Multi-Fluid Simulations of the Jovian Magnetotail under Varying IMF Conditions

Details Multi-Fluid Simulations of the Jovian Magnetotail under Varying IMF Conditions Multi-Fluid Simulations of the Jovian Magnetotail under Varying IMF Conditions

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agufmsm44a..08w&link_type=abstract

American Geophysical Union, Fall Meeting 2007, abstract #SM44A-08

Physics

2740 Magnetospheric Configuration And Dynamics, 2753 Numerical Modeling, 5737 Magnetospheres (2756)

Scientific paper

The New Horizons spacecraft observed large cohesive density structures at great lengths down the Jovian magnetotail. Multi-fluid simulations that separately track the solar wind protons and heavy ions from the Galilean moons are used to investigate potential processes that can lead to such enhanced density structures. There are different dynamical regimes to consider. First, the inner magnetosphere is strongly rotationally driven. In the outer magnetosphere, the system can be subjected to torques from changes in the interplanetary magnetic field (IMF). For example, the IMF at 5 AU is largely tangential and the dominant y-component of the IMF can lead to local time asymmetries of the plasma sheet. Rotation of this IMF component can produce additional stresses on the plasma sheet that can lead to modified plasma flows down the tail. These processes as seen through the densities and energization of different ion species from the inner magnetosphere into the distant tail are discussed.

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