Global flow patterns and ionospheric convection in Jupiter's magnetosphere

Details Global flow patterns and ionospheric convection in Jupiter's magnetosphere Global flow patterns and ionospheric convection in Jupiter's magnetosphere

Apr 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003eaeja.....6812h&link_type=abstract

EGS - AGU - EUG Joint Assembly, Abstracts from the meeting held in Nice, France, 6 - 11 April 2003, abstract #6812

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Scientific paper

The size and configuration of Jupiter's magnetosphere is controlled by the ambient solar wind conditions, Jupiter's strong rotation and intrinsic magnetic field and the plasma sources internal to the magnetosphere. We will examine the relative importance of each of these factors using our 3D global magnetohydrodynamic (MHD) model of the Jovian magnetosphere. This model uses adaptive mesh refinement (AMR) to model the global Jovian system, including the mass loading region near Io's orbit. The inner boundary of the MHD model, at 3 R_J, is coupled to a height integrated ionospheric electric potential model. We will present results of the coupled model and show similarities and differences to other planetary magnetospheres. We will show that Jupiter's magnetosphere without mass loading and rotation is Earth-like in all but size. Adding rotation determines, to a large extent, the flow pattern in the magnetosphere. The addition of mass loading, although extremely important, does not change the character or topology of the magnetospheric convection but instead modifies the locations of magnetospheric features such as the bow shock, the magnetopause and the location of reconnection sites. In addition, we will show how features like the magnetospheric "wings" [Song, ASR, 2001] at the Earth are manifest and modified in the magnetosphere of Jupiter.

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