Three-dimensional computer modeling of dynamic reconnection in the magnetotail

Details Three-dimensional computer modeling of dynamic reconnection in the magnetotail Three-dimensional computer modeling of dynamic reconnection in the magnetotail

Jan 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990ap%26ss.163...95m&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 163, no. 1, Jan. 1990, p. 95-107.

Astronomy and Astrophysics

Astrophysics

Geomagnetic Tail, Magnetic Field Reconnection, Magnetic Storms, Magnetospheric Instability, Space Plasmas, Three Dimensional Models, Computerized Simulation, Field Aligned Currents, Solar Wind

Scientific paper

A three-dimensional MHD code is used to numerically study the phenomenon of a magnetospheric substorm in the magnetotail region. The results of driven reconnection calculations are used to discuss changes in the magnetospheric currents that result from driven reconnection. Emphasis is given to the generation of field-aligned currents. Also, the plasma flows that result from driven reconnection are examined and the theoretical results are compared to observational data.

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