Authors

H. Menager (1), M. Barthélemy (1), C. D. Parkinson (2), J. Lilensten (1)

Affiliations

(1) Laboratoire de Planétologie de Grenoble, France (2) University of Michigan, MI, USA

Abstract

To date, there have been no unambiguous detection of FUV emissions from the atmosphere of a hot Jupiter. In the absence of any precise computation, it is generally agreed that the contrast of the planetary emissions with the parent star FUV emissions are not very favorable to this detection. We propose to estimate these emissions by a) using a kinetic code to model the absorption of the stellar flux and the transport of superthermal electrons to obtain a model atmosphere of a hot Jupiter followed by b) performing radiative transfer calculations using this model atmosphere to calculate the intensity of the H Lyman-α line and H2 bands between 900 and 1650 Å. The kinetic code provides excitation rates of H and H2 and we calculate both the dayglow and the auroral emissions. These calculations are carried out for various hot Jupiter model atmospheres, computed by making parameter perturbations around an arbitrary initial reference model. This investigation should give conditions which yield the best conditions for detection of FUV emissions from a hot Jupiter.