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Horizontal quenching, not extreme metallicity, explains why methane is missing from WASP-43 b’s night side.

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2026-07-10 06:40 UTC pith:FADWY5Q2

load-bearing objection Solid multi-model case that moderate horizontal quenching (plus sulfur) explains the MIRI CH4 non-detection; cloud-free T(p) is the main caveat but does not break the jet-speed argument. the 2 major comments →

arxiv 2607.08486 v1 pith:FADWY5Q2 submitted 2026-07-09 astro-ph.EP astro-ph.IM

Phase-dependent chemistry of WASP-43 b revealed with a suite of one-, two-, and three-dimensional models

Robin Baeyens , Julianne I. Moses , Jasmina Blecic , Elspeth K. H. Lee , Lucas Teinturier , Shang-Min Tsai , Jeehyun Yang , Jingxuan Yang
show 12 more authors
Ludmila Carone Renyu Hu Sven Kiefer Anjali A. A. Piette Taylor J. Bell Nicolas Crouzet Ian Dobbs-Dixon Christiane Helling Nicolas Iro Dominic Samra Olivia Venot Jean-Michel D\'esert
This is my paper
classification astro-ph.EP astro-ph.IM
keywords WASP-43 bhot Jupiterdisequilibrium chemistryhorizontal quenchingmethane depletionsulfur photochemistryphase curveJWST MIRI
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

This paper asks why JWST/MIRI phase-curve spectra of the hot Jupiter WASP-43 b show no night-side methane even though night-side temperatures should favor it. Using a suite of one-, two-, and three-dimensional photochemical models that include day-to-night transport, the authors show that horizontal quenching by the equatorial jet is enough to keep methane depleted once wind speeds exceed roughly 500 m/s. The same models demonstrate that coupled carbon-sulfur chemistry further suppresses methane relative to earlier sulfur-free calculations, while high metallicity would produce SO2 absorption that is not seen. H2O, CO, and CO2 are robust across models; photochemically sensitive species are not. The result matters because it turns a non-detection into a dynamical constraint and shows that phase-resolved chemistry is required to interpret hot-Jupiter phase curves.

Core claim

Horizontal quenching is the prime mechanism that explains the non-detection of methane in the MIRI phase curve of WASP-43 b. The mechanism requires only moderate wind speeds greater than or equal to 500 m/s and operates across the thermal structures and metallicities tested; coupled carbon-sulfur chemistry supplies an additional methane decrease relative to previous sulfur-free models. High metallicity is disfavored because it would have produced observable SO2 features that are absent from the spectra.

What carries the argument

Pseudo-2D photochemical kinetics (ACE-PAC and KINETICS) with longitude-dependent temperature and stellar incidence that rotate at a prescribed equatorial jet speed, plus a self-consistent 3D climate-chemistry run (Exo-FMS + mini-chem). The machinery converts the competition between chemical interconversion timescales and zonal advection into longitude-dependent abundances that can be compared directly to phase-resolved retrieval upper limits.

Load-bearing premise

Cloud-free thermal structures and gas-phase chemistry are treated as adequate for interpreting the MIRI spectra even though the same data require night-side clouds near 100 mbar to mute the night-side flux.

What would settle it

A NIRSpec/G395H phase-curve detection of night-side SO2 absorption at the level predicted by the 10 imes-solar models, or a clear night-side CH4 feature once the same models are recomputed with the cloud deck required by the MIRI continuum, would overturn the horizontal-quenching-plus-moderate-metallicity conclusion.

Watch this falsifier — get emailed when new claim-graph text bears on it.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

2 major / 5 minor

Summary. The paper investigates the phase-dependent gas-phase chemistry of the hot Jupiter WASP-43 b with a suite of pseudo-2D photochemical models (ACE-PAC, KINETICS) and a 3D climate-chemistry model (Exo-FMS + mini-chem), comparing results to JWST/MIRI phase-curve retrievals (Bell et al. 2024; Yang et al. 2024). The central claim is that horizontal quenching by the equatorial jet at speeds ≳500 m s⁻¹ is the primary mechanism for the non-detection of night-side methane, operating across the tested thermal structures and metallicities, with coupled carbon-sulfur chemistry providing an additional CH₄ reduction relative to sulfur-free models (Venot et al. 2020). Metallicity scans show CO₂ and SO₂ as the strongest metallicity tracers, and the absence of mid-IR SO₂ features is used to disfavor ≳10 imes solar metallicity. A four-code 1D intercomparison (ACE-PAC, KINETICS, EPACRIS, VULCAN) demonstrates that H₂O, CO, and CO₂ are robust while photochemically active species (CH₄, NH₃, SO₂, HCN) vary by orders of magnitude depending on network and stellar UV assumptions.

