a Search for the Physical Processes Responsible for the Jovian Equatorial Bulge: CYCLE4 Medium

Details a Search for the Physical Processes Responsible for the Jovian Equatorial Bulge: CYCLE4 Medium a Search for the Physical Processes Responsible for the Jovian Equatorial Bulge: CYCLE4 Medium

Jul 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994hst..prop.5417e&link_type=abstract

HST Proposal ID #5417

Other

Hst Proposal Id #5417 Solar System, Giant P

Scientific paper

A model to explain both the Lyman alpha bulge of Jupiter and the heating excess of the Jovian upper atmosphere has been recently proposed. This model, based on the Voyager UVS and the IUE data collected since 1978,describes how thermospheric winds that form near the northern and southern maximum activity regions of the Jovian auroral ovals, propagate along the planet surface, and collide near the Jovian equator at longitude system III equal to about 100 degrees. In this collision, a part of the energy is converted into random wave motions, and the remaining is transferred to two lateral jets. The random motions enhance the atomic H cross section explaining the excess observed for both the brightness and the width of the Ly-alpha line. On the other hand, the kinetic energy carried by the northern jets spreads over the whole planet surface as thermal energy, explaining the heating excess observed in the Jovian upper atmosphere. To check this model, we propose to make high resolution measurements of the H Ly-alpha lines and to compare their shapes and relative Doppler shifts both in the northern and the southern hemispheres at different lattudes and in the bulge region, in order to spatially follow the propagation of possible turbulent thermospheric motions.

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