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Horizontal transport as a source of disequilibrium chemistry on the nightside of a hot exoplanet

Nature Astronomy (2026)Cite this article

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Abstract

Hot Jupiters have temperature gradients of several hundreds of degrees between their permanent daysides and nightsides. Such a strong gradient creates winds with speeds of the order of kilometres per second, which advect chemical species over the whole planet. When this transport is faster than the time needed for chemical species to react, it holds back the chemical equilibration of the atmospheric carbon reservoir, which would otherwise transition from CO on the dayside to CH4 on the nightside. Direct evidence of this process has remained elusive so far, as it is often degenerate with other atmospheric processes, such as vertical mixing or non-stellar elemental abundances. Here we present observational evidence for such a fast day-to-night horizontal transport of chemical species by observing the full 18-h orbit of the exoplanet NGTS-10A b with the JWST/NIRSpec instrument. We show that the carbon chemistry is dominated by CO in both the dayside and the nightside of the planet, with a strong depletion of CH4 on the nightside compared with expectations from chemical equilibrium. By measuring the atmospheric abundances of all the main carbon and oxygen molecules, we further demonstrate that the lack of CH4 on the planetary nightside cannot be attributed to non-solar elemental abundances or to vertical mixing mechanisms and must, therefore, be due to fast horizontal transport. Our study shows the fundamental role that atmospheric transport plays in shaping the distribution of chemical species on exoplanet atmospheres.

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Fig. 1: JWST/NIRSPEC/PRISM orbital phase curve observation of NGTS-10A b.
The alternative text for this image may have been generated using AI.
Fig. 2: NGTS-10A b spectra.
The alternative text for this image may have been generated using AI.
Fig. 3: Chemical composition of NGTS-10A b.
The alternative text for this image may have been generated using AI.
Fig. 4: Thermochemical structure of NGTS-10A b.
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Data availability

The data used in this paper are associated with JWST guaranteed time observation programme 1185 (PI Parmentier) and are publicly available via MAST60. The reduced data used to produce Fig. 2 are available via Zenodo at https://doi.org/10.5281/zenodo.18861579 (ref. 61).

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Acknowledgements

This work was partially funded by the French National Research Agency (Project EXOWINDS with Grant No. ANR-23-CE31-0001-01). This work is based on observations made with the NASA/ESA/CSA JWST. The data were obtained from MAST at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations are associated with programme ID 2158. J.T. was supported by the Glasstone Benefaction, University of Oxford (Violette and Samuel Glasstone Research Fellowships in Science 2024). J.-M.D. acknowledges the research programme VIDI New Frontiers in Exoplanetary Climatology (Project No. 614.001.601), which is partly financed by the Dutch Research Council (NWO).

Author information

Authors and Affiliations

  1. Laboratoire Lagrange, Observatoire de la Côte d’Azur, Université de la Côte d’Azur, CNRS, Nice, France

    Vivien Parmentier

  2. Johns Hopkins Applied Physics Laboratory, Laurel, MD, USA

    Kevin B. Stevenson

  3. School of Earth and Space Exploration, Arizona State University, Tempe, AZ, USA

    Luis Welbanks & Mike Line

  4. Astrophysics, Department of Physics, University of Oxford, Oxford, UK

    Jake Taylor

  5. Steward Observatory, Department of Astronomy, University of Arizona, Tucson, AZ, USA

    Everett Schlawin

  6. Institut Trottier de Recherche sur les Exoplanètes et Département de Physique, Université de Montréal, Montréal, Quebec, Canada

    Louis-Philippe Coulombe

  7. Department of Astronomy & Astrophysics, University of California, Santa Cruz, CA, USA

    Yao Tang & Jonathan J. Fortney

  8. Anton Pannekoek Institute for Astronomy, University of Amsterdam, Amsterdam, the Netherlands

    Hinna Shivkumar & Jean-Michel Désert

  9. Tsung-Dao Lee Institute & School of Physics and Astronomy, Shanghai Jiao Tong University, Shanghai, People’s Republic of China

    Xianyu Tan

  10. Department of Astronomy & Astrophysics, University of Chicago, Chicago, IL, USA

    Jacob L. Bean & Eliza M.-R. Kempton

  11. Leibniz Institute for Astrophysics Potsdam, Potsdam, Germany

    Jean-Michel Désert

  12. Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC, USA

    Peter Gao

  13. Atmospheric, Oceanic, and Planetary Physics, Department of Physics, University of Oxford, Oxford, UK

    Mark Hammond & Thaddeus D. Komacek

  14. Department of Astronomy, University of Maryland, College Park, MD, USA

    Eliza M.-R. Kempton & Megan Weiner Mansfield

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  1. Vivien Parmentier
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Contributions

