MHD Simulation of the Solar Wind-Magnetosphere Interaction on Magnetospheric Storms for Extreme Conditions

Details MHD Simulation of the Solar Wind-Magnetosphere Interaction on Magnetospheric Storms for Extreme Conditions MHD Simulation of the Solar Wind-Magnetosphere Interaction on Magnetospheric Storms for Extreme Conditions

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufmsm31a0294o&link_type=abstract

American Geophysical Union, Fall Meeting 2006, abstract #SM31A-0294

Physics

2700 Magnetospheric Physics (6939), 2723 Magnetic Reconnection (7526, 7835), 2724 Magnetopause And Boundary Layers, 2740 Magnetospheric Configuration And Dynamics, 2753 Numerical Modeling

Scientific paper

There are typical two kinds of interplanetary disturbances in the solar wind, which are called as ICME (Interplanetary Coronal Mass Ejection) and CIR (Corotating Interaction Region). Generally the former is frequently associated with occurrences of magnetospheric storms and the latter does not usually induce large magnetospheric storms but has often big chance of generation of high energy particles in the radiation belts. Thus it becomes important to simulate responses of the earth's magnetosphere by ICME and CIR to compare the effects. A three-dimensional global MHD simulation of the interaction between the solar wind and the earth's magnetosphere has been executed to study the magnetospheric storms for extreme conditions of the solar wind and IMF. The addition of the Bx component to the IMF creates dawn-dusk and north-south asymmetry to the dayside magnetic reconnection. Reconnected open field lines on the dusk side become relatively straight. They increase the lobe magnetic pressure and compress the plasma sheet. Open field lines on the dawn side are bent sharply and decrease the lobe magnetic pressure. As a result tail reconnection occurs preferably on the dusk side. This tendency is enhanced when the IMF is large and the solar wind Alfven Mach number becomes lower. In such a case, magnetic reconnection frequently occurs in an intermittent and patchy manner. Thus a turbulent structure can be formed in the plasma sheet. The dawn-dusk and north- south asymmetries cause an inclined plasma sheet, rotation of the magnetotail and asymmetric plasma flows in the tail. We demonstrate how reconnection and convection electric fields can be separated in the complicated configuration, and also we present what peculiar magnetospheric configuration is formed for extreme solar wind and IMF conditions.

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