Global Magnetohydrodynamic Simulation of a Steady Magnetospheric Convection event

Details Global Magnetohydrodynamic Simulation of a Steady Magnetospheric Convection event Global Magnetohydrodynamic Simulation of a Steady Magnetospheric Convection event

May 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm..sm32a08e&link_type=abstract

American Geophysical Union, Spring Meeting 2001, abstract #SM32A-08

Physics

2740 Magnetospheric Configuration And Dynamics, 2744 Magnetotail, 2784 Solar Wind/Magnetosphere Interactions

Scientific paper

We performed an MHD simulation of a steady magnetospheric (SMC) event observed on February 3, 1998. We used observations from the Wind spacecraft to provide solar wind and interplanetary magnetic field (IMF) input for our simulation. Both the solar wind density (< 5 cm-3) and flow velocity (< 350 km/s) were below average during this interval. During the first two hours (from 1300 to 1500 UT) the IMF was northward and the ionospheric potential difference was small (~40 kV). After the southward IMF arrived at 1406 UT the potential increased substantially to > 100 kV and both the magnitude and shape of the potential pattern remained steady for the next seven hours. This implies that the amount of magnetic energy transported from the dayside to the nightside magnetosphere was balanced by the loss of magnetic energy due to magnetotail reconnection. We will determine the total ionospheric current and the amount of power deposited into the ionosphere to understand energy transport during SMC. We will also investigate the magnetic field configuration and plasma distribution associated with steady convection.

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