Three Dimensionally Localized Reconnection in the Magnetotail During Substorms

Details Three Dimensionally Localized Reconnection in the Magnetotail During Substorms Three Dimensionally Localized Reconnection in the Magnetotail During Substorms

May 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agusmsm22a..03s&link_type=abstract

American Geophysical Union, Spring Meeting 2002, abstract #SM22A-03

Other

2744 Magnetotail, 2764 Plasma Sheet, 7835 Magnetic Reconnection, 7843 Numerical Simulation Studies

Scientific paper

Magnetic reconnection is a transport process that allows plasma from normally distinct regions to mix, allowoing solar wind plasma to penetrate into the magnetosphere and releasing magnetic energy in substorms. Although much progress has been made recently in understanding the nature of collisionless magnetic reconnection in two dimensions, the nature of reconnection which is localized along the direction perpendicular to the reconnection plane is not well understood. Using 3D two-fluid simulations of magnetic reconnection, we seek answers to the following questions: How fast does an X-line in the magnetotail grow in the Y (GSM) direction? Does an X-line have a preferred length? How do separate X-lines interact with each other? The answers to these questions may enhance our understanding of bursty bulk flows in the magnetotail.

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