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To test the standard flare model (CSHKP-model), we measured the magnetic-fluxchange rate in five flare events of different GOES classes usingchromospheric/photospheric observations and compared its progression withobserved nonthermal flare emission. We calculated the cumulated positive andnegative magnetic flux participating in the reconnection process, as well asthe total reconnection flux. Finally, we investigated the relations between thetotal reconnection flux, the GOES class of the events, and the linear velocityof the flare-associated CMEs. Using high-cadence H-alpha and TRACE 1600 A imagetime-series data and MDI/SOHO magnetograms, we measured the requiredobservables (newly brightened flare area and magnetic-field strength insidethis area). RHESSI and INTEGRAL hard X-ray time profiles in nonthermal energybands were used as observable proxies for the flare-energy release rate. Wedetected strong temporal correlations between the derived magnetic-flux changerate and the observed nonthermal emission of all events. The cumulated positiveand negative fluxes, with flux ratios of between 0.64 and 1.35, were almostequivalent to each other. Total reconnection fluxes ranged between 1.8 x 10^21Mx for the weakest event (GOES class B9.5) and 15.5 x 10^21 Mx for the mostenergetic one (GOES class X17.2). The amount of magnetic flux participating inthe reconnection process was higher in more energetic events than in weakerones. Flares with more reconnection flux were associated with faster CMEs.

Temporal comparison of nonthermal flare emission and magnetic-flux change rates