Significance. If the horizontal-quenching interpretation holds, the work provides a clear, observationally testable explanation for the MIRI night-side CH₄ non-detection that is largely independent of metallicity and requires only moderate jet speeds well below both GCM predictions and the measured Doppler jet. The multi-model suite (pseudo-2D with and without sulfur, self-consistent 3D, and a four-code 1D intercomparison) is a genuine strength: it quantifies model-to-model scatter for photochemically active species and supplies falsifiable predictions for NIRSpec/G395H (CO₂, SO₂, continued CH₄ non-detection). The explicit jet-speed scan (Fig. 8) and equilibrium-versus-disequilibrium spectral contrast (Fig. 13) are particularly useful for the community. The paper also usefully revisits Venot et al. (2020) with sulfur chemistry included.

major comments (2)
  1. Secs. 4 and 6.2, Figs. 4, 7, 12: The load-bearing comparisons of model CH₄ upper limits and SO₂ spectral features to MIRI retrievals and data rest on cloud-free Generic PCM / 2D-ATMO thermal structures, even though Bell et al. (2024) require night-side clouds near 100 mbar to mute the continuum flux. The paper argues that cloud-chemistry feedback is minor and that even a cloud-suppressed jet (~2–2.5 km s⁻¹) remains above the ~500 m s⁻¹ quench threshold (Sec. 6.2, Fig. 8). That argument is plausible but incomplete: cloud-induced changes to the vertical T(p) near the quench level (~500 mbar in Fig. 8) or to the contribution-function envelope could still raise night-side CH₄ enough to tension with the retrieval upper limits used in Fig. 4, or mute the SO₂ features that disfavor 10 imes solar metallicity (Fig. 12). A short sensitivity test with a cloudy T(p) (or an explicit statement of how
  2. Sec. 3.4 and Fig. 7 versus Sec. 4.2 and Fig. 12: The metallicity conclusion (“we do not favor a high metallicity as it would have led to observable SO₂ features”) is drawn from cloud-free synthetic spectra in which SO₂ absorption appears only at 10 imes solar on the night side and morning terminator. Because SO₂ peaks at p ≲ 1 mbar while MIRI contribution functions extend deeper, and because night-side clouds are required by the continuum, the non-detection of SO₂ is a weaker metallicity upper limit than stated. The text should either (i) quantify how much cloud opacity would be needed to hide a 1–10 ppm SO₂ feature or (ii) soften the claim to a clear-atmosphere upper limit pending NIRSpec/G395H.
minor comments (5)
  1. Table 1: The listed molar fractions for CH₄ and HCN at 1 mbar differ by several orders of magnitude between ACE-PAC and KINETICS; a short note in the table caption or Sec. 3.1–3.2 pointing the reader to the later discussion of those differences would help.
  2. Fig. 8 caption and Sec. 3.5: Clarify that the underlying thermal structure is held fixed while only the jet speed is varied; a reader could otherwise infer that each wind speed comes from a self-consistent GCM.
  3. Sec. 5.2 / Fig. 15: The intercomparison is valuable; stating explicitly whether the same photodissociation cross-section database was used (or not) would make the residual scatter easier to interpret.
  4. Appendix A / Table A.1: Confidence levels (1σ vs 95% vs 99%) and the presence/absence of dilution and error-inflation parameters differ across retrievals; a single sentence in the main text reminding the reader of this heterogeneity would reduce the risk of over-interpreting the red/black/blue bars in Figs. 4–7.
  5. Minor typos and notation: “W ASP-43 b” spacing is inconsistent in places; “Kzz” vs “K_zz”; and the abstract uses “> 500 m/s” while the body uses “≳500 m s⁻¹”—standardize units and spacing.

