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REVIEW 3 major objections 5 minor 167 references

Cloud and Haze Parameterization in Atmospheric Retrievals: Insights from Titan's Cassini Data and JWST Observations of Hot Jupiters

T0 review · 3 major / 5 minor · reviewed 2026-08-07 · deepseek-v4-flash

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Pith's one-line read This paper contends that cloud and haze properties in exoplanet atmospheres cannot be reliably retrieved from JWST spectra unless observations combine the visible scattering slope with mid-infrared resonance features, and it supports this…

desk verdict A useful, honest toolkit paper whose main information-content conclusion is solid but slightly overgeneralized: the controlled simulations only test compact-sphere Mie aerosols, and the paper's own porous-particle test shows the bias risk. read the letter →

arxiv 2505.18715 v2 pith:IO6KIRPE submitted 2025-05-24 astro-ph.EP astro-ph.IM

Quentin Changeat , Deborah Bardet , Katy Chubb , Achrene Dyrek , Billy Edwards , Kazumasa Ohno , Olivia Venot This is my paper · ORCID
classification astro-ph.EPastro-ph.IM
keywords exoplanetatmospheresatmosphericretrievalcloudsandhazesaerosolparameterizationJWSTMiescatteringTitanhotJupiters
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 tries to establish that the physical properties of aerosol particles in exoplanet atmospheres—what they are made of, how big they are, and how many there are—cannot be reliably recovered from JWST spectra unless the observations cover both the visible scattering slope and mid-infrared resonance features at the same time. The authors build a flexible, Mie-theory-based aerosol parameterization inside the TauREx retrieval framework, validate it on Cassini occultation data of Titan, and apply it to JWST observations of HAT-P-18 b, WASP-39 b, WASP-96 b, and WASP-107 b. In parallel, controlled retrievals on simulated JWST data show that narrow wavelength coverage produces apparently good fits while retrieving wrong cloud composition, chemistry, and metallicity. The practical consequence is that JWST's single instruments cannot simultaneously provide the needed wavelength range, and stitching together observations from different visits introduces offsets and temporal-variability biases. If the claim holds, interpreting JWST clouds and hazes will require coordinated observations with other facilities or a relaxation of what can be claimed from JWST spectra alone.

What carries the argument

The carrier of the argument is TauREx-PyMieScatt, a plugin for the TauREx retrieval framework that computes Mie extinction cross-sections for spherical aerosol particles from their complex refractive index and a chosen particle size distribution (one-parameter gamma from Budaj et al. 2015, log-normal, or modified gamma), and places the particles in pressure-bounded layers with retrievable number density. It is complemented by TauREx-MultiModel, which mixes clear and cloudy atmospheric regions to model partial cloud coverage, and TauREx-InstrumentSystematics, which fits vertical offsets between combined datasets. The mechanism does the work by letting the same retrieval code treat everything from Titan's tholin hazes to hot-Jupiter silicate clouds, and by enabling controlled experiments in which the input aerosol truth is known and the retrieved parameters can be compared across wavelength subsets.

What would settle it

Take a WASP-107 b-like simulated spectrum with fractal or porous aerosol particles, add JWST noise for NIRISS+NIRSpec+MIRI as in the paper's Case 1b, and run the spherical-particle retrieval: if the retrieved metallicity and cloud composition match the input, the full-coverage prescription survives; the paper's own FM2 experiment already shows metallicity bias, so a positive result would require additional model freedom such as porosity or aggregate parameters to be included in the retrieval.

Watch

Extended reading notes

Core claim

The paper's central claim is stated in its conclusion: to minimally constrain aerosols, observations need to be sensitive to both the visible light scattering slope and longer wavelength resonance features, such as the 10µm Si-O stretch. Without that combined information, and in the absence of priors on aerosol composition, retrievals find spectra that fit the data but infer incorrect cloud species, abundances, and metallicities; in the simulated cases, metallicity is off by roughly 10σ and SO2 by about 4σ when only NIRISS+NIRSpec or MIRI data are used. JWST has no single instrument covering both regions simultaneously, and combining datasets from different visits is plagued by offset and shape incompatibilities, as seen between the NIRSpec and NIRCam data of WASP-107 b. The paper also finds that JWST is largely insensitive to the vertical aerosol distribution and to the full particle size distribution, so simple one-parameter size distributions suffice, while particle porosity and non-spherical shapes introduce biases that even full wavelength coverage does not fully remove.

Load-bearing premise

The load-bearing premise is that the simple spherical-particle aerosol model used in the retrievals is close enough to reality that the wavelength-coverage requirements derived from it transfer to real exoplanet aerosols; if real particles are more complex, as Titan's fractal hazes and the paper's own porous-particle simulations suggest, the required coverage and achievable accuracy could differ.

Editorial extensions

If this is right

  • JWST-only aerosol characterization cannot rely on a single instrument; combinations such as NIRISS plus MIRI are needed, and such combinations must be treated as potentially systematics-limited rather than cleanly constraining.
  • When no mid-infrared resonance feature is covered, simple phenomenological cloud models such as Lee et al. (2013) are sufficient and give results robust to the assumed cloud species, so complex microphysics is not needed for those datasets.
  • Detecting and identifying silicate clouds requires the 8–11 µm Si-O feature; the paper's WASP-107 b retrievals consistently favor SiO2, but the full feature shape needs a secondary component such as MgSiO3 or Mg2SiO4 and depends on particle-shape assumptions.
  • JWST data do not constrain the vertical profile of aerosol abundance or the shape of the particle size distribution, so simplified parameterizations capture the available information and should be used to avoid over-interpretation.
  • Breaking cloud–chemistry degeneracies will require simultaneous visible-to-mid-infrared coverage, which the paper argues can come from synergies with other observatories rather than from JWST alone.

Reading between the lines

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

  • If hot-Jupiter aerosols are as structurally complex as Titan's fractal hazes, the paper's information-content estimates are likely optimistic: its own porous-particle simulation shows biases persist even with full wavelength coverage, so coverage alone may not recover true sizes or metallicities.
  • The WASP-96 b degeneracy between alkali line wings and a scattering slope suggests that stellar activity or limb-darkening errors could masquerade as either clouds or enhanced Na/K; a direct test is to fit the same NIRISS spectrum with and without stellar heterogeneities.
  • The paper's conclusion that JWST is insensitive to vertical aerosol profiles sets a boundary for microphysical cloud models: they can predict observable spectra, but JWST retrievals cannot validate their vertical transport predictions.
  • If the NIRCam/NIRSpec incompatibility in WASP-107 b is astrophysical rather than instrumental, repeated NIRISS visits separated by days could serve as a direct probe of exoplanet aerosol weather.
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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 / 5 minor

Summary. The paper presents a flexible aerosol parameterization implemented as TauREx plugins (TauREx-PyMieScatt, TauREx-MultiModel, TauREx-InstrumentSystematics) and applies it to atmospheric retrievals of Cassini Titan occultation data and JWST observations of HAT-P-18b, WASP-39b, WASP-96b, and WASP-107b. It also reports controlled simulation experiments with synthetic JWST data to study the information content of different wavelength coverages and aerosol model assumptions. The central claim is that robust characterization of cloud and haze properties requires sensitivity to both the visible scattering slope and longer-wavelength resonance features, and that JWST's non-simultaneous coverage from separate instruments makes such characterization difficult.