V.P. led the original proposal, performed the one-dimensional radiative and convective modelling, and wrote the article. K.B.S. reduced the observations and contributed to writing the paper. L.W. performed the free atmospheric retrievals used in the article. J.T. performed the initial atmospheric retrieval explorations. E.S. contributed to the proposal and performed the initial data reduction. L.-P.C. contributed to the proposal text and the effective temperature calculations. Y.T. performed the internal modelling of NGTS-10A b. M.L. performed the grid retrievals. H.S. performed a preliminary fit of the stellar spectra. X.T. provided insights on the transport properties of NGTS-10A b through global circulation models. M.H. performed an initial fit of the light curves. V.P., J.L.B., J.-M.D., J.J.F., P.G., T.D.K., M.L., E.S., K.B.S., J.T., E.M.-R.K. and M.W.M. were all members of the original JWST proposal team. All authors commented on the draft paper.

Corresponding author

Correspondence to Vivien Parmentier.

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Nature Astronomy thanks Thomas Evans-Soma and the other, anonymous, reviewer(s) for their contribution to the peer review of this work. Peer reviewer reports are available.

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Extended data

Extended Data Fig. 1 Observed lightcurve.

Spectroscopic phase curve of NGTS-10A b at 4.45 μm showing mean and standard deviation of the flux. The breaks between exposures at 14.4235 and 14.7140 days are made evident by the flux offsets. The magnitude and direction of the flux offset varies between spectroscopic channels (see Extended Data Fig. 2).

Extended Data Fig. 2 Flux offsets.

Measured flux offsets between our three exposures. The green and orange points depict the measured flux offsets at MJD = 14.4235 and 14.7140, respectively with the 1-σ standard deviation as errorbars.

Extended Data Fig. 3 White lightcurve.

Binned white light curve (blue points with 1 − σ errors) with best fit model (grey line). The red binned points represent the 1,000 masked integrations at the start of each exposure that exhibit a decaying ramp systematic.

Extended Data Fig. 4 NGTS-10 system.

Target acquisition image using NIRSpec. The brighter source near the center of the image is NGTS-10A; the fainter source up and to the right is NGTS-10B. The two stars are separated by ∼ 0.33”.

Extended Data Fig. 5 Imaged spectra.

Dispersed image (left) and vertical cut (right) of NGTS-10A and B. The dashed green lines bound the 3-pixel aperture size and the solid orange lines indicate the inner edges of the background region (used in Stage 1). In order to minimize the contribution from NGTS-10B, we chose not to center the aperture on the peak contribution from NGTS-10A. As seen in the right panel, a small amount of light from the binary star overlaps with the primary.

Extended Data Fig. 6 Stellar spectrum.

Stellar spectrum from the Schlawin reduction (first panel) and the Stevenson reduction (second panel) together with the best fit Phoenix models described in Table 1. We assume errorbars on the absolute flux of 10% The corresponding residuals are shown in the bottom two panels.

Extended Data Fig. 7 Uncertainty enhancement relative to the computed noise.

As part of the spectroscopic light curve fitting step, we adopt the scatter multiplier as a free parameter. The errobars represent the bin width.

Extended Data Fig. 8 Observed correlated noise.

Correlated noise versus bin size from the spectroscopic light curve fits. The blue curves depict the level of time-dependent correlated noise in the residuals from all 47 spectroscopic channels. The median RMS (solid green curve) closely follows the standard error expectation (dashed orange line), thus indicating no important red noise contribution for many of the channels. There is, however, evidence for red noise in the 11 spectroscopic channels < 1.7 μm.

Extended Data Fig. 9 NGTS-10A b interior modeling.

NGTS-10A b radius as a function of it’s internal entropy, parameterized as the internal temperature, calculated for different core mass. The gray line and gray zone represents the mean and the 1σ confidence interval on the measured planetary radius. Internal temperatures higher than ≈ 500K would need a much larger core than predicted by theory to fit the planet radius and are thus unlikely.

Extended Data Table 1 NGTS-10A system parameters
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Parmentier, V., Stevenson, K.B., Welbanks, L. et al. Horizontal transport as a source of disequilibrium chemistry on the nightside of a hot exoplanet. Nat Astron (2026). https://doi.org/10.1038/s41550-026-02845-2

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