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CMEs driven by an eruptive prominence

Published online by Cambridge University Press:  01 November 2006

G. P. Zhou
Affiliation:
National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China email: [email protected]
J. X. Wang
Affiliation:
National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China email: [email protected]
J. Zhang
Affiliation:
National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China email: [email protected]
P. F. Chen
Affiliation:
Department of Astronomy, Nanjing University, Nanjing 210093, China
H. S. Ji
Affiliation:
Purple Mountain Observatory, 2 Beijing Xi Lu, Nanjing 210008, China
K. Dere
Affiliation:
George Mason University, 4400 University Drive, USA
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Abstract

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A clear case on Dec. 28 2002 is presented. It is about the initiation of two successive CMEs, which were related to an eruptive prominence. In EIT 304 Å and 195 Å observations, we found a long filament severely twisting in a piece of its fragments, which appeared as a prominence on Dec. 26. Then, the prominence converted its twist into writhe. Two days later, the prominence displayed a slow rising motion for hours. There happened internal twisting and mass motion before the prominence rapid acceleration and final eruption. Two successive CMEs recorded by LASCO C2 coronagraph corresponded to the early rising and the subsequently eruptive phases of the prominence, respectively. Evidence of magnetic reconnection, i.e., a cusp structure and post-flare loops in EUV wavebands, and hard X-ray sources in the corona, were observed after the prominence disruption. It appears that the kink instability and the mass drainage in the prominence played important roles in triggering two CMEs' initiation. We suspected that the rather impulsive acceleration of the second CME resulted from magnetic reconnection beneath the prominence.

Type
Contributed Papers
Copyright
© 2006 International Astronomical Union