Significance. The paper makes a useful practical contribution by releasing open-source retrieval plugins, benchmarking a general-purpose retrieval code on an external solar-system dataset (Cassini/VIMS Titan occultations), and applying it to recent JWST data. The multiple independent demonstrations of aerosol degeneracies—identical posteriors for KCl, Na2S, and ZnS with NIRISS, the Na/K versus haze degeneracy for WASP-96b, and the reported NIRSpec/NIRCam spectral incompatibility for WASP-107b—support the qualitative conclusion that aerosol properties are hard to pin down with current JWST observations. The controlled simulations also provide useful parameterization guidance, e.g., weak sensitivity to the vertical aerosol profile and to the full particle size distribution. If the result holds, it is a valuable caution for the field, but the strength of the general conclusion is limited by the fact that the simulations are mostly self-retrievals within the same compact-sphere Mie framework.

major comments (3)
  1. [Section 5 and Section 6, Appendix A.1] The controlled experiments of Section 5 generate the true spectra with the same TauREx-PyMieScatt compact-sphere Mie parameterization used in the retrievals (Appendix A.1, Eqs. A.3–A.4). Case 1a versus Case 2 therefore demonstrates degeneracies and their resolution within that assumed model family, but does not test whether the full-coverage remedy survives a more realistic aerosol truth. The one out-of-family experiment present, Case 1b/FM2 with 50% porous particles, shows in Section 5.2 and Figure 4 that spherical-particle retrievals fit the full-coverage spectrum convincingly while returning biased particle size, number density, and metallicity. Since Titan's hazes are known fractal aggregates (Section 3, with references to Rannou et al. 2022) and aggregates are not included in the simulated truths, the conclusion in Section 6 that observations need both the visible scattering slope and longer-wavelength resonance features is not demonstrated to be sufficient; the paper should explicitly qualify this claim to the assumed spherical Mie family, or add an out-of-family aggregate forward-model test.
  2. [Section 3 and Figure B1] The Titan benchmark is a genuine external validation and a strength of the paper, but it validates the flexibility of the parameterized retrieval and its ability to recover bulk chemistry, not the microphysical accuracy of the aerosol model. The retrieved haze radius changes by a factor of two depending on the opacity source (µ_tholins ~0.15 µm for HITRAN versus ~0.3 µm for ExoMol), and the authors note that fractal aggregates, which are crucial for Titan, are not considered. The claim in Section 3 that the Titan experiment offers guidance on which atmospheric properties can be reliably retrieved is therefore supported, but the benchmark should not be used as evidence that the adopted compact-sphere aerosol model is an accurate representation of real aerosol microphysics.
  3. [Section 4.2 and Figure C4] The WASP-107b analysis reports a significant incompatibility between the NIRSpec-G395H and NIRCam-F322W2 spectra, with retrieved inter-instrument offsets up to 250 ppm, and the paper uses this as evidence that combining non-simultaneous JWST datasets is problematic. However, the controlled full-coverage simulations in Section 5 assume idealized, offset-free combination of NIRISS, NIRSpec, and MIRI data. The information-content estimate from those simulations is therefore an upper bound that ignores the systematic combination errors demonstrated on real data. The paper should state this explicitly so that the Section 6 conclusion is not read as applying to real, imperfectly combined datasets without further caveats.
minor comments (5)
  1. [Section 2, Cassini retrievals] The text lists C2H8 among the molecular species included in the Titan retrievals; this should presumably be C3H8, which is the species listed in Table 1 and discussed in Section 3.
  2. [Abstract and Section 4.1] There are several typographical errors: 'by a single instruments' in the abstract, 'think layer' for 'thick layer' in Section 4.1, and 'dis-equilibrium' for 'disequilibrium' in Section 4.2.
  3. [Section 4.1] The statement that the WASP-96b data from Taylor et al. (2023) could not be fully compared because the reduced spectra in Radica et al. (2023) could not be found is vague; the authors should specify which data products were unavailable and how this affects the comparison.
  4. [Figure C3 caption] The phrase 'inverted corner plots' is unclear; the authors likely mean that the FRECKLL posteriors are shown in the upper-right triangle, but this should be stated more explicitly.
  5. [Data Availability] Several URLs are broken across line breaks with inserted spaces (e.g., 'https://github.com/ucl- exopl anets/TauREx3'), which will make them unusable in the published version; the links should be formatted as proper hyperlinks.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the Titan benchmark provides external grounding, the controlled simulations are transparent identifiability checks, and the paper's own limitations prevent any claim from being forced by construction.

full rationale

The paper's central claims are not circular. The aerosol retrieval framework is benchmarked against Cassini/VIMS occultations of Titan, an external dataset with independent in-situ constraints (e.g., Fulchignoni et al. 2005; Niemann et al. 2010; Coustenis et al. 2016), so the method is checked against a known truth that is not generated by the retrieval model itself. The controlled simulations in Section 5 are explicitly self-retrievals, described as such ('Case 1a: Baseline with spheres ... it is a self-retrieval for FM1'), and self-retrieval is a standard identifiability test rather than a construction-level equivalence: the paper does not fit parameters to data and then relabel those fits as predictions. The conclusion that wide wavelength coverage is needed is an information-content statement conditional on the assumed compact-sphere Mie model family, and the paper explicitly discloses this limitation in Section 3 ('cloud and haze particles are assumed to be compact spheres') and Section 5.2, where a porous-particle forward model is still fit by spherical retrievals with biased parameters even with full coverage. This is a stated limitation, not a circular step. The paper also supports the wide-coverage conclusion by citing independent prior studies (Lee et al. 2014; Wakeford & Sing 2015; Mai & Line 2019; Gao et al. 2021). References to TauREx and FRECKLL are code/tool citations rather than load-bearing self-citations, and no uniqueness theorem or ansatz is smuggled in via author-only citations. No derivation step reduces to its own input by definition, so there is no circularity to report.

Assumptions & free parameters 6 free parameters · 7 assumptions · 0 invented entities

The retrieval framework relies on established radiative transfer and chemistry codes; the main non-standard assumptions are the aerosol microphysics (spherical Mie particles, fixed size distributions, limited species menu) and the simplified kinetic scheme. No new physical entities are introduced; the plugins are software artifacts.

