Magnetic Reconnection and Energetics of the 2000 March 22 Solar Flare

Details Magnetic Reconnection and Energetics of the 2000 March 22 Solar Flare Magnetic Reconnection and Energetics of the 2000 March 22 Solar Flare

May 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000spd....31.0260g&link_type=abstract

American Astronomical Society, SPD Meeting #31, #02.60; Bulletin of the American Astronomical Society, Vol. 32, p.821

Astronomy and Astrophysics

Astronomy

1

Scientific paper

The evolution and properties of the 2000 March 22 X--class flare from the β δ active region NOAA 8910 are discussed using high resolution radio observations from the Owen's Valley Solar Array, TRACE UV and EUV filtergrams, GOES soft X-rays, and magnetograms from MDI on board SOHO. The episodic flare evolution is found to be extremely complicated at all observed wavelengths and releases a large amount of both thermal and non--thermal energy. From the UV and EUV observations, the flare is shown to be consistent with the model in which the release of energy is caused by several, successive loop interactions while the radio observations identify multiple non--thermal electron acceleration sites. The final stage of the flare is then characterised by the emergence of a set of post--flare loops parallel to the magnetic neutral line as the system relaxes.

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