Physics
Scientific paper
Dec 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufmsm31d..04k&link_type=abstract
American Geophysical Union, Fall Meeting 2009, abstract #SM31D-04
Physics
[2744] Magnetospheric Physics / Magnetotail, [2753] Magnetospheric Physics / Numerical Modeling, [2784] Magnetospheric Physics / Solar Wind/Magnetosphere Interactions, [6275] Planetary Sciences: Solar System Objects / Saturn
Scientific paper
Cassini has observed multiple plasmoids in Saturn’s magnetotail that are thought to be produced by substorm-like events. However, the single spacecraft measurements make it difficult to determine the location of a reconnection site as well as the speed and composition of plasmoid-like structures. Measurements by Cassini have determined that solar wind pressure modulations have a stronger effect on reconnection and the development of plasmoids than the orientation of the interplanetary magnetic field. In this paper we use a three-dimensional multi-fluid model to investigate whether substorm-like events are more likely to be influenced by an increase in solar wind pressure that is a result of increased solar wind density or by an increase in solar wind velocity. We demonstrate that initial conditions are very important with large scale plasmoids being associated with IMF turnings anti-parallel to the Kronian magnetosphere. Smaller scale and more frequent flux ropes are generated in the wake of the plasma and/or by increases in the solar wind dynamic pressure. The global nature of this model will enable the determination of the distance, Saturn Local Time, speeds and recurrence rate of any plasmoids. We also examine the three-dimensional movement and geometry of the plasma sheet - in particular its location relative to any plasmoids observed to form in the model and its dayside and nightside thicknesses.
Harnett Erika M.
Kidder A.
Winglee Robert
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