free parameters (6)
  • L13 cloud particle radius (log10 mu_lee) for HAT-P-18b = -1.41 (free), -0.89 (FRECKLL)
    Aerosol particle size fitted to NIRISS data; central to the claim that aerosol properties are retrievable but degenerate with haze model choice.
  • L13 cloud number density (log10 chi_lee) for HAT-P-18b = 11.27 (free), 8.88 (FRECKLL)
    Fitted aerosol column density; posteriors are wide, reflecting weak constraints.
  • Instrument vertical offsets (HST, MIRI) for WASP-107b = -194 to +269 ppm depending on model
    Fitted offsets used to combine multi-epoch data; up to 250 ppm, indicating systematics or variability.
  • Metallicity Z (FRECKLL) for WASP-107b = log Z = 1.44 to 1.64 (20-50x solar)
    Fitted via FRECKLL chemistry; depends on reduced chemical scheme.
  • Vertical mixing coefficient log10(Kzz) = 8.5 to 10.8 across retrievals
    Fitted disequilibrium chemistry parameter; high values needed to match spectra.
  • SiO2 particle radius (log10 mu) for WASP-107b = -0.45 to -1.74 depending on dataset/model
    Fitted to 8-10 micron silicate feature; central evidence for SiO2 detection.
assumptions (7)
  • standard math Mie theory scattering for spherical homogeneous particles
    Used in TauREx-PyMieScatt to compute extinction efficiencies (Section 2, Appendix A.1); standard electromagnetic scattering result.
  • standard math Effective Medium Theory (Bruggeman/Maxwell-Garnett) for porous particles
    Used in Appendix A.1 to derive refractive indices of porous particles in FM2; standard mixing rules.
  • domain assumption One-parameter gamma size distribution (Budaj et al. 2015) adequately represents aerosol size distributions
    Adopted for all main retrievals; Section 5.3 shows JWST is insensitive to the full size distribution, supporting the simplification but still an assumption.
  • domain assumption Aerosols in the analyzed exoplanet atmospheres are compact spheres
    Section 2 states 'we concentrate on spherical particles'; Section 5.2 shows porosity biases retrievals, so this assumption affects retrieved sizes and metallicities.
  • domain assumption Reduced FRECKLL chemical scheme without photochemistry is adequate
    Used for FRECKLL retrievals (Venot et al. 2020 reduced scheme); the authors note photochemistry and S-species are missing (Sections 2, 4.1, 4.2), which could bias abundances.
  • domain assumption Multi-instrument datasets can be combined using per-instrument vertical offsets
    TauREx-InstrumentSystematics adds offsets; WASP-107b requires up to 250 ppm offsets, and NIRSpec/NIRCam shapes are incompatible (Section 4.2).
  • domain assumption Robinson et al. (2014) consolidated Cassini occultations are suitable as a benchmark
    Used in Section 3; the data combine four occultations and are not spatially/temporally resolved, limiting fidelity.

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Cite this review

Pith. "Pith review of Cloud and Haze Parameterization in Atmospheric Retrievals: Insights from Titan's Cassini Data and JWST Observations of Hot Jupiters." pith.science (2026). https://pith.science/paper/IO6KIRPE

@misc{pith2026250518715,
  author       = {Pith},
  title        = {Pith review of: Cloud and Haze Parameterization in Atmospheric Retrievals: Insights from Titan's Cassini Data and JWST Observations of Hot Jupiters},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/IO6KIRPE}},
  note         = {Machine review of arXiv:2505.18715}
}
read the original abstract

Context: Before JWST, telescope observations were not sensitive enough to constrain the nature of clouds in exo-atmospheres. Recent observations, however, have inferred cloud signatures as well as haze-enhanced scattering slopes motivating the need for modern inversion techniques and a deeper understanding of the JWST information content. Aims: We aim to investigate the information content of JWST exoplanet spectra. We particularly focus on designing an inversion technique able to handle a wide range of cloud and hazes. Methods: We build a flexible aerosol parameterization within the TauREx framework, enabling us to conduct atmospheric retrievals of planetary atmospheres. The method is evaluated on available Cassini occultations of Titan. We then use the model to interpret the recent JWST data for the prototypical hot Jupiters HAT-P-18 b, WASP-39 b, WASP-96 b, and WASP-107 b. In parallel, we perform complementary simulations on controlled scenarios to further understand the information content of JWST data and provide parameterization guidelines. Results: Our results use free and kinetic chemistry retrievals to extract the main atmospheric properties of key JWST exoplanets, including their molecular abundances, thermal structures, and aerosol properties. In our investigations, we show the need for a wide wavelength coverage to robustly characterize clouds and hazes-which is necessary to mitigate biases arising from our lack of priors on their composition-and break degeneracies with atmospheric chemical composition. With JWST, the characterization of clouds and hazes might be difficult due to the lack of simultaneous wavelength coverage from visible to mid-infrared by a single instruments and the likely presence of temporal variability between visits (from e.g., observing conditions, instrument systematics, stellar host variability, or planetary weather).

Figures

Figures reproduced from arXiv: 2505.18715 by the authors.

Figure 1
Figure 1. Retrievals of Cassini/VIMS occultation of Titan. Top left: observations and best-fit TauREx retrievals. Bottom left: breakdown of the extinction contributions in the tholin + CH4(l) (HITRAN) case. Right: Atmospheric properties inferred for the tholin + CH4(l) (HITRAN) case. The source for the opacity data (i.e, HITRAN or ExoMol) is important and can slightly change the best-fit spectrum and retrieval interpretation.… view at source ↗
Figure 2
Figure 2. Results of the atmospheric retrievals using the Lee et al. (2013) cloud model for the NIRISS observations. The observed spectra, best-fit models (free chemistry in blue and FRECKLL chemistry in purple) and residuals for the FRECKLL retrieval are shown in the top panel. The lower panels show retrieved T − p and chemistry—free chemistry in middle row, and FRECKLL chemistry in bottom row—with 1 σ confidence intervals, … view at source ↗
Figure 3
Figure 3. Summarized results of the retrievals on the WASP-107 b HST and JWST data. The top left panel shows the observed spectra corrected for offsets for the FRECKLL retrievals (datapoints), the best-fits of free and FRECKLL retrievals (solid lines), and the contributions of the FRECKLL HST+NIRCam+MIRI retrieval (shaded areas). The top right panel shows the retrieved thermal structures including 1 σ and 3 σ confidence regio… view at source ↗
Figures from the paper (1 more)
Figure 4
Figure 4. Figure 4: Simulated observations and retrieval best-fit models of our controlled experiments. The top panel shows retrievals on the full simulated spectrum with JWST/NIRISS, JWST/NIRSpec-G395H, and JWST/MIRI. The middle panel shows retrievals on subsets of the simulated data. Bo…

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Reference graph

Works this paper leans on

167 extracted references · 28 canonical work pages

  1. [1]

    , " * 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 ...

  2. [2]

    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....

  3. [3]

    Abel, M., Frommhold, L., Li, X., & Hunt, K. L. 2011, The Journal of Physical Chemistry A, 115, 6805

    2011

  4. [4]

    2012, The Journal of chemical physics, 136, 044319

    ---. 2012, The Journal of chemical physics, 136, 044319

    2012

  5. [5]

    L., Hayes , A

    \'A d \'a mkovics , M., Mitchell , J. L., Hayes , A. G., et al. 2016, , 270, 376, 10.1016/j.icarus.2015.05.023

    work page doi:10.1016/j.icarus.2015.05.023 2016

  6. [6]

    Adams , D., Gao , P., de Pater , I., & Morley , C. V. 2019, , 874, 61, 10.3847/1538-4357/ab074c

    doi:10.3847/1538-4357/ab074c 2019

  7. [7]

    R., Furtenbacher , T., Tennyson , J., Yurchenko , S

    Al Derzi , A. R., Furtenbacher , T., Tennyson , J., Yurchenko , S. N., & Cs \'a sz \'a r , A. G. 2015, Journal of Quantitative Spectroscopy and Radiative Transfer, 161, 117, 10.1016/j.jqsrt.2015.03.034

    work page doi:10.1016/j.jqsrt.2015.03.034 2015

  8. [8]

