Avalanche models for solar flares (Invited Review)

Details Avalanche models for solar flares (Invited Review) Avalanche models for solar flares (Invited Review)

Nov 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001soph..203..321c&link_type=abstract

Solar Physics, v. 203, Issue 2, p. 321-353 (2001).

Physics

86

Scientific paper

This paper is a pedagogical introduction to avalanche models of solar flares, including a comprehensive review of recent modeling efforts and directions. This class of flare model is built on a recent paradigm in statistical physics, known as self-organized criticality. The basic idea is that flares are the result of an ‘avalanche’ of small-scale magnetic reconnection events cascading through a highly stressed coronal magnetic structure, driven to a critical state by random photospheric motions of its magnetic footpoints. Such models thus provide a natural and convenient computational framework to examine Parker's hypothesis of coronal heating by nanoflares.

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