Catastrophe Model for the Onset of Fast Magnetic Reconnection

Details Catastrophe Model for the Onset of Fast Magnetic Reconnection Catastrophe Model for the Onset of Fast Magnetic Reconnection

May 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...210.6803c&link_type=abstract

American Astronomical Society Meeting 210, #68.03; Bulletin of the American Astronomical Society, Vol. 39, p.175

Astronomy and Astrophysics

Astrophysics

Scientific paper

It is widely accepted that magnetic reconnection is the mechanism releasing the magnetic energy in solar eruptions, but what initiates an eruption has long been an unresolved problem. We present a model for the onset of fast magnetic reconnection, which potentially explains why the energy release begins abruptly. In particular, we have found that magnetic reconnection is bistable: both the slow (Sweet-Parker) and the fast (Hall/Petschek) mode of reconnection independently exist for a wide range of resistivities. However, the Sweet-Parker solution disappears catastrophically at a critical value, leading to the onset of Hall reconnection and the accompanying increase in the rate of magnetic energy release by many orders of magnitude. We present theory and simulations confirming the model, discuss potential mechanisms for onset, and compare predictions with eruptions in the solar corona.

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