The Magnetic Topology of Solar Activity

Details The Magnetic Topology of Solar Activity The Magnetic Topology of Solar Activity

Nov 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998aps..dpp.b1m05a&link_type=abstract

American Physical Society, Division of Plasma Physics Meeting, November 16-20, 1998 New Orleans, LA, abstract #B1M.05

Physics

Plasma Physics

Scientific paper

Solar activity can appear in many forms, ranging from small spicules with size scales < 1000 km and energies < 10^24 ergs, to giant coronal mass ejections and eruptive flares with scales of order the solar radius and energies up to 10^33 ergs. The underlying driver for all this dynamics is the Sun's magnetic field. The high-beta plasma below the photosphere generates and stresses magnetic field which emerges through the surface and, in turn, energizes the plasma in the low-beta corona. We describe the recent observations of violent solar activity and present a general theoretical framework for understanding them. We argue that strong activity requires two key features: the magnetic field must have a multi-polar topology, and magnetic reconnection in the solar corona must have a bursty nature. We present results from numerical simulations that show how these features lead to the observed dynamics. (This work was supported in part by NASA and ONR.)

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