Astronomy and Astrophysics – Astrophysics
Scientific paper
2002-08-13
Astrophys.J. 589 (2003) 615-622
Astronomy and Astrophysics
Astrophysics
15 pages, 9 figures -- Accepted to The Astrophysical Journal -- The paper is significantly revised and expanded
Scientific paper
10.1086/374387
Using a self-consistent atmosphere code, we construct a new model of the atmosphere of the transiting extrasolar giant planet HD 209458b to investigate the disparity between the observed strength of the sodium absorption feature at 589 nm and the predictions of previous models. For the atmospheric temperature-pressure profile we derive, silicate and iron clouds reside at a pressure of several mbar in the planet's atmosphere. These clouds have significant vertical extent and optical depth due to our slant viewing geometry and lead to increased absorption in bands directly adjacent to the sodium line core. Using a non-LTE sodium ionization model that includes photoionization by stellar UV flux, collisional processes with H_2, and radiative recombination, we show that the ionization depth in the planet's atmosphere reaches ~1/2 mbar at the day/night terminator. Ionization leads to a slight weakening of the sodium feature. We present our baseline model, including ionization and clouds, which falls near the observational error bars. The sensitivity of our conclusions to the derived atmospheric temperature-pressure profile is discussed.
Burrows Adam
Cooper Curtis S.
Fortney Jonathan J.
Hubbard William B.
Hubeny Ivan
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