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High-temperature measurements of acetylene VUV absorption cross sections and application to warm exoplanet atmospheres

T0 review · 3 major / 4 minor · reviewed 2026-08-10 · deepseek-v4-flash

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Pith's one-line read Heated acetylene absorbs increasingly more vacuum-ultraviolet light across 115–230 nm, and applying 773 K data to a hot-Jupiter model lowers predicted C2H2 by up to 40%.

desk verdict New high-temperature C2H2 VUV cross sections are a real step forward, but the headline factor-of-20 rise at 773 K near 220 nm rests on data the authors themselves suspect of pyrolysis contamination. read the letter →

arxiv 2501.02864 v1 pith:W5CN2JM4 submitted 2025-01-06 astro-ph.EP

Benjamin Fleury , Mathilde Poveda , Yves Benilan , Roméo Veillet , Olivia Venot , Pascal Tremblin , Nicolas Fray , Marie-Claire Gazeau
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Martin Schwell Antoine Jolly Nelson de Oliveira Et-touhami Es-sebbar
This is my paper · ORCID
classification astro-ph.EP
keywords acetyleneC2H2VUVabsorptioncrosssectionstemperaturedependenceexoplanetatmospheresphotochemistryhotJupitersthermo-photochemicalmodeling
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 reports the first laboratory measurements of acetylene (C2H2) vacuum-ultraviolet (VUV) absorption cross sections at the high temperatures typical of warm exoplanet atmospheres, from 296 K to 773 K over 115–230 nm. The authors show that heating acetylene increases its absolute VUV absorption: the increase is roughly uniform from 115 to 185 nm, then climbs steeply from 185 to 230 nm, reaching about a factor of 20 near 220 nm at 773 K. Feeding these data into a one-dimensional thermo-photochemical model of a hot Jupiter raises the high-altitude photodissociation rate of C2H2 by about a factor of three and lowers the predicted C2H2 abundance by up to 40% near $5\times10^{-5}$ bar, with smaller changes to CH4 and C2H4. The work matters because photochemical models of exoplanets currently rely on room-temperature cross sections, and temperature-dependent data change both the chemistry and the depth at which starlight penetrates.

What carries the argument

The carrying mechanism is the temperature-dependent population of vibrationally excited ground-state levels, which produces hot bands in the $A{}^1A_u \leftarrow X{}^1\Sigma_g^+$ band system longward of 185 nm and a new band near 156.7 nm; these changes are quantified with the factor $F_T = (\sigma_T - \sigma_{296\,\mathrm{K}})/\sigma_{296\,\mathrm{K}}$. Experimentally, the cross sections are derived from the Beer–Lambert law using a 165 cm quartz cell heated up to 773 K with MgF$_2$ windows, a deuterium lamp plus VUV monochromator, and synchrotron spectra for wavelength calibration and cross-checks. The atmospheric application uses the paper's one-dimensional thermo-photochemical model, which computes photodissociation rates and steady-state abundances from the new cross sections.

What would settle it

Measure the composition of the gas inside the static cell as a function of time at 773 K (e.g., mass spectrometry or time-resolved spectroscopy), or repeat the 773 K long-wavelength measurement in a fast-flow or shock-tube cell with microsecond residence times. If the 222.5 nm bump and the steep rise above 210 nm disappear or shrink when pyrolysis products are absent, the reported factor-of-20 increase is inflated and the 40% modeled abundance decrease would be too large.

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Extended reading notes

Core claim

The central discovery, on the paper's own terms, is that acetylene's absolute VUV absorption cross section is strongly temperature dependent across the full photodissociation window. As temperature rises from 296 to 773 K, the continuum absorption increases while the discrete band intensities decrease, so the net cross section grows; from 115 to 185 nm the relative increase is nearly wavelength-independent (average $F_T$ of 0.5 at 773 K, with band-to-band excursions up to 3.5), and from 185 to 230 nm it rises sharply to a maximum $F_T$ of about 20 near 220 nm, attributed to hot bands of the A–X system. A new hot band appears near 156.7 nm at 473 K and above, assigned to the $\nu_2$ vibrational mode. In the model atmosphere, using the 773 K cross sections instead of the 296 K ones makes C2H2 photodissociate three times faster at pressures below $10^{-2}$ bar, pushes the photodissociation cutoff upward, reduces the C2H2 abundance by 40% near $5\times10^{-5}$ bar, and alters CH4 and C2H4 abundances down to $10^{-2}$ bar. The authors flag that the 222.5 nm feature at 773 K could partly reflect thermal decomposition products rather than C2H2 itself, and that additional time-resolved composition measurements are needed to confirm this.

