Modeling of HST Observations of O I Emissions of Io in Eclipse

Details Modeling of HST Observations of O I Emissions of Io in Eclipse Modeling of HST Observations of O I Emissions of Io in Eclipse

Jul 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002hst..prop.9535g&link_type=abstract

HST Proposal ID #9535

Computer Science

Hst Proposal Id #9535 Solar System

Scientific paper

Observations by Trauger et al with WFPC2 in May 1997 of several bright regions of O I 630nm emission from Io in eclipse, and lack of ionized S II emission, may be interpreted to yield information about how Io interacts with the Jovian magnetosphere. A patchy corona was seen along the limb at high altitude which was generally brighter on the side of Io facing the plasma stream. It also tended to be brighter in the plasma wake region near 340^o long., +20^o lat.. Yet these observations remain to be fully examined in terms of impingement of plasma from the Jovian torus on volcanic plumes and a sublimation atmosphere. We have recently been developing the ability to simulate the interaction of plasma particles with Io's neutral SO_2 atmosphere. We have integrated our Monte Carlo flow field modeling with a line-by-line radiation code so we can determine radiation and absorption spectra along any line of sight. We propose to utilize our existing computer code to sum together separate volcanic and sublimation solutions for the atmosphere at the time of the 1997 observations. Into such a 3D steady-state instantaneous flow field we can project a plasma stream bombardment to model the O I and S II emission using the recently developed ``overlay'' approach to model absolute surface brightness and spatial distribution from minor species. The proposed work is a collaboration between one of the original observers and modellers.

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