O+ at Titan's Exobase from a Hybrid Simulation

Details O+ at Titan's Exobase from a Hybrid Simulation O+ at Titan's Exobase from a Hybrid Simulation

May 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agusm.p41b..10s&link_type=abstract

American Geophysical Union, Spring Meeting 2007, abstract #P41B-10

Physics

6026 Ionospheres (2459), 6033 Magnetospheres (2756), 6281 Titan, 7827 Kinetic And Mhd Theory

Scientific paper

Titan's extensive atmosphere and exosphere interact with Saturn's rotating magnetospheric flow. We have studied this interaction with an advanced hybrid simulation model and present results for both the general characteristics of the interaction and the behavior of the O+ flow ions near the exobase for the conditions during the Voyager 1 flyby. Our model, that employs improved resolution and a realistic ion composition in the upstream flow (O+ and H+), shows that the ionotail and the magnetotail bend in a direction opposite to the convection electric field. We also present a simulated impact map for the oxygen ions of the flow with total O+ precipitation rate 1.3 · 1024, s-1 onto Titan's exobase. Although this rate indicates that the plasma conditions above the exobase do not inhibit O+ precipitation on the exobase, the direction of the O+ flow, however, is shown to turn drastically near the exobase. However, the light flow ions (H+) are effectively deflected by the magnetic barrier formed around Titan.

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