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The hard X-ray emission in a solar flare is typically characterized by anumber of discrete sources, each with its own spectral, temporal, and spatialvariability. Establishing the relationship amongst these sources is critical todetermine the role of each in the energy release and transport processes thatoccur within the flare. In this paper we present a novel method to identify andcharacterize each source of hard X-ray emission. The method permits aquantitative determination of the most likely number of subsources present, andof the relative probabilities that the hard X-ray emission in a given subregionof the flare is represented by a complicated multiple source structure or by asimpler single source. We apply the method to a well-studied flare on2002~February~20 in order to assess competing claims as to the number ofchromospheric footpoint sources present, and hence to the complexity of theunderlying magnetic geometry/toplogy. Contrary to previous claims of the needfor multiple sources to account for the chromospheric hard X-ray emission atdifferent locations and times, we find that a simpletwo-footpoint-plus-coronal-source model is the most probable explanation forthe data. We also find that one of the footpoint sources moves quite rapidlythroughout the event, a factor that presumably complicated previous analyses.The inferred velocity of the footpoint corresponds to a very high inducedelectric field, compatible with those in thin reconnecting current sheets.

Identification of multiple hard X-ray sources in solar flares: A Bayesian analysis of the February 20 2002 event