Other
Scientific paper
May 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...210.9320j&link_type=abstract
American Astronomical Society Meeting 210, #93.20; Bulletin of the American Astronomical Society, Vol. 39, p.214
Other
Scientific paper
Recently it became popular to estimate the energy release rate during two-ribbon flares from the ribbon observations within the framework of standard reconnection theory. One of the key parameters in this technique is the actual area of the reconnecting current sheet in the corona, by which we can finally convert the electromagnetic Poynting flux to the energy release rate. Many studies chose to estimate this parameter from the visual size of the magnetic arcade involved with the reconnection and keep it constant of time. We present an alternative method to derive it from its observed counterpart, the ribbon area, under the principle of magnetic flux conservation. An observational requirement is that the ribbon radiation should represent only the instantly illuminated chromospheric part connected to the coronal diffusion region. H-alpha centerline images are certainly inadequate for this usage as they retain the previously heated areas to some extent. We instead run the technique on other ribbon images obtained at H-alpha blue wing, Near Infrared, and UV/EUV wavelengths that often show sharper ribbon edges. Not only the spatial properties but temporal behaviors of those ribbon areas are used to test whether they are suitable quantities for this purpose or not. The test result is presented along with our measurements of all parameters involved with the magnetic reconnection.
Jing Ju
Lee Julian
Liu Chan Chiang
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