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Upward velocities of the reconnection points and coronal magnetic field strengths in flaring regions derived from the GOES X-ray light curves

Published online by Cambridge University Press:  01 November 2006

Tetsuya T. Yamamoto  and
T. Sakurai
Tetsuya T. Yamamoto
Affiliation:
Department of Astronomy, The University of Tokyo, Bunkyo-ku, Tokyo 113-0033, Japan email: yamamoto@solar.mtk.nao.ac.jp
T. Sakurai
Affiliation:
Department of Astronomy, The University of Tokyo, Bunkyo-ku, Tokyo 113-0033, Japan email: yamamoto@solar.mtk.nao.ac.jp National Astronomical Observatory of Japan, Mitaka, Tokyo, 181-8588, Japan
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Abstract

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From Yohkoh and SoHO observations, the magnetic reconnection is considered as a main energy release mechanism of the solar active phenomena. In this study, we try to reproduce GOES X-ray light curves (1–8 $\AA$) of solar flares using a model incorporating the radiative and conductive cooling and the magnetic reconnection heating.

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S233: Solar Activity and its Magnetic Origin , March 2006 , pp. 128 - 129
Copyright
© 2006 International Astronomical Union