Modeling The Atmosphere Of The Transiting Super-earth GJ 1214b

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GJ 1214b is the first transiting super-Earth that requires a significant atmosphere to explain its observed mass and radius. Two classes of models have been proposed to explain the planet's observed low density. One requires a rocky inner core with a significant hydrogen-helium atmosphere. The other is a "water world" scenario where the bulk of the planet would be composed primarily of water. Such a planet would be enshrouded by a thick water vapor atmosphere. Breaking the degeneracy between these two classes of models requires observing the planet's atmosphere to identify the key differences between a mostly hydrogen atmosphere and a water atmosphere. Our modeling effort reveals that transit (transmission) spectroscopy should be the most straightforward way of affirming the composition of GJ 1214b's atmosphere. Furthermore, the signature of a hydrogen-dominated atmosphere on GJ 1214b should be quite large -- on the order of 0.1-0.3% relative to its host star -- and readily observable with current ground-based and space-based instrumentation. The presence of clouds or hazes in the planet's atmosphere could further complicate the interpretation of transmission spectra for GJ 1214b. We find that some chemical species may condense to form clouds in the atmosphere of GJ 1214b. We have additionally applied a photochemical model to this planet, and we find that hydrocarbon hazes may readily form in GJ 1214b's atmosphere.

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