Julianne I. Moses

TL;DR: In this paper, a one-dimensional photochemical and thermochemical kinetics and diffusion model was developed to study the effects of disequilibrium chemistry on the atmospheric composition of hot-Jupiter exoplanets.

TL;DR: In this paper, a 1-D photochemical and thermochemical kinetics and diffusion model was developed for transiting exoplanets HD 189733b and HD 209458b to study the effects of disequilibrium chemistry on the atmospheric composition of hot Jupiters.

TL;DR: In this paper, a diurnally averaged model that couples hydrocarbon and oxygen photochemistry, molecular and eddy diffusion, radiative transfer, and condensation was developed to investigate the details of hydrocarbon photochemistry on Saturn, and the model results are compared with observations from the Infrared Space Observatory (ISO) to place tighter constraints on molecular abundances, to better define Saturn's eddy coefficient profile, and to identify important chemical schemes that control the abundances of the observable hydrocarbons in Saturn's upper atmosphere.

TL;DR: The results of these models are compared with secondary-eclipse photometric data from the Spitzer Space Telescope and conclude that disequilibrium models with C/O ~ 1 are consistent with spectra of WASP-12b, XO-1b, and CoRoT-2b, confirming the possible carbon-rich nature of these planets.

TL;DR: The predicted equilibrium and disequilibrium chemistry of generic hot Neptunes is explored and it is concluded that although the spectral fit from the high-metallicity forward models is not quite as good as the best fit obtained from pure retrieval methods, the atmospheric composition predicted is more physically and chemically plausible in terms of the relative abundance of major constituents.