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The Relationship between CMEs and Prominence Eruptions

Published online by Cambridge University Press:  13 May 2016

B. Schmieder ,
L. van Driel-Gesztelyi ,
C. Delannée ,
G. M. Simnett  and
J. E. Wiik
B. Schmieder
Affiliation:
Observatoire de Paris, 92195 Meudon, Cedex Principal, France
L. van Driel-Gesztelyi
Affiliation:
Observatoire de Paris, 92195 Meudon, Cedex Principal, France
C. Delannée
Affiliation:
NASA/GSFC, Code 682.3, Greenbelt, MD 20771, USA
G. M. Simnett
Affiliation:
School of Phys. and Astro., University of Birmingham, B15 2TT, UK
J. E. Wiik
Affiliation:
Institut of Astrophysics, University of Oslo, Blindern, Norway

Abstract

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We have studied the temporal relationship between three selected prominence eruptions and their associated coronal mass ejections (CME). For these three events it is not possible to predict from the CME time history when the prominence would erupt. However, both are signatures of destabilisation of the global coronal magnetic field. The lack of a precise temporal relationship reflects the fact that several coronal stuctures are destabilised, and in general one will predominate in the CME structure. If this structure happens to be the same as that constraining the prominence, then the latter will erupt following the launch of the CME. If the prominence is constrained by a separate magnetic structure, then it may erupt before or after the main CME. Reconfiguration of the global coronal field probably drives a fast increase of the poloidal field in the prominence flux tube or introduces destabilising shear forces. Events on May 1, 1996, September 25-27, 1996, and May 31 1997 are discussed.

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. 310 - 313
Copyright
Copyright © Astronomical Society of the Pacific 2001 

References

Aulanier, G. and Démoulin, P.: 1998, A&A, 329, 125.Google Scholar
Schmieder, B., Delannée, C., Deng, Y. et al.: 2000, A&A 358, 728.Google Scholar
Wiik, J., Schmieder, B., Kucera, T., Simnett, G.: 1997, Solar Phys., 175, 411.CrossRefGoogle Scholar