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Magnetic Configuration and Evolution in a Solar Active Region

Published online by Cambridge University Press:  13 May 2016

Y. Liu  and
H. Zhang
Y. Liu
Affiliation:
Beijing Astronomical Observatory, NAOCAS, A20 Datun Road, Chaoyang District, Beijing, 100012 China
H. Zhang
Affiliation:
Beijing Astronomical Observatory, NAOCAS, A20 Datun Road, Chaoyang District, Beijing, 100012 China

Abstract

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We present results of the analysis of NOAA 8668, which was observed successively by space satellite (SOHO) and ground-based observatories (BBSO, Huairou). The combined observation offers us a good example of a region observed from low to high solar atmosphere. Several flares and a sigmoid filament were observed in the AR, and we observed the sigmoid filament from its birth to disintegration. The configuration of the magnetic field of the AR changed quickly as well as the loops. From EIT movies, we can even judge the sign of the sigmoid filament's magnetic helicity. The forming and heating of the loops were the result of magnetic reconnection, and the corona seemed heated when the loops became opened.

Type
Session III: Active Region Structure and Dynamics
Information
Symposium - International Astronomical Union , Volume 203: Recent Insights into the Physics of the Sun and Heliosphere: Highlights from Soho and Other Space Missions , 2001 , pp. 294 - 296
Copyright
Copyright © Astronomical Society of the Pacific 2001 

References

Aschwanden, et al., 1999, ApJ, 520, 880.CrossRefGoogle Scholar
Jongchui, Chae, 2000, ApJ, 540, L115.Google Scholar
Chiu, Y. T. & Hilton, H. 1977, ApJ, 212, 873.Google Scholar