Load-bearing premise

The load-bearing premise is that the strong absorption seen at 773 K above about 210 nm is truly acetylene, not absorption by molecules formed as acetylene thermally decomposes inside the static cell.

Editorial extensions

If this is right

  • Warm-exoplanet photochemical models should replace 296 K C2H2 cross sections with temperature-appropriate ones; in the paper's hot-Jupiter test, the 773 K data triple the high-altitude C2H2 photodissociation rate and reduce the predicted C2H2 abundance by 40% near $5\times10^{-5}$ bar.
  • Using hot cross sections shifts the 150–230 nm actinic-flux cutoff upward by roughly an order of magnitude in pressure, so photochemistry at deeper levels is suppressed and species that share that opacity window are shielded.
  • The new 156.7 nm hot band, growing with temperature, gives a spectral signature that can identify warm acetylene and test the assumed temperature in future laboratory or atmospheric spectra.
  • Because similar temperature sensitivity is already documented for CO2, the implication for modelers is that other major VUV absorbers (CH4, C2H4, NH3, H2S) need high-temperature measurements if photochemical predictions are to be trusted.

Reading between the lines

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

  • Editorial inference: the 40% abundance change is a single-model realization (C/O = 2× solar, F-star, $K_{zz}=10^8$ cm$^2$ s$^{-1}$); for planets with different C/O, eddy mixing, or cooler upper atmospheres, the effect could be larger or smaller, and the paper does not map that sensitivity.
  • Editorial inference: if the 222.5 nm bump is confirmed as pyrolysis-product absorption rather than C2H2 hot bands, the $F_T \approx 20$ near 220 nm and the 40% modeled decrease would need downward revision; a time-resolved measurement of the cell gas composition at 773 K, which the authors call for, would settle this.
  • Editorial inference: the steep rise longward of 185 nm arises from hot-band populations, so at even hotter temperatures (1000–1500 K) the simple scaled cross-section approach may break down; a vibrationally state-resolved treatment or measurements at those temperatures would extend the result.
  • Editorial inference: the atmospheric model assumes a single C2H2 photodissociation channel with unit quantum yield; if the quantum yield for C2H + H also varies with temperature, the abundance impact could differ from the 40% estimate.
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Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 4 minor

Summary. The paper reports new VUV absorption cross-section measurements of acetylene (C2H2) at seven temperatures between 296 and 773 K over 115-230 nm, made with a new LISA static-cell spectrometer and, at selected temperatures, with synchrotron radiation at SOLEIL. The data are reduced via the Beer-Lambert law and compared with existing literature. The authors define a factor of change FT relative to the 296 K spectrum, find that the cross section increases with temperature, report a particularly sharp increase beyond ~185 nm with FT reaching about 20 near 220 nm at 773 K, and identify a hot band near 156.7 nm. They then use the 296 K and 773 K cross sections in the FRECKLL 1D thermo-photochemical model of a hot-Jupiter-like atmosphere, finding that the modeled C2H2 abundance decreases by up to 40% near 5e-5 bar when the 773 K data replace the 296 K data, with smaller changes for CH4 and C2H4.

