Astronomy and Astrophysics – Astronomy
Scientific paper
Jun 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006spd....37.0801m&link_type=abstract
American Astronomical Society, SPD meeting #37, #8.01; Bulletin of the American Astronomical Society, Vol. 38, p.230
Astronomy and Astrophysics
Astronomy
Scientific paper
We tried to verify whether the local reconnection rate (coronal electric field) and the global reconnection rate (magnetic flux change rate) as well as the energy release rate (Poynting flux) in a two-ribbon flare can be derived from chromospheric/photospheric observations. Furthermore, we tested whether equal shares of positive and negative magnetic flux are involved in the flare process.A well observed GOES M3.9 two-ribbon flare was analyzed. The required observables (ribbon expansion velocity, magnetic field strength at the ribbon front, and newly brightened area) were extracted from TRACE 1600 Å and Kanzelhöhe H-alpha image time series, and a SOHO MDI magnetogram, respectively. Furthermore, the ratio of the converted positive vs. negative magnetic flux was determined. RHESSI Hard X-ray 20 - 60 keV full-disk time profiles as well as subregion imaging light curves derived from a time series of RHESSI images in the same energy range, were used as independent, observable proxies of the reconnection and the energy release rate, respectively. The RHESSI images were also used to localize the sites where the bulk of the energy was deposited by fast electrons.We found good temporal correlations between derived time profiles (local and global reconnection rate, Poynting flux) and observed HXR flux. The local reconnection rate peak values ranged from 1.4 V/cm to 4.6 V/cm, and the ratio of converted positive vs. negative magnetic flux deviated from the theoretically expected value by only 5 - 10%.The results indicate that the local reconnection rate, the global reconnection rate as well as the energy release rate in a simple two-ribbon flare can be derived from chromospheric/photospheric observations. Furthermore, it was confirmed that equal shares of positive and negative magnetic flux participated in the reconnection process.This work is supported by the Austrian ‘Fonds zur Förderung der wissenschaftlichen Forschung’ under project P15344.
Miklenic Christiane H.
Veronig Astrid M.
Vrsnak Bojan
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