Interpretation of Statistical Flare Data using Magnetic Reconnection Models

Details Interpretation of Statistical Flare Data using Magnetic Reconnection Models Interpretation of Statistical Flare Data using Magnetic Reconnection Models

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002soph..211..275c&link_type=abstract

Solar Physics, v. 211, Issue 1, p. 275-287 (2002).

Physics

3

Scientific paper

The ability of magnetic reconnection solutions to explain statistical flare data is discussed. It is assumed that flares occur at well-defined, isolated sites within an active region, determined by the null points and separators of the coronal magnetic field (Craig, 2001). Statistical flare observations then derive from a multiplicity of independent sites, flaring in parallel, that produce events of widely varying output (Wheatland, 2002). Given that the `separator length' at an individual site controls the event frequency and the mean energy release, it is shown that the observed frequency-energy spectrum N(E)can be inverted to yield a source function that relates directly to the distribution of separator lengths. It is also pointed out that, under the parallel flaring model, inferred waiting-time distributions are naturally interpreted as a superposition of individual point processes. Only a modest number of flaring separators is required to mimic a Poisson process.

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