Significance. If the high-temperature long-wavelength cross sections are reliable, the paper fills a genuine gap: previously, C2H2 VUV data above ~400 K were essentially absent, even though C2H2 is a key hydrocarbon in warm-exoplanet photochemistry. The work combines two independent facilities, and the 573 K comparison between LISA and SOLEIL gives confidence in the qualitative picture below 205 nm. The data are publicly deposited, the model application uses a published chemical scheme, and the cross sections are obtained from direct transmission measurements rather than from any fit to the atmospheric result, so there is no circularity in the laboratory part. However, the headline quantitative claims—the FT factor of about 20 near 220 nm at 773 K and the 40% modeled abundance decrease—rest on spectral regions and assumptions that are called into question by the authors' own remarks about possible thermal decomposition and by the acknowledged temperature-gradient uncertainty. The manuscript therefore needs additional validation or a quantitative bounding of these effects before its central quantitative results can be accepted.

major comments (3)
  1. [3.2 (Figs. 4, 6, 8)] The factor-of-change FT reaching about 20 near 220 nm at 773 K is supported only by the LISA dataset in the 205-230 nm range; the SOLEIL measurements stop near 205 nm, so there is no independent validation of this critical spectral window. The authors themselves state that the bump at 222.5 nm 'could be attributed to the thermal degradation of C2H2' and that 'additional work will be needed to confirm this hypothesis,' and they cite Zabeti et al. (2017) showing that static-cell C2H2 measurements with long residence times were affected by pyrolysis. Because the same 150-230 nm opacity increase drives the modeled 40% abundance decrease (Sect. 3.3.5 and Figs. 9-10), both headline results are not fully supported unless the authors provide time-resolved evidence of gas stability in the cell or an upper-limit estimate of absorption by possible pyrolysis products.
  2. [3.1.1 and Eq. (2)] FT is normalized by the 296 K cross section, yet the LISA and SOLEIL ambient spectra differ by roughly 25% in the continuum level in the 195-230 nm region, and the text states that the origin of these differences is difficult to establish. Since the 773 K long-wavelength spectra come from the LISA setup with its own 296 K normalization, the reported factor of about 20 could be substantially biased by this baseline discrepancy. The paper should report FT with the ambient-continuum uncertainty propagated, or show explicitly how FT changes when the 296 K continuum is shifted by the observed LISA-SOLEIL scatter.
  3. [2.2.2 (last paragraph)] The uniform-temperature assumption is acknowledged to potentially bias high-temperature cross sections by 'several tens of percent' because the column density in the colder end sections may be about twice that in the hot central section. The modeled C2H2 abundance change is 40%, i.e., of the same order as this systematic uncertainty. The authors should propagate this systematic range through the model calculation, or at least state quantitatively how the 40% figure changes when the high-temperature cross sections are shifted within the plausible systematic range.
minor comments (4)
  1. [Abstract vs. Section 4] The Abstract states the temperature range as 296 to 773 K, while Section 4 states '296 to 793 K' and Section 2.1 says the maximum studied temperature was 773 K; 793 K appears to be a typo in the Conclusions.
  2. [Figure 3 caption] The caption reads 'absorption cross of C2H2 section' and should read 'absorption cross section of C2H2'.
  3. [3.3.5 and 3.3.4] The model sets the C2H2 photodissociation quantum yield to zero for wavelengths longer than 217 nm while the cross-section grid is used up to 228 nm; the text should clarify that the 217-228 nm opacity change does not directly photolyze C2H2 in the model and can affect modeled abundances only through shielding of other absorbers or through the general opacity calculation.
  4. [3.3.4] The model is run with cross sections and stellar fluxes binned to 1 nm, which strongly smooths the sharp long-wavelength rise reported near 220 nm; a sentence stating that the 40% abundance result is stable to the binning choice would help the reader judge the atmospheric conclusion.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the cross sections are direct Beer-Lambert measurements and the atmospheric application is a forward model calculation.

full rationale

The paper's central claims—temperature-dependent C2H2 VUV cross sections, an FT factor reaching about 20 near 220 nm at 773 K, and a 40% modeled abundance decrease—rest on direct experimental measurements, not on fitted parameters or self-derived predictions. The absorption cross sections are obtained from the Beer-Lambert law (Eq. 1) using independently measured pressure, temperature, and path length; no parameter is fitted to the target result. The factor FT is a definition (Eq. 2) applied after the fact, not a prediction. The atmospheric simulations feed the measured cross sections into the FRECKLL model with a published chemical scheme (Veillet et al. 2024) and a fixed stellar spectrum; the resulting abundance change is a forward calculation. Self-citations, such as adopting the temperature-profile assumption from Venot et al. (2018), are not circular: they import an independently characterized experimental condition, and the paper explicitly acknowledges that this assumption could bias high-temperature cross sections by several tens of percent. The flagged possibility of thermal decomposition of C2H2 at 773 K above 210 nm is a data-quality and contamination risk, not a circularity, because the measurements remain direct transmissions and any bias would be experimental error rather than a logical reduction of the result to its inputs. The paper is therefore self-contained against external benchmarks and shows no significant circularity.

