and gas-phase C/O outside the water iceline falls below unity. That is a transparent robustness limitation, not a circular reduction. Self-citations, including the chemcomp code (Schneider & Bitsch, with Bitsch as co-author) and comparison models such as Mah et al. (2023), are not load-bearing in a circular way: the code is public and re-validated in Appendix C against a new implementation, and the cited comparisons serve as external benchmarks rather than as justification of the central premise. No uniqueness theorem or fitted parameter is invoked to force the conclusion. Therefore no specific circular step can be exhibited, and the appropriate finding is no significant circularity.

Assumptions & free parameters 5 free parameters · 5 assumptions · 0 invented entities

The central model depends on several chosen parameters and domain assumptions. The most influential are the irreversible decomposition product (C2H2) and the Schmidt number, both acknowledged as uncertain by the authors. No new physical entities are introduced.

free parameters (5)

Refractory organic decomposition temperature T_sub = 350 K
Fixed at 350 K within the 300-500 K laboratory range (Nakano et al. 2003). Sets the organics line at about 0.3 au for a solar-mass star and therefore where carbon-rich gas is released.
Schmidt number Sc = 1/3
Standard chemcomp gas evolution fixes Sc=1/3 (Eq. 3), maximizing outward diffusion. Section 4.4 shows that for Sc=0.7 the C2H2 reaching 7 au drops by about a factor of 5 and C/O outside the water iceline drops below unity.
Initial carbon partitioning = 60% organics, 29% CO, 10% CO2, 1% CH4
Determines the size of the refractory carbon reservoir and the background oxygen budget; variations are explored in Appendix B.4.
Fragmentation velocity v_frag = 1 m/s fiducial
Sets pebble size and thus pebble flux and drift timescales; varied to 5 m/s in Appendix B.2.
Turbulence parameter alpha = 1e-3 fiducial (explored 1e-4 to 1e-2)
Sets viscosity, diffusion, and particle sizes; varied across the grid in Section 3.2.2. Not fitted, but strongly controls whether the pebble flux runs out.

assumptions (5)

domain assumption Thermal decomposition of refractory organics is irreversible and the products do not recondense into the solid phase at the organics line.
Laboratory experiments (Kouchi et al. 2002, Nakano et al. 2003) are cited as evidence; without irreversibility the organics line behaves like a normal iceline and the central mechanism disappears.
ad hoc to paper All decomposed refractory carbon is released as C2H2 with T_sub=70 K.
Acknowledged as unknown in Section 2.1; motivated by JWST observations and thermo-chemical models. The CH4 alternative is explored in Section 4.3.
domain assumption Gas-phase chemistry after decomposition is neglected; C2H2 does not convert to other carbon species.
The model evolves only transport and phase exchange and does not include a chemical network. The paper argues thermo-chemical models quickly store carbon in C2H2, but no network is solved.
domain assumption A 1D viscous alpha-disk with advection, diffusion, sublimation, condensation, dust coagulation, and drift describes the disk.
Standard chemcomp framework (Schneider and Bitsch 2023); ignores vertical structure and 2D flows, which could affect where outward diffusion deposits carbon.
domain assumption Refractory carbon is not destroyed by oxidation or photolysis.
Acknowledged in Section 4.6 as a simplification; alternative irreversible pathways would also release carbon gas and likely reinforce the mechanism.

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Cite this review

Pith. "Pith review of Burned to ashes: How the thermal decomposition of refractory organics in the inner protoplanetary disc impacts the gas-phase C/O ratio." pith.science (2026). https://pith.science/paper/6FGG7PQJ

