Volume 565, May 2014
|Number of page(s)||14|
|Section||Planets and planetary systems|
|Published online||20 May 2014|
Modeling magnesium escape from HD 209458b atmosphere
1 CNRS, UMR 7095, Institut d’Astrophysique de Paris, 98bis boulevard Arago, 75014 Paris, France
2 UPMC Univ. Paris 6, UMR 7095, Institut d’Astrophysique de Paris, 98bis boulevard Arago, 75014 Paris, France
Received: 15 November 2013
Accepted: 18 March 2014
Transit observations in the Mg i line of HD 209458b revealed signatures of neutral magnesium escaping the upper atmosphere of the planet, while no atmospheric absorption was found in the Mg ii doublet. Here we present a 3D particle model of the dynamics of neutral and ionized magnesium populations, coupled with an analytical modeling of the atmosphere below the exobase. Theoretical Mg i absorption line profiles are directly compared with the absorption observed in the blue wing of the line during the planet transit. Observations are well-fitted with an escape rate of neutral magnesium ṀMg0 = 2.9 -0.9+0.5× 107 g s-1, an exobase close to the Roche lobe (Rexo = 3 -0.9+1.3 Rp , where Rp is the planet radius) and a planetary wind velocity at the exobase vpl − wind = 25 km s-1. The observed velocities of the planet-escaping magnesium up to −60 km s-1 are well explained by radiation pressure acceleration, provided that UV-photoionization be compensated for by electron recombination up to ~ 13 Rp. If the exobase properties are constrained to values given by theoretical models of the deeper atmosphere (Rexo = 2 Rp and vpl − wind = 10 km s-1), the best fit to the observations is found at a similar electron density and escape rate within 2σ. In all cases, the mean temperature of the atmosphere below the exobase must be higher than ~6100 K. Simulations predict a redward expansion of the absorption profile from the beginning to the end of the transit. The spatial and spectral structure of the extended atmosphere is the result of complex interactions between radiation pressure, planetary gravity, and self-shielding, and can be probed through the analysis of transit absorption profiles in the Mg i line.
Key words: planets and satellites: atmospheres / stars: individual: HD 209458 / methods: numerical
© ESO, 2014
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