Modeling the precipitation flux in the Jovian auroral zones. I - The model and its application to the UV auroral emissions

Details Modeling the precipitation flux in the Jovian auroral zones. I - The model and its application to the UV auroral emissions Modeling the precipitation flux in the Jovian auroral zones. I - The model and its application to the UV auroral emissions

Dec 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991jgr....9621371p&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 96, Dec. 1, 1991, p. 21,371-21,389. Research supported by INSU.

Physics

27

Auroral Zones, Charged Particles, Jupiter Atmosphere, Particle Energy, Particle Precipitation, Iue, Planetary Magnetic Fields, Planetary Magnetospheres, Spatial Resolution

Scientific paper

The atmospheric auroral features of EUV Jovian auroral emission observed by the IUE observatory and the Voyager UV spectrometer are interpreted using a model of precipitation for particles azimuthally drifting in the Jovian magnetic field. The model computes the precipitating flux along constant L shells for particles drifting in the asymmetrical magnetic field. It is shown that the effect of the magnetic field asymmetry by itself is able to account for the main longitudinal features of the observed emissions through the loss cone variations. The dependence of the predicted precipitation flux profiles on the model parameters was obtained. By a comparison with observations, it was found that the bulk of the emissions is due to quasi-isotropic equatorial distributions in the loss cone; it depends only slightly on the L shell parameter and does not depend on the particle species. This implies that the auroral brightness observations alone cannot provide enough information on this main component of magnetospheric losses.

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