@misc{pith2026250520427,
  author       = {Pith},
  title        = {Pith review of: Burned to ashes: How the thermal decomposition of refractory organics in the inner protoplanetary disc impacts the gas-phase C/O ratio},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/6FGG7PQJ}},
  note         = {Machine review of arXiv:2505.20427}
}

abstract

The largest reservoir of carbon in protoplanetary discs is stored in refractory organics, which thermally decompose into the gas-phase at the organics line, well interior to the water iceline. Because this region is so close to the host star, it is often assumed that the released gaseous material is rapidly accreted and plays little role in the evolution of the disc composition. However, laboratory experiments show that the thermal decomposition process is irreversible, breaking macromolecular refractory organics into simpler, volatile carbon-bearing compounds. As a result, unlike the iceline of other volatiles, which traps vapor inwards due to recondensation, the organics line remains permeable, allowing gaseous carbon to diffuse outward without returning to the solid phase. In this paper, we investigate how this process affects the disc composition, particularly the gas-phase C/H and C/O ratios, by incorporating it into a 1D evolution model for gas and solids, and assuming refractory organics dominantly decompose into C$_2$H$_2$. Our results show that this process allows this carbon-rich gas to survive well beyond the organics line (out to $7 \mathrm{~au}$ around a solar-mass star) and for much longer timescales, such that its abundance is increased by an order of magnitude. This has several implications in planet formation, notably by altering how the composition of solids and gas relate, and the fraction of heavy elements available to giant planets. In the framework of our model, refractory organics significantly influence the evolution of the gas-phase C/O ratio, which may help interpreting measurements made with Spitzer and JWST.

Figures

Figures reproduced from arXiv: 2505.20427 by the authors.

**Figure 1.** Gas surface density (top) and solid surface density (bottom) of the main chemical species that contribute to the C/O ratio at 0.1, 1, and 5 Myr. We ran this simulation with M∗ = 1 M⊙ and α = 10−3 . The total (dust or gas) surface density is represented as a dark solid line in each row. Vertical dashed lines indicate the sublimation lines of the displayed species in their respective color, using Tsub,CO = 20 K, Tsub,… view at source ↗

**Figure 2.** Evolution of the total mass of refractory organics and of the carbon-rich gas they release upon thermal processing at the organics line as a function of time in our fiducial disc setup (α = 10−3 , M∗ = 1 M⊙). The blue line represents a standard model that excludes the thermal decomposition of refractory organics (e.g., Mah et al. 2023), where the carbon-rich gas released by refractory organics remains inside the o… view at source ↗

**Figure 3.** Gas-phase (left panel) and solid-phase (right panel) C/O ratios as functions of distance from a solar-mass star for a disc characterised by α = 10−3 . Blue lines represent a standard model that excludes the thermal decomposition of refractory organics (e.g., Mah et al. 2023), while red lines show the results from our model, including that effect. The horizontal dashed grey line represents the initial C/O ratio. The … view at source ↗

Figures from the paper (5 more)

**Figure 4.** Figure 4: Gas-phase C/H ratio (normalised by the ratio at t0) as a function of distance from a solar-mass star for a disc characterised by α = 10−3 . Blue lines represent a standard model that excludes the thermal decomposition of refractory organics (e.g., Mah et al. 2023), wh…

**Figure 5.** Figure 5: Gas-phase C/O ratio as a function of distance to the star for the two different values of the stellar mass (M∗ = 1, 0.1 M⊙) and three values of the turbulent viscosity (α = 10−2 , 10−3 , 10−4 ). The horizontal dashed grey line represents the initial C/O ratio. The subl…

**Figure 6.** Figure 6: Gas-phase C/O ratio as a function of time and distance to the star for the two different values of the stellar mass (M∗ = 1, 0.1 M⊙) and three values of the turbulent viscosity (α = 10−2 , 10−3 , 10−4 ). The sublimation lines of the main species contributing to the C/O…

**Figure 7.** Figure 7: Gas-phase C/O ratio as a function of distance from a solar-mass star for a disc characterised by α = 10−3 . Red lines represent our fiducial model where refractory organics thermally decompose into C2H2 (Tsub = 70 K), while green lines show the results of a model wher…

**Figure 8.** Figure 8: Gas surface density of C2H2 (top) and gas-phase C/O ratio (bottom) at 1 Myr for various Schmidt numbers for a disc around a solarmass star with α = 10−3 . We ran an additional model with a lower initial abundance of CO2 and Sc = 0.7 to show that it allows to obtain C…

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