Circularity Check

0 steps flagged

No load-bearing circularity: forward photochemical models with independent GCM thermal/jet inputs are compared to external JWST retrieval upper limits; self-citations are comparative only.

full rationale

The central claim (horizontal quenching at jet speeds ≳500 m s⁻¹ explains the MIRI night-side CH₄ non-detection, with sulfur chemistry providing an extra decrease) is obtained by solving the kinetics equation on fixed thermal structures and Kzz profiles taken from Generic PCM / 2D-ATMO / Exo-FMS (Secs. 2.1–2.3, B), then scanning jet speed (Sec. 3.5, Fig. 8) and metallicity (Secs. 3.4, 4). The resulting CH₄, SO₂ and CO₂ abundances are compared to independent multi-framework retrieval upper limits and non-detections (Bell et al. 2024; Yang et al. 2024; Appendix A). No free parameter is fitted to the CH₄ non-detection and then re-used as a “prediction”; the 500 m s⁻¹ threshold is an output of the kinetics, and both GCM jets (~3.3–3.4 km s⁻¹) and the Doppler measurement (5.4 km s⁻¹) lie well above it. The Venot et al. (2020) comparison (same ATMO T(p) and Kzz, sulfur network added) is a controlled difference test, not a uniqueness theorem or self-definitional step. Cloud omission is an acknowledged modelling choice (Secs. 4, 6.2), not a circular reduction. Model intercomparison (Sec. 5) quantifies pathway scatter rather than closing a definitional loop. Hence the derivation chain is self-contained against external data; residual self-citation is minor and non-load-bearing.

Axiom & Free-Parameter Ledger

5 free parameters · 5 axioms · 0 invented entities

The central claim rests on standard chemical kinetics and GCM-derived thermal/dynamical inputs, plus several free numerical choices (jet speed, Kzz, metallicity grid, stellar UV) that are varied or taken from prior literature rather than fitted to force the MIRI CH4 non-detection. No new physical entities are invented. The largest modeling axiom is that cloud-free equatorial pseudo-2D/3D chemistry is sufficient to interpret a phase curve known to require night-side clouds for the continuum flux.

free parameters (5)
  • Equatorial jet speed in pseudo-2D models
    Nominal 3.4 km/s (ACE-PAC from Generic PCM) or 4.6 km/s (KINETICS following Venot et al. 2020); scanned from ~10 m/s to multi-km/s in Fig. 8. Not fitted to MIRI CH4, but the ≳500 m/s threshold is a free dynamical input that controls the claim.
  • Vertical eddy diffusion Kzz profile
    Parametrized forms (Moses et al. 2022 for ACE-PAC; Venot et al. 2020 power law for KINETICS) and a high-Kzz experiment at 10^11 cm^2 s^-1. Controls quench levels of CH4/NH3/HCN and night-side SO2 build-up.
  • Atmospheric metallicity scale factor
    Grid 1–10× solar (Lodders 2019) with corresponding GCM thermal structures and jet speeds. Used to map CO2/SO2 and to argue against high Z from SO2 non-detection.
  • Stellar high-energy spectrum choice
    MUSCLES WASP-43 spectrum vs proxy reconstructions (Venot composite, HD 85512, Rugheimer K7V). Intercomparison shows this choice drives large scatter in CH4/NH3/HCN photochemistry.
  • 2D-ATMO deep heat advection parameter α
    Cold (α=10^4) vs hot (α=10) interior cases for KINETICS thermal structure; paper finds little effect above 1 bar but it remains a free structural choice inherited from Venot et al. 2020.
axioms (5)
  • domain assumption Chemical kinetics PDE (Eq. 1) with reversible networks and photodissociation adequately describe gas-phase composition of a hot H2 atmosphere.
    Sec. 2; standard exoplanet photochemistry premise shared by ACE-PAC, KINETICS, VULCAN, EPACRIS.
  • domain assumption A pseudo-2D rotating equatorial column with prescribed jet speed approximates zonal mixing for the spectroscopically dominant equatorial region.
    Secs. 2.1–2.2; justified by comparison to 3D Exo-FMS in Sec. 3.7 but remains an approximation of full 3D transport.
  • ad hoc to paper Cloud-free GCM/ATMO thermal structures are usable boundary conditions for chemistry even when night-side clouds are required by the continuum phase curve.
    Secs. 4 and 6.2 explicitly omit clouds for chemistry/spectra while citing Bell et al. night-side clouds at ~100 mbar.
  • domain assumption Elemental abundances scale with solar ratios (Lodders 2019) except for bulk metallicity multiplier; C/O and N/H are not free beyond that.
    Sec. 3.4 metallicity grid; used when comparing to Yang et al. NH3 tension and SO2 predictions.
  • standard math Thermodynamic reverse rates from equilibrium constants close the networks and recover deep-atmosphere equilibrium.
    Sec. 2.1 and intercomparison Sec. 5; small deep-atmosphere differences attributed to thermodynamic data.

