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C. D. Parkinson, E. Griffioen, J. C. McConnell (Dept. of Earth and Atmospheric Science, York University, Canada), L. Ben Jaffel, A. Vidal-Madjar (Institut d'Astrophysique de Paris-CNRS, France), J. T. Clarke (Space Phyysics Research Laboratory, University of Michigan), G. R. Gladstone (Southwest Research Institute, San Antonio, Texas)
We have made calculations of the atomic D distribution in the thermosphere of Jupiter. The principal reactions determining the D abundance appear to be generation by reaction of H with vibrationally hot HD and loss by reaction of D with H2(v=0,1) and CH3. The H and CH3 distributions have been calculated using a 1-D photochemical-diffusion model with the column H constrained using the Lyman--\alpha airglow. For H2 effective vibrational temperatures, Tv, between 1 and 4 times kinetic we find D columns between 4\times 1011 and 2 \times 1013 atoms~cm-2. HD can be vibrationally excited due to VV energy transfer from H2(v=1). Using a radiative transfer model with coupling of the H and D Lyman--\alpha lines we have calculated line profiles and total intensities across the Jovian disk and on the limb. For the above D columns and a H column ~ 3.5 \times 1017,{\rm cm-2} --compatible with equatorial Lyman--\alpha airglow observations--, the disk D intensity varies from 80 to 600~R for overhead Sun and viewing, whereas on the terminator the D maximum total intensity is ~~60~R at ~~860~km above the 1 bar level for the maximum D column.