Changes of the energetic particle characteristics in the inner jovian magnetosphere and the relation to auroral features

Details Changes of the energetic particle characteristics in the inner jovian magnetosphere and the relation to auroral features Changes of the energetic particle characteristics in the inner jovian magnetosphere and the relation to auroral features

Apr 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003eaeja.....9357t&link_type=abstract

EGS - AGU - EUG Joint Assembly, Abstracts from the meeting held in Nice, France, 6 - 11 April 2003, abstract #9357

Computer Science

Scientific paper

Based on 33 Galileo passages through the inner part of the jovian magnetosphere the properties of the energetic charged particle population are investigated. Pronounced changes in the particle intensities, and in their energy and pitch angle distribution are generally observed. The good coverage in local time and radial distance provided by Galileo allowed to trace the location of the most distinct changes within the equatorial plane. Independent on local time they occur at distances between 10 R_J and 30 R_J. Within this region particle intensities drop by several orders of magnitude and the energy spectra softens considerably. However, most prominent is a change of the electron pitch angle distribution from a pancake or trapped to a bi-directional distribution with maxima close to 0^0 and 180^0. The change occurs rapidly, usually within the time resolution of the measurements, giving rise to a sharp and distinct boundary. This boundary is located dependent on the orbit between 10 and 17 R_J, and occurs in a region where the magnetic field topology is still close to a dipolar field configuration. In order to establish a relation to and implications for the jovian high-latitude aurora, the mentioned region was then mapped into the ionosphere of Jupiter, using the Khurana and the VIP4 model for the tracing of magnetic field lines. Estimation of the electron precipitation flux and a detailed comparison with HST observations suggest that the sharp pitch angle boundary is related to the transition between the belt of diffuse auroras and the main auroral oval of Jupiter.

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