pith-pipeline@v1.1.0-grok45 · 50128 in / 4103 out tokens · 51025 ms · 2026-07-10T06:40:43.536364+00:00 · methodology

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Our goal is to investigate the chemistry of the hot Jupiter WASP-43 b in detail using theoretical models, considering the constraints of the James Webb Space Telescope MIRI phase curve. With a suite of pseudo-two-dimensional and three-dimensional photochemical models, we simulate the composition of WASP-43 b in various configurations, and compare them with atmospheric retrieval models. We confirm that disequilibrium chemistry in our theoretical models reduces the methane concentration on the planet night side for wind jet speeds > 500 m/s. Varying the metallicity in the models induces large changes in the CO$_2$ and SO$_2$ concentrations, with SO$_2$ producing mid-infrared absorption features in synthetic emission spectra of the night side at atmospheric metallicities > 10x solar. Our models provide evidence for pole-to-equator circulation enhancing the CH$_4$, NH$_3$, and HCN abundances, which is nonetheless insufficient for detectable spectral features. Finally, we show that H$_2$O, CO, and CO$_2$ are robustly modeled, but species affected by photochemistry are more sensitive to model-specific assumptions and pathways. We conclude that horizontal quenching is the prime mechanism that explains the non-detection of methane in the MIRI phase-curve of WASP-43 b. This mechanism requires only moderate wind speeds and is operative at various thermal structures and atmospheric metallicities. Furthermore, coupled carbon-sulfur chemistry leads to an additional decrease in methane compared to previous models in the literature that did not contain sulfur chemistry. We do not favor a high metallicity as it would have led to observable SO$_2$ features in the MIRI spectra. Our study shows that phase-dependent photochemistry models are essential tools in the interpretation of hot-Jupiter phase curves, but benchmarking is needed to improve the accuracy of photochemical models in the future.

Figures

Figures reproduced from arXiv: 2607.08486 by Anjali A. A. Piette, Christiane Helling, Dominic Samra, Elspeth K. H. Lee, Ian Dobbs-Dixon, Jasmina Blecic, Jean-Michel D\'esert, Jeehyun Yang, Jingxuan Yang, Julianne I. Moses, Lucas Teinturier, Ludmila Carone, Nicolas Crouzet, Nicolas Iro, Olivia Venot, Renyu Hu, Robin Baeyens, Shang-Min Tsai, Sven Kiefer, Taylor J. Bell.

