Dayglow Emission Line Profiles from the Outer Planets CYCLE4-MED

Details Dayglow Emission Line Profiles from the Outer Planets CYCLE4-MED Dayglow Emission Line Profiles from the Outer Planets CYCLE4-MED

Jul 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994hst..prop.5414c&link_type=abstract

HST Proposal ID #5414

Physics

Hst Proposal Id #5414 Solar System Giant Planets

Scientific paper

Recent IUE observations of the H Ly alpha emission line profile from Jupiter's dayglow and aurora reveal a substantial line broadening, implying that the observed high brightness is due to resonant scattering of solar emission with a broad line rather than charged particle excitation. This may reflect highly energetic processes producing a 5-10 km/sec suprathermal population of H atoms in Jupiter's upper atmosphere, which in turn may be related to the unresolved question of the high exospheric temperatures of 400-1200 K detected on all 4 giant planets during the Voyager encounters. It is clear that if the bright H Ly alpha emissions from the outer planets are due mainly to resonant scattering of solar and interplanetary emissions, as observed on Jupiter and Saturn from long term correlations with the solar Ly alpha flux, then the lines from all 4 planets must be broad to explain the observed high albedos. The H Ly alpha lineshapes provide a discriminant between the processes of resonant scattering and charged particle excitation. We propose to obtain high signal to noise H Ly alpha line profile measurements from Saturn, Uranus, and Neptune to resolve the questions about the excitation processes for the bright airglow emissions. ALL SATURN OBSERVATIONS HAVE BEEN MOVED TO A NEW PROPOSAL.

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