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Magnetic Topology before a 3B/X1.2 Flare and the Associated CME

Published online by Cambridge University Press:  01 November 2006

H. Li ,
B. Schmieder ,
G. Aulanier  and
A. Berlicki
H. Li
Affiliation:
Purple Mountain Observatory, Nanjing 210008, China Email: lihui@mail.pmo.ac.cn
B. Schmieder
Affiliation:
Observatoire de Paris, Section de Meudon, LESIA, F-92195, Meudon Principal Cedex, France
G. Aulanier
Affiliation:
Observatoire de Paris, Section de Meudon, LESIA, F-92195, Meudon Principal Cedex, France
A. Berlicki
Affiliation:
Observatoire de Paris, Section de Meudon, LESIA, F-92195, Meudon Principal Cedex, France Astronomy Institute of the Wrocław University, ul.Kopernika 11, 51-622 Wrocław, Poland
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Abstract

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We extrapolated observed photospheric magnetic field before the 3B/X1.2 flare occurred in NOAA 10486 on 2003 October 26. Two magnetic null points exist above the active region, which have no crucial role in triggering the flare, even though enhanced TRACE EUV/UV emission was observed before the main flare due to magnetic reconnection near the lower-altitude null point. We conclude that this flare results from the loss of equilibrium due to persistent flux emergence and photospheric motion, and strong shear. The accompanying fast CME with velocity of $\sim$ 800 km $s^{-1}$ shows quick mass pickup and energy increase in the low corona. Its kinetic energy is always larger than its potential energy.

Keywords

sun: flaressun: magnetic fieldsun: UV radiation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S233: Solar Activity and its Magnetic Origin , March 2006 , pp. 399 - 400
Copyright
© 2006 International Astronomical Union