Figure 2
Figure 2. Figure 2: The chemical abundances of major species in WASP-43 b, com￾puted using the KINETICS pseudo-2D photochemical model, assuming solar metallicity. The adopted temperature profiles were computed with the radiative transfer code 2D-ATMO (as in Venot et al. 2020). Two as￾sumptions for interior heat transport are used, resulting in compositional differences for a cold (solid) and hot interior (dotted) [PITH_FULL_… view at source ↗
Figure 3
Figure 3. Figure 3: Stellar radiative flux and the abundances of H and H2 as a func￾tion of atmospheric pressure for the ACE-PAC solar metallicity model. Displayed are the wavelength-integrated XUV (10 nm - 121 nm) and FUV (121 nm - 200 nm) fluxes, showing different penetration depth in the atmosphere. Three zenith angles are shown: 0◦ (substellar point), 60◦ , and 90◦ (limb). The different abundance profiles correspond to di… view at source ↗
Figure 4
Figure 4. Figure 4: The methane abundance calculated using the ACE-PAC pseudo￾2D kinetics model (solid) deviates strongly from chemical equilibrium (dashed) on the planet’s night side and cold morning terminator. The results agree with upper limits from atmospheric retrievals, in contrast to the chemical equilibrium predictions. Metallicities between 1 × solar to 10 × solar are shown, with darker colors corresponding to a hig… view at source ↗
Figure 6
Figure 6. Figure 6: Analogous to [PITH_FULL_IMAGE:figures/full_fig_p008_6.png] view at source ↗
Figure 8
Figure 8. Figure 8: Map of the methane abundance at 1 mbar as a function of longi￾tude and wind jet speed, computed from a suite of pseudo-2D models. The nominal wind speed predicted by the GCM is 3400 m s−1 . The plot on the top shows the temperature deeper in the atmosphere, near the vertical quench level (∼500 mbar), which ultimately determines the dis￾equilibrium CH4 abundance if horizontal advection would be neglected. D… view at source ↗
Figure 9
Figure 9. Figure 9: The chemical abundances of major species in WASP-43 b modelled using ACE-PAC for strong vertical mixing (Kzz = 1011 cm2 s −1 ), assuming solar (left) and 10× solar (right) metallicity. Different lines represent different equatorial longitudes, with lighter shades being located closer to the substellar longitude. 90°W 0° 90°E 30°S 0° 30°N -8.0 -7.5 -7.0 -6.5 -6.0 -5.6 -5.1 log10 (CH4 molar fraction) 90°W 0°… view at source ↗
Figure 10
Figure 10. Figure 10: Longitude-latitude maps of the CH4 (top left), NH3 (top right), CO2 (bottom left) and HCN (bottom right) concentrations at 0.1 bar from the 3D Exo-FMS GCM + mini-chem simulation. The sub-stellar point is at the coordinates (0◦ ,0◦ ). Please note the differently scaled color bars. fect can be attributed to meridional transport of gas from the cold night-side gyres to the equator, enriching the low-latitude… view at source ↗
Figure 11
Figure 11. Figure 11: Equatorial abundances as a function of pressure of several species, computed using the 3D Exo-FMS + mini-chem simulation. The abundances are cos(latitude)-weighted and averaged between ±20◦ lat￾itude. As a comparison, the pseudo-2D ACE-PAC results are shown in muted colors. 4. Model emission spectra 4.1. Spectral code setup To quantify the potential effects of (disequilibrium) chemistry on the observed pl… view at source ↗
Figure 12
Figure 12. Figure 12: Synthetic cloud-free emission spectra of WASP-43 b at phases 0.00 (night), 0.25 (evening), 0.50 (day), and 0.75 (morning), generated using the 3D radiative transfer code gCMCRT (Lee et al. 2022). Observational data by Bell et al. (2024) (gray markers) are shown as reference, but since the photochemical models do not include clouds, no accurate match to the observational data is pursued. Data points in the… view at source ↗
Figure 13
Figure 13. Figure 13: Comparison between the morning terminator emission spec￾trum of a model with horizontal transport (orange) and a model with equilibrium chemistry (black dotted). The MIRI/LRS observations (Bell et al. 2024) are shown as reference. The main difference between the models is due to methane absorption, highlighted in black. solar metallicity model exhibits SO2 absorption near 4 µm. This is again most notable … view at source ↗
Figure 14
Figure 14. Figure 14: The four different stellar fluxes that are used by each photo￾chemical model in the intercomparison. For details regarding each spec￾tral energy distribution, see Sec. 5.1. input spectra are uniformized, and when each of their stellar fluxes is differently sourced. 5.2. Photochemical model intercomparison The solution space of several chemical species, consisting of the maximal and minimal values among al… view at source ↗
Figure 15
Figure 15. Figure 15: Illustration of the chemical species variation between four different but equivalent photochemical models: ACE-PAC, KINETICS, EPACRIS, and VULCAN. Left: All models use the same stellar spectrum as input. Right: All models use different stellar fluxes (see text for details). The composition is solar elemental composition. Colored areas indicate the maximum and minimum values resulting from all models. Inde… view at source ↗

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