    F., Changeat , Q., Venot , O., Waldmann , I

    Al-Refaie , A. F., Changeat , Q., Venot , O., Waldmann , I. P., & Tinetti , G. 2022, , 932, 123, 10.3847/1538-4357/ac6dcd

    doi:10.3847/1538-4357/ac6dcd 2022

Show all 167 references
  1. [9]

    F., Changeat , Q., Waldmann , I

    Al-Refaie , A. F., Changeat , Q., Waldmann , I. P., & Tinetti , G. 2021, The Astrophysical Journal, 917, 37, 10.3847/1538-4357/ac0252

    2021 doi

  2. [10]

    F., Venot , O., Changeat , Q., & Edwards , B

    Al-Refaie , A. F., Venot , O., Changeat , Q., & Edwards , B. 2024, , 967, 132, 10.3847/1538-4357/ad3dee

    2024 doi

  3. [11]

    F., Spiegelman , F., & Kielkopf , J

    Allard , N. F., Spiegelman , F., & Kielkopf , J. F. 2016, , 589, A21, 10.1051/0004-6361/201628270

    2016 doi

  4. [12]

    F., Spiegelman , F., Leininger , T., & Molliere , P

    Allard , N. F., Spiegelman , F., Leininger , T., & Molliere , P. 2019, , 628, A120, 10.1051/0004-6361/201935593

    2019 doi

  5. [13]

    M., Samuelson , R

    Anderson , C. M., Samuelson , R. E., & Nna-Mvondo , D. 2018, , 214, 125, 10.1007/s11214-018-0559-5

    2018 doi

  6. [14]

    O., Chubb , K

    Anisman , L. O., Chubb , K. L., Elsey , J., et al. 2022, , 278, 108013, 10.1016/j.jqsrt.2021.108013

    2022

  7. [15]

    2024, , 530, 482, 10.1093/mnras/stae826

    Arfaux , A., & Lavvas , P. 2024, , 530, 482, 10.1093/mnras/stae826

    2024 doi

  8. [16]

    J., & Scott , P

    Asplund , M., Grevesse , N., Sauval , A. J., & Scott , P. 2009, , 47, 481, 10.1146/annurev.astro.46.060407.145222

    2009

  9. [17]

    2005, Space Sci Rev, 116, 121, 10.1007/s11214-005-1951-5

    Atreya , S., & Wong , A. 2005, Space Sci Rev, 116, 121, 10.1007/s11214-005-1951-5

    2005 doi

  10. [18]

    K., Crida , A., Guillot , T., et al

    Atreya , S. K., Crida , A., Guillot , T., et al. 2022, arXiv e-prints, arXiv:2205.06914, 10.48550/arXiv.2205.06914

    2022 doi arXiv

  11. [19]

    Azzam , A. A. A., Tennyson , J., Yurchenko , S. N., & Naumenko , O. V. 2016, Monthly Notices of the Royal Astronomical Society, 460, 4063, 10.1093/mnras/stw1133

    2016 doi

  12. [20]

    J., Strange, J

    Barber, R. J., Strange, J. K., Hill, C., et al. 2013, Monthly Notices of the Royal Astronomical Society, 437, 1828–1835, 10.1093/mnras/stt2011

    2013 doi

  13. [21]

    Barth , E. L. 2017, , 137, 20, 10.1016/j.pss.2017.01.003

    2017 doi

  14. [22]

    2020, Refractive Indices For Virga Exoplanet Cloud Model, 1.2, Zenodo, 10.5281/zenodo.5179187

    Batalha, N., & Marley, M. 2020, Refractive Indices For Virga Exoplanet Cloud Model, 1.2, Zenodo, 10.5281/zenodo.5179187

    2020 doi

  15. [23]

    E., Mandell , A., Pontoppidan , K., et al

    Batalha , N. E., Mandell , A., Pontoppidan , K., et al. 2017, , 129, 064501, 10.1088/1538-3873/aa65b0

    2017 doi

  16. [24]

    2009, , 201, 198, 10.1016/j.icarus.2008.12.024

    Bellucci , A., Sicardy , B., Drossart , P., et al. 2009, , 201, 198, 10.1016/j.icarus.2008.12.024

    2009 doi

  17. [25]

    F., & Huffman, D

    Bohren, C. F., & Huffman, D. R. 2008, Absorption and scattering of light by small particles (John Wiley & Sons)

    2008

  18. [26]

    1987, , 318, 940, 10.1086/165426

    Borysow , A., & Frommhold , L. 1987, , 318, 940, 10.1086/165426

    1987 doi

  19. [27]

    1993, , 105, 175, 10.1006/icar.1993.1117

    Borysow , A., & Tang , C. 1993, , 105, 175, 10.1006/icar.1993.1117

    1993

  20. [28]

    Bruggeman, V. D. 1935, Annalen der physik, 416, 636

    1935

  21. [29]

    2015, , 454, 2, 10.1093/mnras/stv1711

    Budaj , J., Kocifaj , M., Salmeron , R., & Hubeny , I. 2015, , 454, 2, 10.1093/mnras/stv1711

    2015 doi

  22. [30]

    1993, , 41, 257, 10.1016/0032-0633(93)90021-S

    Cabane , M., Rannou , P., Chassefiere , E., & Israel , G. 1993, , 41, 257, 10.1016/0032-0633(93)90021-S

    1993 doi

  23. [31]

    2019, Astronomy & Astrophysics, 623, A161, 10.1051/0004-6361/201834384

    Caldas, A., Leconte, J., Selsis, F., et al. 2019, Astronomy & Astrophysics, 623, A161, 10.1051/0004-6361/201834384

    2019 doi

  24. [32]

    L., May , E

    Carter , A. L., May , E. M., Espinoza , N., et al. 2024, Nature Astronomy, 8, 1008, 10.1038/s41550-024-02292-x

    2024 doi

  25. [33]

    2025, Reference HDF5 cross-sections for TauREx3, Zenodo, 10.5281/zenodo.15495830

    Changeat, Q. 2025, Reference HDF5 cross-sections for TauREx3, Zenodo, 10.5281/zenodo.15495830

    2025 doi

  26. [34]

    2020, The Astrophysical Journal, 898, 155, 10.3847/1538-4357/ab9b82

    Changeat , Q., & Al-Refaie , A. 2020, The Astrophysical Journal, 898, 155, 10.3847/1538-4357/ab9b82

    2020 doi

  27. [35]

    F., Edwards , B., Waldmann , I

    Changeat , Q., Al-Refaie , A. F., Edwards , B., Waldmann , I. P., & Tinetti , G. 2021, The Astrophysical Journal, 913, 73, 10.3847/1538-4357/abf2bb

    2021 doi

  28. [36]

    F., et al

    Changeat , Q., Edwards , B., Al-Refaie , A. F., et al. 2020 a , The Astronomical Journal, 160, 260, 10.3847/1538-3881/abbe12

    2020 doi

  29. [37]

    P., & Tinetti, G

    Changeat, Q., Edwards, B., Waldmann, I. P., & Tinetti, G. 2019, The Astrophysical Journal, 886, 39, 10.3847/1538-4357/ab4a14

    2019 doi

  30. [38]

    P., & Tinetti , G

    Changeat , Q., Keyte , L., Waldmann , I. P., & Tinetti , G. 2020 b , The Astrophysical Journal, 896, 107, 10.3847/1538-4357/ab8f8b

