Journal
ASTROPHYSICAL JOURNAL
Volume 717, Issue 1, Pages 496-502Publisher
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/717/1/496
Keywords
atmospheric effects; methods: numerical; planetary systems; planets and satellites: atmospheres; stars: individual (HD 189733b); radiative transfer
Categories
Funding
- JPL Graduate Fellowship (JPLGF)
- NSC [98-2111-M-001-014-MY3]
- NASA [NX09AB72G]
Ask authors/readers for more resources
Recent infrared spectroscopy of hot exoplanets is beginning to reveal their atmospheric composition. Deep within the planetary atmosphere, the composition is controlled by thermochemical equilibrium. Photochemistry becomes important higher in the atmosphere, at levels above similar to 1 bar. These two chemistries compete between similar to 1 and 10 bars in hot-Jupiter-like atmospheres, depending on the strength of the eddy mixing and temperature. HD 189733b provides an excellent laboratory in which to study the consequences of chemistry of hot atmospheres. The recent spectra of HD 189733b contain signatures of CH4, CO2, CO, and H2O. Here we identify the primary chemical pathways that govern the abundances of CH4, CO2 , CO, and H2O in the cases of thermochemical equilibrium chemistry, photochemistry, and their combination. Our results suggest that the disequilibrium mechanisms can significantly enhance the abundances of these species above their thermochemical equilibrium value, so some caution must be taken when assuming that an atmosphere is in strict thermochemical equilibrium.
Authors
I am an author on this paper
Click your name to claim this paper and add it to your profile.
Reviews
Recommended
No Data Available