Assumptions & free parameters 3 free parameters · 5 assumptions · 0 invented entities

The measured cross sections are derived from transmission data with no fitted parameters. The model application introduces hand-chosen scenario parameters (C/O, Kzz, irradiation) and relies on literature quantum yields and a published chemical scheme. The two experimentally fragile assumptions are uniform T_max and absence of pyrolysis contamination at 773 K.

free parameters (3)
  • C/O ratio = 2 (twice solar)
    Chosen to produce high C2H2 abundance so the effect of the new data is visible; affects the modeled abundance profiles.
  • Eddy diffusion coefficient Kzz = 1e8 cm2 s-1
    Constant with altitude, chosen as in previous studies; affects vertical mixing and abundance profiles.
  • Irradiation temperature = 2303 K (semi-major axis 0.05735 AU around an F2V star)
    Sets the thermal profile via Parmentier and Guillot 2014; chosen to maximize photolysis and C2H2 in the upper atmosphere.
assumptions (5)
  • standard math Beer-Lambert law with ideal-gas density n = P/(k_B T) converts measured transmission into absolute cross sections.
    Used in Eq. 1, Sect. 2.2.1. Standard and not in question.
  • domain assumption Gas temperature is uniform and equal to T_max along the entire 165 cm optical path.
    Sect. 2.2.2; authors follow Venot et al. 2018 but note cold ends could change column density and bias cross sections by tens of percent.
  • domain assumption Absorption measured at 773 K above about 210 nm is due to C2H2 and not to pyrolysis products formed in the static cell.
    Sect. 3.2; a bump at 222.5 nm is tentatively attributed to thermal degradation; no gas-composition time evolution was measured.
  • domain assumption C2H2 photodissociation quantum yield is 1 from 120 to 217 nm.
    Sect. 3.3.5; based on Läuter et al. 2002 and Huebner and Mukherjee 2015, used in the model application.
  • domain assumption The Veillet et al. 2024 chemical scheme is valid for the modeled hot Jupiter conditions.
    Sect. 3.3.2; scheme validated against combustion data, used without re-validation for this scenario.

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Cite this review

Pith. "Pith review of High-temperature measurements of acetylene VUV absorption cross sections and application to warm exoplanet atmospheres." pith.science (2026). https://pith.science/paper/W5CN2JM4

@misc{pith2026250102864,
  author       = {Pith},
  title        = {Pith review of: High-temperature measurements of acetylene VUV absorption cross sections and application to warm exoplanet atmospheres},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/W5CN2JM4}},
  note         = {Machine review of arXiv:2501.02864}
}
read the original abstract

Most observed exoplanets have high equilibrium temperatures. Understanding the chemistry of their atmospheres and interpreting their observations requires the use of chemical kinetic models including photochemistry. The thermal dependence of the vacuum ultraviolet (VUV) absorption cross sections of molecules used in these models is poorly known at high temperatures, leading to uncertainties in the resulting abundance profiles. The aim of our work is to study experimentally the thermal dependence of VUV absorption cross sections of molecules of interest for exoplanet atmospheres and provide accurate data for use in atmospheric models. This study focuses on acetylene (C2H2). We measured absorption cross sections of C2H2 at seven temperatures ranging from 296 to 773 K recorded in the 115-230 nm spectral domain using VUV spectroscopy and synchrotron radiation. These data were used in our 1D thermo-photochemical model, to assess their impact on the predicted composition of a generic hot Jupiter-like exoplanet atmosphere. The absolute absorption cross sections of C2H2 increase with temperature. This increase is relatively constant from 115 to 185 nm and rises sharply from 185 to 230 nm. The abundance profile of C2H2 calculated using the model shows a slight variation, with a maximum decrease of 40% near 5 x 10-5 bar, when using C2H2 absorption cross sections measured at 773 K compared to those at 296 K. This is explained by the absorption, higher in the atmosphere, of the actinic flux from 150 to 230 nm due to the increase in the C2H2 absorption in this spectral range. This change also impacts the abundance profiles of other by-products such as methane (CH4) and ethylene (C2H4). We present the first experimental measurements of the VUV absorption cross sections of C2H2 at high temperatures. Similar studies of other major species are needed to improve our understanding of exoplanet atmospheres.