    2020 doi

  31. [39]

    W., Cho , J

    Changeat , Q., Skinner , J. W., Cho , J. Y. K., et al. 2024, , 270, 34, 10.3847/1538-4365/ad1191

    2024 doi

  32. [40]

    N., Finenko , A

    Chistikov , D. N., Finenko , A. A., Lokshtanov , S. E., Petrov , S. V., & Vigasin , A. A. 2019, , 151, 194106, 10.1063/1.5125756

    2019 doi

  33. [41]

    Cho , J. Y. K., & Polvani , L. M. 1996, Physics of Fluids, 8, 1531, 10.1063/1.868929

    1996 doi

  34. [42]

    Y-K ., Menou, K., Hansen, B

    Cho, J. Y-K ., Menou, K., Hansen, B. M. S., & Seager, S. 2003, The Astrophysical Journal, 587, L117–L120, 10.1086/375016

    2003 doi

  35. [43]

    L., Tennyson , J., & Yurchenko , S

    Chubb , K. L., Tennyson , J., & Yurchenko , S. N. 2020, Monthly Notices of the Royal Astronomical Society, 493, 1531, 10.1093/mnras/staa229

    2020 doi

  36. [44]

    L., Rocchetto, M., Yurchenko, S

    Chubb, K. L., Rocchetto, M., Yurchenko, S. N., et al. 2021, Astronomy & Astrophysics, 646, A21, 10.1051/0004-6361/202038350

    2021 doi

  37. [45]

    L., Robert , S., Sousa-Silva , C., et al

    Chubb , K. L., Robert , S., Sousa-Silva , C., et al. 2024, RAS Techniques and Instruments, 3, 636, 10.1093/rasti/rzae039

    2024 doi

  38. [46]

    A., Yurchenko , S

    Coles , P. A., Yurchenko , S. N., & Tennyson , J. 2019, Monthly Notices of the Royal Astronomical Society, 490, 4638, 10.1093/mnras/stz2778

    2019 doi

  39. [47]

    D., Kreidberg , L., Welbanks , L., et al

    Col \'o n , K. D., Kreidberg , L., Welbanks , L., et al. 2020, , 160, 280, 10.3847/1538-3881/abc1e9

    2020 doi

  40. [48]

    2023, , 943, L10, 10.3847/2041-8213/acaead

    Constantinou , S., Madhusudhan , N., & Gandhi , S. 2023, , 943, L10, 10.3847/2041-8213/acaead

    2023 doi

  41. [49]

    2020, , 339, 113571, 10.1016/j.icarus.2019.113571

    Cours , T., Cordier , D., Seignovert , B., Maltagliati , L., & Biennier , L. 2020, , 339, 113571, 10.1016/j.icarus.2019.113571

    2020

  42. [50]

    2003, , 161, 383, 10.1016/S0019-1035(02)00028-3

    Coustenis , A., Salama , A., Schulz , B., et al. 2003, , 161, 383, 10.1016/S0019-1035(02)00028-3

    2003 doi

  43. [51]

    E., Nixon , C

    Coustenis , A., Jennings , D. E., Nixon , C. A., et al. 2010, , 207, 461, 10.1016/j.icarus.2009.11.027

    2010 doi

  44. [52]

    E., Achterberg , R

    Coustenis , A., Jennings , D. E., Achterberg , R. K., et al. 2016, , 270, 409, 10.1016/j.icarus.2015.08.027

    2016 doi

  45. [53]

    Cox, A. N. 2015, Allen’s astrophysical quantities (Springer)

    2015

  46. [54]

    1964, , 3, 187, 10.1364/AO.3.000187

    Deirmendjian , D. 1964, , 3, 187, 10.1364/AO.3.000187

    1964 doi

  47. [55]

    2023, , 669, A150, 10.1051/0004-6361/202244881

    Di Maio , C., Changeat , Q., Benatti , S., & Micela , G. 2023, , 669, A150, 10.1051/0004-6361/202244881

    2023 doi

  48. [56]

    2024, , 625, 51, 10.1038/s41586-023-06849-0

    Dyrek , A., Min , M., Decin , L., et al. 2024, , 625, 51, 10.1038/s41586-023-06849-0

    2024 doi

  49. [57]

    2024, , 962, L30, 10.3847/2041-8213/ad2000

    Edwards , B., & Changeat , Q. 2024, , 962, L30, 10.3847/2041-8213/ad2000

    2024 doi

  50. [58]

    Edwards , B., Tsiaras , A., Changeat , Q., & Yip , K. H. 2024, RAS Techniques and Instruments, 3, 415, 10.1093/rasti/rzae023

    2024 doi

  51. [59]

    2023, , 269, 31, 10.3847/1538-4365/ac9f1a

    Edwards , B., Changeat , Q., Tsiaras , A., et al. 2023, , 269, 31, 10.3847/1538-4365/ac9f1a

    2023 doi

  52. [60]

    M., et al

    Espinoza , N., \'U beda , L., Birkmann , S. M., et al. 2023, , 135, 018002, 10.1088/1538-3873/aca3d3

    2023 doi

  53. [61]

    R., & Roudier , G

    Estrela , R., Swain , M. R., & Roudier , G. M. 2022, , 941, L5, 10.3847/2041-8213/aca2aa

    2022 doi

  54. [62]

    2001, , 378, 228, 10.1051/0004-6361:20011196

    Fabian , D., Henning , T., J \"a ger , C., et al. 2001, , 378, 228, 10.1051/0004-6361:20011196

    2001 doi

  55. [63]

    R., & MacDonald , R

    Fairman , C., Wakeford , H. R., & MacDonald , R. J. 2024, , 167, 240, 10.3847/1538-3881/ad3454

    2024 doi

  56. [64]

    D., Radica , M., Welbanks , L., et al

    Feinstein , A. D., Radica , M., Welbanks , L., et al. 2023, , 614, 670, 10.1038/s41586-022-05674-1

    2023 doi

  57. [65]

    K., Line , M

    Feng , Y. K., Line , M. R., Fortney , J. J., et al. 2016, The Astrophysical Journal, 829, 52, 10.3847/0004-637X/829/1/52

    2016 doi

  58. [66]

    N., Gustafsson, M., & Orton, G

    Fletcher, L. N., Gustafsson, M., & Orton, G. S. 2018, The Astrophysical Journal Supplement Series, 235, 24

    2018

  59. [67]

    2023, , 520, 4683, 10.1093/mnras/stad245

    Fonte , S., Turrini , D., Pacetti , E., et al. 2023, , 520, 4683, 10.1093/mnras/stad245

    2023 doi

  60. [68]

    J., Radica , M., et al

    Fournier-Tondreau , M., MacDonald , R. J., Radica , M., et al. 2024, , 528, 3354, 10.1093/mnras/stad3813

    2024 doi

  61. [69]

    K., et al

    Fu , G., Espinoza , N., Sing , D. K., et al. 2022, , 940, L35, 10.3847/2041-8213/ac9977

    2022 doi

  62. [70]

    2005, , 438, 785, 10.1038/nature04314

    Fulchignoni , M., Ferri , F., Angrilli , F., et al. 2005, , 438, 785, 10.1038/nature04314

    2005 doi

  63. [71]

