| Issue |
A&A
Volume 423, Number 1, August III 2004
|
|
|---|---|---|
| Page(s) | 391 - 395 | |
| Section | Planets and planetary systems | |
| DOI | https://doi.org/10.1051/0004-6361:20034532 | |
| Published online | 29 July 2004 | |
Modelling the Lyman 
dayglow in the Jovian atmosphere*
1
Laboratoire de Planétologie de Grenoble, CNRS-UJF, BP 53, 38041 Saint Martin d'Hères, Cedex 9, France e-mail: mathieu.barthelemy@ujf-grenoble.fr
2
MS 150-21, Caltech, Pasadena, California 91125, USA
3
MS 183-501, JPL, Pasadena, California 9110, USA e-mail: cdp@gps.caltech.edu
4
Observatoire de Paris-Meudon, 5 place Jules Jansen, 92195 Meudon, France e-mail: renee.prange@obspm.fr
Received:
17
October
2003
Accepted:
15
March
2004
The Lyman dayglow of Jupiter provides an important source of
information about its atmosphere. The H Lyman and the
H2 6–0 P(1) line of the Lyman system overlap, resulting in a coupling effect between these two lines. In this paper, we evaluate the effect of this overlapping via radiative transfer modelling and show its
effect both on the integrated intensity and the line profile. The intensity
increases at about 1025 Å at the centre of the disc, tends to slightly
decrease at the limb, and creates an asymmetry in the profile. This
asymmetry is also present in the jovian H-Lyman α bulge
region.
Key words: radiative transfer / planets and satellites: individual: Jupiter / ultraviolet: solar system
© ESO, 2004
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