Morphology of the magnetic field near Titan: Hybrid model study of the Cassini T9 flyby

Details Morphology of the magnetic field near Titan: Hybrid model study of the Cassini T9 flyby Morphology of the magnetic field near Titan: Hybrid model study of the Cassini T9 flyby

Oct 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007georl..3424s09k&link_type=abstract

Geophysical Research Letters, Volume 34, Issue 24, CiteID L24S09

Physics

8

Planetary Sciences: Solar System Objects: Titan, Magnetospheric Physics: Planetary Magnetospheres (5443, 5737, 6033), Magnetospheric Physics: Numerical Modeling, Magnetospheric Physics: Solar Wind Interactions With Unmagnetized Bodies, Ionosphere: Planetary Ionospheres (5435, 5729, 6026)

Scientific paper

We study the deformation and morphology of the magnetic field near Titan by a three-dimensional numerical quasi-neutral hybrid model (HYB-Titan). We analyze two runs, one in which the sub-rotating plasma consists of oxygen (O+) ions and protons (H+) and another with only protons. We find that both cases result in the generation of Alfvén wing-like flux tubes. In comparison with the proton-only case, the direction and magnitude of the magnetic field in the oxygen-rich flow case are in better agreement with Cassini magnetic field observations during its Titan T9 flyby on Dec. 26, 2006, suggesting that the sub-rotating plasma contained heavy ions. The oxygen-rich run also supports the hypotheses that (1) the sub-rotating flow direction was offset by ~30°-40° from the ideal rotating flow direction and that (2) the spacecraft was magnetically connected to the sunlit side of near-Titan space in the tail when it approached Titan on the T9 flyby.

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