    2018, , 863, 165, 10.3847/1538-4357/aad461

    Gao , P., & Benneke , B. 2018, , 863, 165, 10.3847/1538-4357/aad461

    2018 doi

  64. [72]

    R., Moran , S

    Gao , P., Wakeford , H. R., Moran , S. E., & Parmentier , V. 2021, Journal of Geophysical Research (Planets), 126, e06655, 10.1029/2020JE006655

    2021 doi

  65. [73]

    S., Batalha , N

    Gharib-Nezhad , E. S., Batalha , N. E., Chubb , K., et al. 2024, RAS Techniques and Instruments, 3, 44, 10.1093/rasti/rzad058

    2024 doi

  66. [74]

    K., Wakeford , H

    Grant , D., Lewis , N. K., Wakeford , H. R., et al. 2023, , 956, L29, 10.3847/2041-8213/acfc3b

    2023 doi

  67. [75]

    J., Allen, N

    Harrison, J. J., Allen, N. D. C., & Bernath, P. F. 2010, Journal of Quantitative Spectroscopy and Radiative Transfer, 111, 357, 10.1016/j.jqsrt.2009.09.010

    2010 doi

  68. [76]

    J., & Bernath, P

    Harrison, J. J., & Bernath, P. F. 2010, Journal of Quantitative Spectroscopy and Radiative Transfer, 111, 1282, 10.1016/j.jqsrt.2009.11.027

    2010 doi

  69. [77]

    Hejazi , N., Crossfield , I. J. M., Nordlander , T., et al. 2023, , 949, 79, 10.3847/1538-4357/accb97

    2023 doi

  70. [78]

    Helling , C., Woitke , P., & Thi , W. F. 2008, , 485, 547, 10.1051/0004-6361:20078220

    2008 doi

  71. [79]

    R., Timmes , F

    Hinkel , N. R., Timmes , F. X., Young , P. A., Pagano , M. D., & Turnbull , M. C. 2014, , 148, 54, 10.1088/0004-6256/148/3/54

    2014 doi

  72. [80]

    2023, arXiv e-prints, arXiv:2306.04676, 10.48550/arXiv.2306.04676

    Holmberg , M., & Madhusudhan , N. 2023, arXiv e-prints, arXiv:2306.04676, 10.48550/arXiv.2306.04676

    2023 doi arXiv

  73. [81]

    H \"o rst , S. M. 2017, Journal of Geophysical Research (Planets), 122, 432, 10.1002/2016JE005240

    2017 doi

  74. [82]

    2014, , 568, A42, 10.1051/0004-6361/201323199

    Kataoka , A., Okuzumi , S., Tanaka , H., & Nomura , H. 2014, , 568, A42, 10.1051/0004-6361/201323199

    2014 doi

  75. [83]

    2019, , 877, 109, 10.3847/1538-4357/ab1b1d

    Kawashima , Y., & Ikoma , M. 2019, , 877, 109, 10.3847/1538-4357/ab1b1d

    2019 doi

  76. [84]

    2009, Journal of Physics Condensed Matter, 21, 095404, 10.1088/0953-8984/21/9/095404

    Khachai , H., Khenata , R., Bouhemadou , A., et al. 2009, Journal of Physics Condensed Matter, 21, 095404, 10.1088/0953-8984/21/9/095404

    2009 doi

  77. [85]

    N., Sagan , C., Arakawa , E

    Khare , B. N., Sagan , C., Arakawa , E. T., et al. 1984, , 60, 127, 10.1016/0019-1035(84)90142-8

    1984 doi

  78. [86]

    A., et al

    Kiefer , S., Samra , D., Lewis , D. A., et al. 2024, , 690, A244, 10.1051/0004-6361/202450526

    2024 doi

  79. [87]

    2018, , 475, 94, 10.1093/mnras/stx3141

    Kitzmann , D., & Heng , K. 2018, , 475, 94, 10.1093/mnras/stx3141

    2018 doi

  80. [88]

    V., Gordon , I

    Kochanov , R. V., Gordon , I. E., Rothman , L. S., et al. 2016, , 177, 15, 10.1016/j.jqsrt.2016.03.005

    2016 doi

  81. [89]

    I., & Burrows , A

    Lacy , B. I., & Burrows , A. 2020 a , , 905, 131, 10.3847/1538-4357/abc01c

    2020 doi

  82. [90]

    2020 b , , 904, 25, 10.3847/1538-4357/abbc6c

    ---. 2020 b , , 904, 25, 10.3847/1538-4357/abbc6c

    2020 doi

  83. [91]

    V., & Griffith , C

    Lavvas , P., Yelle , R. V., & Griffith , C. A. 2010, , 210, 832, 10.1016/j.icarus.2010.07.025

    2010 doi

  84. [92]

    Lee , E. K. H. 2023, , 524, 2918, 10.1093/mnras/stad2037

    2023 doi

  85. [93]

    Lee , J.-M., Heng , K., & Irwin , P. G. J. 2013, The Astrophysical Journal, 778, 97, 10.1088/0004-637X/778/2/97

    2013 doi

  86. [94]

    Lee , J.-M., Irwin , P. G. J., Fletcher , L. N., Heng , K., & Barstow , J. K. 2014, , 789, 14, 10.1088/0004-637X/789/1/14

    2014 doi

  87. [95]

    E., Rothman, L

    Li, G., Gordon, I. E., Rothman, L. S., et al. 2015, The Astrophysical Journal Supplement Series, 216, 15

    2015

  88. [96]

    G., Wakeford , H

    Lodge , M. G., Wakeford , H. R., & Leinhardt , Z. M. 2024, , 527, 11113, 10.1093/mnras/stad3743

    2024 doi

  89. [97]

    2024, , 687, A110, 10.1051/0004-6361/202348802

    Lueber , A., Novais , A., Fisher , C., & Heng , K. 2024, , 687, A110, 10.1051/0004-6361/202348802

    2024 doi

  90. [98]

    F., et al

    Ma , S., Ito , Y., Al-Refaie , A. F., et al. 2023, , 957, 104, 10.3847/1538-4357/acf8ca

    2023 doi

  91. [99]

    2025, arXiv e-prints, arXiv:2504.07823, 10.48550/arXiv.2504.07823

    Ma , S., Saba , A., Faris Al-Refaie , A., et al. 2025, arXiv e-prints, arXiv:2504.07823, 10.48550/arXiv.2504.07823

    2025 doi arXiv

  92. [100]

    J., Goyal, J

    MacDonald, R. J., Goyal, J. M., & Lewis, N. K. 2020, The Astrophysical Journal, 893, L43, 10.3847/2041-8213/ab8238

    2020 doi

  93. [101]

    2009, The Astrophysical Journal, 707, 24, 10.1088/0004-637X/707/1/24

    Madhusudhan , N., & Seager , S. 2009, The Astrophysical Journal, 707, 24, 10.1088/0004-637X/707/1/24

    2009 doi

  94. [102]

    Mai , C., & Line , M. R. 2019, , 883, 144, 10.3847/1538-4357/ab3e6d

    2019 doi

  95. [103]

    2015, Icarus, 248, 1, https://doi.org/10.1016/j.icarus.2014.10.004

    Maltagliati, L., Bézard, B., Vinatier, S., et al. 2015, Icarus, 248, 1, https://doi.org/10.1016/j.icarus.2014.10.004

