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T. Majeed (U. Michigan), R. V. Yelle, J. H. Waite (U. Arizona), G. R. Gladstone (SwRI), J. C. McConnell (York U., Canada)
Fluorescence of H2 Lyman and Werner bands has been proven to be an important process in explaining the observations of Jupiter's dayglow (both in terms of brightness and spectral shape), and has also been interpreted as an important source of vibrationally excited H2(v) molecules in their ground electronic state. The distribution of sufficiently abundant H2(v>3) molecules at the thermospheric heights may have a substantial impact on the ionospheric electron densities. Fluorescence in the Lyman and Werner bands can be induced by either solar EUV photon or photoelectron. Regardless of the relative importance of these sources, the H2 band emission at non-auroral latitudes requires a detailed radiative transfer calculation. We have recently modified our thermospheric-ionospheric codes to perform more realistic calculations of density distribution of each of the 14 vibrationally excited levels of H2 molecules self-consistently with the jovian ionospheric electron and ion densities. We incorporated high-resolution solar EUV fluxes (between 850A and 1150A), measured with the SUMER instrument on-board SOHO, and updated molecular data on H2. However, photoelectron fluxes from a recently modified two-stream code were used. The calculated H2 emission spectra were compared with recently observed high-resolution jovian dayglow spectra. The calculated electron density profiles were compared with those inferred from the analysis of the Galileo RSS data. Details of the results will be presented.
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Bulletin of the American Astronomical Society, 35 #4
© 2003. The American Astronomical Soceity.