@article{oai:nagoya.repo.nii.ac.jp:00020130,
 author = {Ogino, Tatsuki and Walker, Raymond J. and Ashour-Abdalla, Maha},
 journal = {Proceedings of the Research Institute of Atmospherics, Nagoya University},
 month = {Mar},
 note = {The dependence of the magnetospheric configuration and polar cap structure on the north-south component of the interplanetary magnetic field (IMF) has been modeled by performing a three-dimensional time-dependent magnetohydrodynamlc (MHD) simulation of the interaction between the solar wind and the earth's magnetosphere. When a uniform southward IMF (Bz=-5nT) is initially imposed throughout the system, magnetic neutral lines are formed in the subsolar and midnight tail regions on the equator. The magnetic field lines are dipolar near the earth and very concave in the magnetotail. The plasma convection is antisunward near the noon-midnight meridian and the plasma sheet becomes extremely thin. When the southward IMF begins to flow into the simulation box with the solar wind it takes more than about 40 minutes until tall magnetic reconnectlon begins. For no IMF, the dayside magnetic reconnection stops. When a uniform northward IMF (Bz=5nT) is initially imposed throughout the system, the plasma sheet thickens in a small region near the noon-midnight meridian and extends into the tail lobes. When viewed from the polar cap, this appears as a narrow finger of closed field lines extending into the polar cap. The plasma sheet extension becomes less pronounced when the northward IMF begins to enter the simulation box with the solar wind. For both cases the convection near the noon-midnight meridian is sunward, and field aligned currents of the region 1 type appear on both sides of the plasma sheet extension. When the IMF is southward, the polar cap expands until it reaches 65° latitude at midnight while it shrinks to 80° for northward IMF.},
 pages = {1--23},
 title = {A COMPUTER MODEL OF THE EARTH'S MAGNETOSPHERE},
 volume = {35},
 year = {1988}
}