    2015 doi

  96. [104]

    P., Yachmenev, A., Tennyson, J., & Yurchenko, S

    Mant, B. P., Yachmenev, A., Tennyson, J., & Yurchenko, S. N. 2018, Monthly Notices of the Royal Astronomical Society, 478, 3220–3232, 10.1093/mnras/sty1239

    2018 doi

  97. [105]

    V., & Orton , G

    Martonchik , J. V., & Orton , G. S. 1994, , 33, 8306, 10.1364/AO.33.008306

    1994 doi

  98. [106]

    Maxwell-Garnett, J. C. 1904, Philosophical Transactions of the Royal Society of London. Series A, Containing Papers of a Mathematical or Physical Character, 203, 385

    1904

  99. [107]

    P., Coustenis , A., Samuelson , R

    McKay , C. P., Coustenis , A., Samuelson , R. E., et al. 2001, , 49, 79, 10.1016/S0032-0633(00)00051-9

    2001 doi

  100. [108]

    E., Biller , B

    Miles , B. E., Biller , B. A., Patapis , P., et al. 2023, , 946, L6, 10.3847/2041-8213/acb04a

    2023 doi

  101. [109]

    W., Chubb , K., Helling , C., & Kawashima , Y

    Min , M., Ormel , C. W., Chubb , K., Helling , C., & Kawashima , Y. 2020, Astronomy and Astrophysics, 642, A28, 10.1051/0004-6361/201937377

    2020 doi

  102. [110]

    Min , M., Waters , L. B. F. M., de Koter , A., et al. 2007, , 462, 667, 10.1051/0004-6361:20065436

    2007 doi

  103. [111]

    E., Stevenson , K

    Moran , S. E., Stevenson , K. B., Sing , D. K., et al. 2023, , 948, L11, 10.3847/2041-8213/accb9c

    2023 doi

  104. [112]

    B., Atreya , S

    Niemann , H. B., Atreya , S. K., Demick , J. E., et al. 2010, Journal of Geophysical Research (Planets), 115, E12006, 10.1029/2010JE003659

    2010 doi

  105. [113]

    K., Fortney , J

    Nikolov , N., Sing , D. K., Fortney , J. J., et al. 2018, , 557, 526, 10.1038/s41586-018-0101-7

    2018 doi

  106. [114]

    E., et al

    Niraula , P., de Wit , J., Gordon , I. E., et al. 2022, Nature Astronomy, 6, 1287, 10.1038/s41550-022-01773-1

    2022 doi

  107. [115]

    C., & Madhusudhan , N

    Nixon , M. C., & Madhusudhan , N. 2022, , 935, 73, 10.3847/1538-4357/ac7c09

    2022 doi

  108. [116]

    2018, , 859, 34, 10.3847/1538-4357/aabee3

    Ohno , K., & Okuzumi , S. 2018, , 859, 34, 10.3847/1538-4357/aabee3

    2018 doi

  109. [118]

    2020 b , , 891, 131, 10.3847/1538-4357/ab44bd

    ---. 2020 b , , 891, 131, 10.3847/1538-4357/ab44bd

    2020 doi

  110. [119]

    W., & Min , M

    Ormel , C. W., & Min , M. 2019, , 622, A121, 10.1051/0004-6361/201833678

    2019 doi

  111. [120]

    Palik , E. D. 1991, Handbook of optical constants of solids II

    1991

  112. [121]

    L., et al

    Peek , J., Desai , V., White , R. L., et al. 2019, in Bulletin of the American Astronomical Society, Vol. 51, 105. 1907.06234

    2019 arXiv

  113. [122]

    2025, Icarus, 429, 116418, 10.1016/j.icarus.2024.116418

    Perrin, Z., Carrasco, N., Gautier, T., et al. 2025, Icarus, 429, 116418, 10.1016/j.icarus.2024.116418

    2025

  114. [123]

    2017, , 471, 4355, 10.1093/mnras/stx1849

    Pinhas , A., & Madhusudhan , N. 2017, , 471, 4355, 10.1093/mnras/stx1849

    2017 doi

  115. [124]

    2020, Astronomy & Astrophysics, 636, A66, 10.1051/0004-6361/202037678

    Pluriel, W., Zingales, T., Leconte, J., & Parmentier, V. 2020, Astronomy & Astrophysics, 636, A66, 10.1051/0004-6361/202037678

    2020 doi

  116. [125]

    Polman , J., Waters , L. B. F. M., Min , M., Miguel , Y., & Khorshid , N. 2023, , 670, A161, 10.1051/0004-6361/202244647

    2023 doi

  117. [126]

    L., Kyuberis, A

    Polyansky, O. L., Kyuberis, A. A., Zobov, N. F., et al. 2018, Monthly Notices of the Royal Astronomical Society, 480, 2597

    2018

  118. [127]

    2024, , 969, 5, 10.3847/1538-4357/ad3de4

    Powell , D., & Zhang , X. 2024, , 969, 5, 10.3847/1538-4357/ad3de4

    2024 doi

  119. [128]

    2018, , 860, 18, 10.3847/1538-4357/aac215

    Powell , D., Zhang , X., Gao , P., & Parmentier , V. 2018, , 860, 18, 10.3847/1538-4357/aac215

    2018 doi

  120. [129]

    Querry, M., Chemical Research, D. . E. C. U., United States. Army Armament, M., Command, C., & Service, U. S. N. T. I. 1987, Optical Constants of Minerals and Other Materials from the Millimeter to the Ultraviolet, CRDC-CR (Chemical Research, Development & Engineering Center, ...

    1987

  121. [130]

    2023, , 524, 835, 10.1093/mnras/stad1762

    Radica , M., Welbanks , L., Espinoza , N., et al. 2023, , 524, 835, 10.1093/mnras/stad1762

    2023 doi

  122. [131]

    1995, , 118, 355, 10.1006/icar.1995.1196

    Rannou , P., Cabane , M., Chassefiere , E., et al. 1995, , 118, 355, 10.1006/icar.1995.1196

    1995

  123. [132]

    2010, , 208, 850, 10.1016/j.icarus.2010.03.016

    Rannou , P., Cours , T., Le Mou \'e lic , S., et al. 2010, , 208, 850, 10.1016/j.icarus.2010.03.016

    2010 doi

  124. [133]

    2022, , 666, A140, 10.1051/0004-6361/202243045

    Rannou , P., Coutelier , M., Rey , M., & Vinatier , S. 2022, , 666, A140, 10.1051/0004-6361/202243045

    2022 doi

  125. [134]

    D., Maltagliati , L., Marley , M

    Robinson , T. D., Maltagliati , L., Marley , M. S., & Fortney , J. J. 2014, Proceedings of the National Academy of Science, 111, 9042, 10.1073/pnas.1403473111

    2014 doi

  126. [135]

    P., Venot, O., Lagage, P.-O., & Tinetti, G

    Rocchetto, M., Waldmann, I. P., Venot, O., Lagage, P.-O., & Tinetti, G. 2016, The Astrophysical Journal, 833, 120, 10.3847/1538-4357/833/1/120

    2016 doi

  127. [136]

    R., et al

    Rotman , Y., Welbanks , L., Line , M. R., et al. 2025, arXiv e-prints, arXiv:2503.21702, 10.48550/arXiv.2503.21702

