Hα , EUV, and Microwave Observations of a Large Flare as Evidence for Spontaneous Magnetic Reconnection

Details Hα , EUV, and Microwave Observations of a Large Flare as Evidence for Spontaneous Magnetic Reconnection Hα , EUV, and Microwave Observations of a Large Flare as Evidence for Spontaneous Magnetic Reconnection

May 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003spd....34.1604l&link_type=abstract

American Astronomical Society, SPD meeting #34, #16.04; Bulletin of the American Astronomical Society, Vol. 35, p.833

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Scientific paper

The large solar flare with GOES class X1.1 occurred on 2000 March 22 is observed with the Owens Valley Solar Array (OVSA), Hα filtergram of Big Bear Solar observatory (bbso), the Transition region and Coronal Explorer (trace), and the Michelson Doppler Imager (mdi) onboard Solar and Heliospheric Observatory (SOHO). During the impulsive phase a set of EUV loops are visible in a small volume confined to the center of the large β γ δ -type active region. Radio emission at 5 GHz appears as a single source encompassing multiple Hα ribbons, and radio emissions at other frequencies also appear within the central core region. We interpret these observations under the idea of the confined flare in contrast with the more commonly cited, eruptive flare, using a schematic magnetic reconnection geometry based on the mdi magnetogram. It is suggested that the EUV loops represent a separatrix in part, and that the radio and Hα sources coincide with the whole part of the separatrix and its footpoints, respectively. In addition, a Coronal Mass Ejection (CME) as detected in the LASCO coronagraph after this flare is briefly discussed in relation to the above idea of magnetic reconnection.
This work has been supported by NASA grants NAG 5-10891 and NAG-11875.

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