Evidence for disequilibrium chemistry from vertical mixing in hot Jupiter atmospheres. A comprehensive survey of transiting close-in gas giant exoplanets with warm-Spitzer/IRAC

C. Baxter; J-M. Désert; S-M. Tsai; K. O. Todorov; J. L. Bean; D. Deming; V. Parmentier; J. J. Fortney; M. Line; D. Thorngren; R. T. Pierrehumbert; A. Burrows; A. P. Showman

doi:10.1051/0004-6361/202039708

arXiv · 2103.07185

Evidence for disequilibrium chemistry from vertical mixing in hot Jupiter atmospheres. A comprehensive survey of transiting close-in gas giant exoplanets with warm-Spitzer/IRAC

C. Baxter·J-M. Désert·S-M. Tsai·K. O. Todorov·J. L. Bean·D. Deming·V. Parmentier·J. J. Fortney·M. Line·D. Thorngren·R. T. Pierrehumbert·A. Burrows·A. P. Showman

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Abstract

[Abridged] Aims. We present a large atmospheric study of 49 gas giant exoplanets using infrared transmission photometry with Spitzer/IRAC at 3.6 and 4.5um. Methods. We uniformly analyze 70 photometric light curves of 33 transiting planets using our custom pipeline, which implements pixel level decorrelation. We use this survey to understand how infrared photometry traces changes in atmospheric chemical properties as a function of planetary temperature. We compare our measurements to a grid of 1D radiative-convective equilibrium forward atmospheric models which include disequilibrium chemistry. We explore various strengths of vertical mixing (Kzz = 0 - 10^12 cm2/s) as well as two chemical compositions (1x and 30x solar). Results. We find that, on average, Spitzer probes a difference of 0.5 atmospheric scale heights between 3.6 and 4.5um, which is measured at 7.5sigma level of significance. We find that the coolest planets show a lack of methane compared to expectations, which has also been reported by previous studies of individual objects. We show that the sample of coolest planets rule out 1x solar composition with >3sigma confidence while supporting low vertical mixing (Kzz = 10^8 cm2/s). On the other hand, we find that the hot planets are best explained by models with 1x solar metallicity and high vertical mixing (Kzz = 10^12 cm2/s). We interpret this as the lofting of CH4 to the upper atmospheric layers. Changing the interior temperature changes the expectation for equilibrium chemistry in deep layers, hence the expectation of disequilibrium chemistry higher up. We also find a significant scatter in the transmission signatures of the mid-temperate and ultra-hot planets, likely due to increased atmospheric diversity, without the need to invoke higher metallicities. Additionally, we compare Spitzer transmission with emission for the same planets and find no evidence for correlation.

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C. Baxter, J-M. Désert, S-M. Tsai, K. O. Todorov, J. L. Bean, D. Deming, V. Parmentier, J. J. Fortney, M. Line, D. Thorngren, R. T. Pierrehumbert, A. Burrows, A. P. Showman. 2021-03-12. Evidence for disequilibrium chemistry from vertical mixing in hot Jupiter atmospheres. A comprehensive survey of transiting close-in gas giant exoplanets with warm-Spitzer/IRAC. https://doi.org/10.1051/0004-6361/202039708

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