    2025 doi arXiv

  128. [137]

    J., Morley , C

    Rowland , M. J., Morley , C. V., & Line , M. R. 2023, , 947, 6, 10.3847/1538-4357/acbb07

    2023 doi

  129. [138]

    K., Mukherjee , S., et al

    Rustamkulov , Z., Sing , D. K., Mukherjee , S., et al. 2023, , 614, 659, 10.1038/s41586-022-05677-y

    2023 doi

  130. [139]

    2022, , 663, A47, 10.1051/0004-6361/202142651

    Samra , D., Helling , C., & Birnstiel , T. 2022, , 663, A47, 10.1051/0004-6361/202142651

    2022 doi

  131. [140]

    2020, , 639, A107, 10.1051/0004-6361/202037553

    Samra , D., Helling , C., & Min , M. 2020, , 639, A107, 10.1051/0004-6361/202037553

    2020 doi

  132. [141]

    2024, arXiv e-prints, arXiv:2409.09127, 10.48550/arXiv.2409.09127

    Schleich , S., Boro Saikia , S., Changeat , Q., et al. 2024, arXiv e-prints, arXiv:2409.09127, 10.48550/arXiv.2409.09127

    2024 doi arXiv

  133. [142]

    Scott , A., & Duley , W. W. 1996, , 105, 401, 10.1086/192321

    1996 doi

  134. [143]

    K., Fortney , J

    Sing , D. K., Fortney , J. J., Nikolov , N., et al. 2016, , 529, 59, 10.1038/nature16068

    2016 doi

  135. [144]

    K., Rustamkulov , Z., Thorngren , D

    Sing , D. K., Rustamkulov , Z., Thorngren , D. P., et al. 2024, , 630, 831, 10.1038/s41586-024-07395-z

    2024 doi

  136. [145]

    W., & Cho, J

    Skinner, J. W., & Cho, J. Y.-K. 2022, Monthly Notices of the Royal Astronomical Society, 511, 3584, 10.1093/mnras/stab2809

    2022 doi

  137. [146]

    W., Cho , J

    Skinner , J. W., Cho , J. Y. K., & N\"attil\"a, J. 2022, Submitted

    2022

  138. [147]

    J., Heinson , W

    Sumlin , B. J., Heinson , W. R., & Chakrabarty , R. K. 2018, , 205, 127, 10.1016/j.jqsrt.2017.10.012

    2018 doi

  139. [148]

    A., Vinatier , S., Lebonnois , S., & Irwin , P

    Sylvestre , M., Teanby , N. A., Vinatier , S., Lebonnois , S., & Irwin , P. G. J. 2018, , 609, A64, 10.1051/0004-6361/201630255

    2018 doi

  140. [149]

    Taylor , J., Parmentier , V., Irwin , P. G. J., et al. 2020, Monthly Notices of the Royal Astronomical Society, 493, 4342, 10.1093/mnras/staa552

    2020 doi

  141. [150]

    2023, , 10.1093/mnras/stad1547

    Taylor , J., Radica , M., Welbanks , L., et al. 2023, , 10.1093/mnras/stad1547

    2023 doi

  142. [151]

    N., Al-Refaie, A

    Tennyson, J., Yurchenko, S. N., Al-Refaie, A. F., et al. 2016, Journal of Molecular Spectroscopy, 327, 73 , https://doi.org/10.1016/j.jms.2016.05.002

    2016 doi

  143. [152]

    N., Zhang , J., et al

    Tennyson , J., Yurchenko , S. N., Zhang , J., et al. 2024, , 326, 109083, 10.1016/j.jqsrt.2024.109083

    2024

  144. [153]

    G., Doose , L., Engel , S., et al

    Tomasko , M. G., Doose , L., Engel , S., et al. 2008, , 56, 669, 10.1016/j.pss.2007.11.019

    2008 doi

  145. [154]

    Tsai , S.-M., Lee , E. K. H., Powell , D., et al. 2023, , 617, 483, 10.1038/s41586-023-05902-2

    2023 doi

  146. [155]

    P., Zingales , T., et al

    Tsiaras , A., Waldmann , I. P., Zingales , T., et al. 2018, The Astronomical Journal, 155, 156, 10.3847/1538-3881/aaaf75

    2018 doi

  147. [156]

    S., Tennyson , J., Yurchenko , S

    Underwood , D. S., Tennyson , J., Yurchenko , S. N., et al. 2016, , 459, 3890, 10.1093/mnras/stw849

    2016 doi

  148. [157]

    E., Marley , M

    Vahidinia , S., Moran , S. E., Marley , M. S., & Cuzzi , J. N. 2024, , 136, 084404, 10.1088/1538-3873/ad6cf2

    2024 doi

  149. [158]

    2020, , 634, A78, 10.1051/0004-6361/201936697

    Venot , O., Cavali \'e , T., Bounaceur , R., et al. 2020, , 634, A78, 10.1051/0004-6361/201936697

    2020 doi

  150. [159]

    2025, , 982, L38, 10.3847/2041-8213/adbd46

    Voyer , M., Changeat , Q., Lagage , P.-O., et al. 2025, , 982, L38, 10.3847/2041-8213/adbd46

    2025 doi

  151. [160]

    R., & Sing , D

    Wakeford , H. R., & Sing , D. K. 2015, , 573, A122, 10.1051/0004-6361/201424207

    2015 doi

  152. [161]

    J., Beatty , T

    Welbanks , L., Bell , T. J., Beatty , T. G., et al. 2024, , 630, 836, 10.1038/s41586-024-07514-w

    2024 doi

  153. [162]

    A., & Smith , P

    West , R. A., & Smith , P. H. 1991, , 90, 330, 10.1016/0019-1035(91)90113-8

    1991 doi

  154. [163]

    P., Pucci , A., & Trieloff , M

    Wetzel , S., Klevenz , M., Gail , H. P., Pucci , A., & Trieloff , M. 2013, , 553, A92, 10.1051/0004-6361/201220803

    2013 doi

  155. [164]

    C., Borucki, W

    Whitten, R. C., Borucki, W. J., O'brien, K., & Tripathi, S. N. 2008, Journal of Geophysical Research, 113. https://api.semanticscholar.org/CorpusID:53446710

    2008

  156. [165]

    H., et al

    Woitke , P., Helling , C., Hunter , G. H., et al. 2018, Astronomy & Astrophysics, 614, A1, 10.1051/0004-6361/201732193

    2018 doi

  157. [166]

    H., Changeat , Q., Edwards , B., et al

    Yip , K. H., Changeat , Q., Edwards , B., et al. 2021, The Astronomical Journal, 161, 4, 10.3847/1538-3881/abc179

    2021 doi

  158. [167]

    N., Amundsen, D

    Yurchenko, S. N., Amundsen, D. S., Tennyson, J., & Waldmann, I. P. 2017, A&A, 605, A95, 10.1051/0004-6361/201731026

    2017 doi

  159. [168]

    N., Mellor, T

    Yurchenko, S. N., Mellor, T. M., Freedman, R. S., & Tennyson, J. 2020, Monthly Notices of the Royal Astronomical Society, 496, 5282–5291, 10.1093/mnras/staa1874

    2020 doi

Pith tools

Reviewed August 7, 2026 · model on record in the stance chip above.