Flare-like energy release by flux pile-up reconnection

Details Flare-like energy release by flux pile-up reconnection Flare-like energy release by flux pile-up reconnection

Feb 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000soph..191..359c&link_type=abstract

Solar Physics, v. 191, Issue 2, p. 359-379 (2000).

Physics

16

Scientific paper

Flux pile-up magnetic merging solutions are discussed using the simple robust arguments of traditional steady-state reconnection theory. These arguments determine a unique scaling for the field strength and thickness of the current layer, namely B_s~ɛ^-1/3, l~ɛ^2/3, which are consistent with a variety of plasma inflow conditions. Next we demonstrate that flux pile-up merging can also be understood in terms of exact magnetic annihilation solutions. Although simple annihilation models cannot provide unique reconnection scalings, we show that the previous current sheet scalings derive from an optimized solution in which the peak dynamic and magnetic pressures balance in the reconnection region. The build-up of magnetic field in the current sheet implicit in flux pile-up solutions naturally leads to the idea of saturation. Hydromagnetic pressure effects limit the magnetic field in the sheet, yielding an upper limit on the reconnection rate for such solutions. This rate is still far superior to the Sweet-Parker merging rate, which can be derived by seeking solutions that avoid all forms of saturation. Finally we compare time dependent numerical simulations of the coalescence instability with the optimized flux pile-up models. This comparison suggests that merging driven by the relatively slow approach of large flux systems may be favored in practice.

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