Atmospheres, Climate, Weather

Signature of Vertical Mixing in Hydrogen-dominated Exoplanet Atmospheres

By Keith Cowing
Status Report
astro-ph.EP
October 17, 2024
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Signature of Vertical Mixing in Hydrogen-dominated Exoplanet Atmospheres
The transit depth excess due to vertical mixing in the exoplanet atmosphere from our 1D chemical kinetics model run (Tequi = 500 βˆ’ 2000 K; Tint = 150, 250, 350, 450 and 550 K; log10(Kzz) = 9; surface gravity = 1000 cm sβˆ’2 ). The color contours from blue to red in panels (a) – (e) represent the transit depth excess due to CH4 and panels (f) – (j) due to NH3 . The white to black colormesh plot in all the panels represent the total transit depth excess. — astro-ph.EP

Vertical mixing is a crucial disequilibrium process in exoplanet atmospheres, significantly impacting chemical abundance and observed spectra. While current state-of-the-art observations have detected its signatures, the effect of vertical mixing on atmospheric spectra varies widely based on planetary parameters.

In this study, we explore the influence of disequilibrium chemistry across a parameter space that includes eddy diffusion, surface gravity, internal and equilibrium temperature, and metallicity. We also assess the effectiveness of retrieval models in constraining the eddy diffusion coefficient. By running numerous 1D chemical kinetics models, we investigate the impact of vertical mixing on the transmission spectrum.

We also built a custom fast-forward disequilibrium model, which includes vertical mixing using the quenching approximation and calculates the model abundance orders of magnitude faster than the chemical kinetics model. We coupled this forward model with an open source atmospheric retrieval code and used it on the JWST simulated output data of our chemical kinetics model and retrieved eddy diffusion coefficient, internal temperature and atmospheric metallicity.

We find that there is a narrow region in the parameters space in which vertical mixing has a large effect on the atmospheric transmission spectrum. In this region of the parameter space, the retrieval model can put high constraints on the transport strength and provide optimal exoplanets to study vertical mixing. Also, the NH3 abundance can be used to constrain the internal temperature for equilibrium temperature T_equi > 1400 K.

Vikas Soni, Kinsuk Acharyya

Comments: 28 pages, 12 figures, 5 table, accepted for publication in the Astrophysical Journal
Subjects: Earth and Planetary Astrophysics (astro-ph.EP)
Cite as: arXiv:2410.12737 [astro-ph.EP] (or arXiv:2410.12737v1 [astro-ph.EP] for this version)
https://doi.org/10.48550/arXiv.2410.12737
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Submission history
From: Vikas Soni
[v1] Wed, 16 Oct 2024 16:55:59 UTC (18,065 KB)
https://arxiv.org/abs/2410.12737

Astrobiology,

Explorers Club Fellow, ex-NASA Space Station Payload manager/space biologist, Away Teams, Journalist, Lapsed climber, Synaesthete, Na’Vi-Jedi-Freman-Buddhist-mix, ASL, Devon Island and Everest Base Camp veteran, (he/him) πŸ––πŸ»