The Topology of Magnetic Reconnection in the Sun's Corona

Details The Topology of Magnetic Reconnection in the Sun's Corona The Topology of Magnetic Reconnection in the Sun's Corona

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agufmsm12a..07a&link_type=abstract

American Geophysical Union, Fall Meeting 2005, abstract #SM12A-07

Astronomy and Astrophysics

Astrophysics

2100 Interplanetary Physics, 2700 Magnetospheric Physics (6939), 7500 Solar Physics, Astrophysics, And Astronomy, 7835 Magnetic Reconnection (2723, 7526)

Scientific paper

It has long been recognized that magnetic topology plays the critical role in reconnection at the magnetopause. The essential requirement for reconnection is that the system has a multi-flux topology, and the location of the reconnection is at the boundaries between the different flux systems, specifically separator lines and null points. On the other hand, it is commonly believed that reconnection driven by photospheric motions can occur more-or-less anywhere in the Sun's corona. We present both theoretical and 3D numerical simulation results arguing that, in fact, the magnetosphere and corona are physically similar in that topology strongly restricts how and where coronal reconnection can occur. We also discuss important differences between the reconnection in the corona and magnetosphere. This work was supported, in part, by ONR and NASA.

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