Computer Science – Sound
Scientific paper
Sep 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002dps....34.1814d&link_type=abstract
American Astronomical Society, DPS Meeting #34, #18.14; Bulletin of the American Astronomical Society, Vol. 34, p.875
Computer Science
Sound
Scientific paper
Cassini/VIMS observations during the Jupiter encounter between December 2000 and January 2001 give the first opportunity to study phase angle variations of H3+ emission at 3.5 μ m, together with fluorescence CH4 emission at a high level of sensitivity. Spectral images with long integration time (640 ms) are used, for maximum sensitivity. The spectrum of Jupiter in the 3.3-3.6 μ m range exhibits H3+ thermal emission and CH4 emission, interpreted as due to fluorescence of solar light (Drossart et al., ESA-SP427 1999). Synthetic spectra confirms this later detection, first seen on ISO/SWS at a global scale on the disk, and reproduces the P/Q/R branches of the ν 3 band of CH4. Limb profiles of the CH4 emission are obtained for various phase angles, between 0 and 70 dg, which give a new constraint on the mesospheric sounding. On the other hand, limb profiles of H3+ thermal emission are consistent with a H3+ density controlled by the solar flux, confirming the solar control on the H3+ density in equatorial and mid latitude regions, in contrast with high latitude auroral emissions.
Baines Kevin Hays
Bellucci Giancarlo
Bibring Jean-Pierre
Brown Harvey R.
Buratti Bonnie Jean
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