The structure of the distanct geomagnetic tail during long periods of northward IMF

Details The structure of the distanct geomagnetic tail during long periods of northward IMF The structure of the distanct geomagnetic tail during long periods of northward IMF

Feb 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995georl..22..349r&link_type=abstract

Geophysical Research Letters (ISSN 0094-8276), vol. 22, no. 4, p. 349-352

Physics

94

Earth Ionosphere, Earth Magnetosphere, Geomagnetic Tail, Interplanetary Magnetic Fields, Magnetohydrodynamics, Mathematical Models, Solar Wind, Atmospheric Models, Boundary Layers, Computerized Simulation, Field Aligned Currents

Scientific paper

We have used a newly developed, parallelized, global MHD magnetosphere - ionosphere simulation model with a 400 R(sub E) long tail to study the evolution, structure, and dynamics of the distant magnetotail during extended periods of northward interplanetary magnetic field (IMF). We find that the tail evolves to a nearly time stationary structure about one solar wind transit time after the IMF turns northward. Four regions of different magnetic topology can be distinguished which extend at least to the end of the simulation box at 400 R(sub E). Besides lobe field lines and open solar wind field lines tailward of an X-line, there is a broad boundary layer of closed field lines which we call the tail flank boundary layer (TFBL). Just inside the TFBL there is a region of closed field loops. Besides the X-line we find two O-lines which are enclosed by the closed field loops and are roughly aligned with the tail axis. Together they form a U shaped separator between the northward and the southward plasma sheet fields.

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