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CMEs and Flux Appearance in the Periphery of Two Unipolar Sunspots

Published online by Cambridge University Press:  03 June 2005

X.L. Yang ,
W.B. Song ,
G.P. Zhou ,
J. Zhang  and
J.X. Wang
X.L. Yang
Affiliation:
National Astronomy Observatories, Chinese Academy of Sciences, Beijing 100012, China email: [email protected] Present address: A20 Datun Rd., Chaoyang Dist., Beijing 100012, China
W.B. Song
Affiliation:
National Astronomy Observatories, Chinese Academy of Sciences, Beijing 100012, China email: [email protected]
G.P. Zhou
Affiliation:
National Astronomy Observatories, Chinese Academy of Sciences, Beijing 100012, China email: [email protected]
J. Zhang
Affiliation:
National Astronomy Observatories, Chinese Academy of Sciences, Beijing 100012, China email: [email protected]
J.X. Wang
Affiliation:
National Astronomy Observatories, Chinese Academy of Sciences, Beijing 100012, China email: [email protected]
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Abstract

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A class of large-scale magnetic compositions have been identified to be CME-prolific, which is characterized by a huge unipolar sunspot appearing in a large-scale extended bipolar region in synoptic magnetic charts. To understand the CMEs' origin and the nature of flux appearance, we scrutinize the long time-sequence of MDI magnetograms of high-resolution mode for super active region AR9236. Two types of magnetic features are clearly identified. They are moving magnetic features (MMFs) emanated radially from the penumbral boundary and emerging flux regions (EFRs) whose growing opposite polarities rotate out from the inner boundary of sunspot moat along helical paths in opposite directions. The interaction between the MMFs and EFRs often creates multi-fold magnetic neutral lines where the flare/CMEs initiated.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Keywords

CMEsmoving magnetic featureemerging flux region
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2004 , Issue IAUS226 , September 2004 , pp. 215 - 216
Copyright
© 2005 International Astronomical Union