Solar Wind-Magnetosphere Interaction as Simulated by a 3-D EM Particle Code

Details Solar Wind-Magnetosphere Interaction as Simulated by a 3-D EM Particle Code Solar Wind-Magnetosphere Interaction as Simulated by a 3-D EM Particle Code

May 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995ap%26ss.227..265n&link_type=abstract

Astrophysics and Space Science, Volume 227, Issue 1-2, pp. 265-276

Astronomy and Astrophysics

Astrophysics

8

Solar Wind, Magnetosphere, Imf, Magnetic Reconnection

Scientific paper

We have studied the solar wind-magnetosphere interaction using a 3-D electromagnetic particle code. The results for an unmagnetized solar wind plasma streaming past a dipole magnetic field show the formation of a magnetopause and a magnetotail, the penetration of energetic particles into cusps and radiation belt and dawn-dusk asymmetries. The effects of interplanetary magnetic field (IMF) have been investigated in a similar way as done by MHD simulations. The simulation results with a southward IMF show the shrunk magnetosphere with great particle entry into the cusps and nightside magnetosphere. This is a signature of a magnetic reconnection at the dayside magnetopause. After a quasi-stable state is established with an unmagnetized solar wind we switched on a solar wind with an northward IMF. In this case the significant changes take place in the magnetotail. The waving motion was seen in the magnetotail and its length was shortened. This phenomena are consistent with the reconnections which occur at the high latitude magnetopause. In our simulations kinetic effects will determine the self-consistent anomalous resistivity in the magnetopause that causes reconnections.

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