Physics
Scientific paper
Dec 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsm23d..02s&link_type=abstract
American Geophysical Union, Fall Meeting 2011, abstract #SM23D-02
Physics
[2732] Magnetospheric Physics / Magnetosphere Interactions With Satellites And Rings, [2753] Magnetospheric Physics / Numerical Modeling, [6275] Planetary Sciences: Solar System Objects / Saturn, [6281] Planetary Sciences: Solar System Objects / Titan
Scientific paper
We analyze how the dynamics of Saturn's dayside magnetosphere affect Titan's plasma interaction with a three-dimensional multifluid/multiscale model of Titan embedded in a global model of Saturn's magnetosphere. The characteristics of Titan's environment at 09:00 Saturn local time (SLT) were studied for three cases: a stationary magnetopause, an inward moving magnetopause, and an outward moving magnetopause. The results show that the plasma and magnetic field upstream of Titan vary on short and long time scales. Rotating cold, interchange fingers cause rapid changes in the plasma velocity, density, and composition, while gradual changes are due to the relatively slow compression and expansion of Saturn's magnetopause. We find that Titan can enter the boundary layer on the inside of the magnetopause, which is characterized by shearing flows and a mix of magnetospheric and magnetosheath plasma. The irregular flows in the boundary layer strongly modify Titan's induced magnetosphere. We also examine how Titan's induced magnetosphere and ion tail are affected when Titan crosses Saturn's magnetopause at 13.6 Saturn local time (SLT). During the simulation Titan crosses Saturn's magnetopause twice, exiting and reentering the magnetosphere. Inside Saturn's magnetosheath, Titan's connection to Saturn's magnetic field lines is removed by slow ionospheric convection in ˜1.8 hours and, after Titan crosses back into the magnetosphere, Titan's connection to magnetosheath field lines is removed through ionospheric convection in ˜50 minutes. We also use the two simulations to investigate how Titan may affect the dynamics of Saturn's magnetopause and find that Titan's ion tail may be able to prevent the magnetopause from moving inward and crossing Titan when Titan is in the pre-noon sector. The results of the simulations are compared to data from Cassini's TA and T32 flybys and to the observed variability at Titan's orbital radius.
Kidder A.
Snowden D. S.
Winglee Robert
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