Figures

Figures reproduced from arXiv: 2501.02864 by the authors.

Figure 1
Figure 1. Experimental setup used at LISA to measure the VUV spectra of acetylene. The VUV spectra of C2H2 were measured from 115 to 230 nm using a McPherson 225 ultrahigh vacuum (UHV) monochromator (1 m focal length) pumped down to 8 × 10−8 mbar using an ionic pump to prevent absorption by atmospheric molecules (nitrogen, N2, oxygen, O2, etc.). The limits of the wavelength range are due, respectively, to the MgF2 windows cut… view at source ↗
Figure 2
Figure 2. Absorption cross section of C2H2 determined from 115 to 230 nm at LISA (black) and from 160.8 to 230 nm at SOLEIL with a resolution of 0.1 nm (red). Electronic transitions associated with ob￾served absorption bands are indicated. noise level and uncertainty of the intensity of the continuum in this region [PITH_FULL_IMAGE:figures/full_fig_p006_2.png] view at source ↗
Figure 3
Figure 3. Comparison of absorption cross of C2H2 section measured at ambient temperature from 115 to 230 nm at LISA (black) with the ones measured by Cheng et al. (2011) (red), Smith et al. (1991) (purple), and Bénilan et al. (2000) (blue). From 185 to 195 nm, our data agree with Bénilan et al. (2000) but we observe important differences compared to the data from Smith et al. (1991), which exhibit two large absorption bands t… view at source ↗
Figures from the paper (6 more)
Figure 4
Figure 4. Figure 4: Absorption cross section of C2H2 determined at LISA at 296 K (black), 373 K (red), 473 K (blue), 573 K (green), 673 K (violet), and 773 K (yellow). Top: Spectra covering the whole studied spectral range from 115 to 230 nm. Bottom: Same spectra with a focus on the 155- …
Figure 6
Figure 6. Figure 6: Factor of changes, FT , in the absorption cross section of C2H2 between high temperatures, T (K), and the ambient temperature (296 K) for LISA measurements. Top: FT calculated for the whole studied spec￾tral range (116 to 229 nm) along with an inset of 155-159 nm regio…
Figure 7
Figure 7. Figure 7: Long wavelength region (λ > 215 nm) of the A-X band system of C2H2 measured at ambient temperature at SOLEIL (black) and LISA (blue) as well as measured at 773 K at LISA (red). Absorption bands in the ν3 and ν2 + ν3 vibrational modes are identified based on the studies…
Figure 8
Figure 8. Figure 8: Comparison of the factor of changes of the absorption cross sec￾tion of C2H2 for the measurements made at 573 and 773 K at LISA and at SOLEIL from 160 to 204 nm. ders 2010) and a C/O ratio twice the solar one. From a pure modeling point of view, such an assumption allo…
Figure 10
Figure 10. Figure 10: Penetration of the actinic flux in the atmosphere (level where the optical depth is equal to 1) when using σC2H2 (296 K) (dashed blue line) and σC2H2 (773 K) (full red line). This takes into account absorp￾tion and diffusion by the different chemical species presents …
Figure 11
Figure 11. Figure 11: Abundance profiles for the main hydrocarbons at steady state in the atmosphere of our hypothetical planet. Solid lines correspond to the abundances calculated using the absorption cross section of C2H2 measured at 773 K, and dotted lines correspond to 296 K. also that…

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