Jupiter's H LY Alpha Auroral/airglow Line Profile: Cycle 3 Medium

Details Jupiter's H LY Alpha Auroral/airglow Line Profile: Cycle 3 Medium Jupiter's H LY Alpha Auroral/airglow Line Profile: Cycle 3 Medium

Jul 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993hst..prop.4601c&link_type=abstract

HST Proposal ID #4601

Physics

Hst Proposal Id #4601

Scientific paper

In a series of IUE observations with 0.14 Angstrom resolution we have resolved the width of the H Ly alpha emission line from Jupiter's aurora and dayglow. The initial motivation was to detect the signature of proton aurora in Jupiter's hydrogen atmosphere, i.e. highly Doppler- shifted Ly alpha emission from fast proton charge exchange. No proton aurora have been observed on Jupiter, with a tight upper limit, but the auroral Ly alpha line does appear broadened with an asymmetry toward the blue (upward moving) side. Although this was initially interpreted in terms of fast protons accelerated by auroral potentials, it is also possible that it represents a supersonic thermospheric wind. Equatorial data on Jupiter have shown that the observed brightening, or "bulge", is due to a symmetric broadening of the line rather than a bright core (as expected for electron collisional excitation). This appears more consistent with a superthermal population in the upper atmosphere than particle excitation, and suggests that the auroral broadening may be a related process. We can in principle identify an auroral thermospheric expansion away from the auroral oval by spatially resolved spectra at points on either side of the auroral oval, and we propose to do this in cycle 3. We will then relate the auroral observations to scheduled equatorial observations in cycle 2.

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