Hostname: page-component-586b7cd67f-t8hqh Total loading time: 0 Render date: 2024-11-28T01:14:40.836Z Has data issue: false hasContentIssue false
  • English
  • Français

CMEs ‘en rafale’ observations and simulations

Published online by Cambridge University Press:  01 September 2008

Cristiana Dumitrache
Cristiana Dumitrache*
Affiliation:
Astronomical Institute of Romanian Academy, Str. Cutitul de Argint 5, Bucharest 040557, Romania email: [email protected]
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

A CME is triggered by the disappearance of a stable equilibrium as a result of the slow evolution of the photospheric magnetic field. This disappearance may be due to a loss of ideal-MHD equilibrium or stability as in the kink mode, or to a loss of resistive-MHD equilibrium as a result of magnetic reconnection. We have obtained CMEs in sequence by a time dependent magnetohydrodynamic computation performed on three solar radii. These successive CMEs resulted from a prominence eruption. Velocities of these CMEs decrease in time, from a CME to another. We present observational evidences for large-scale magnetic reconnections that caused the destabilization of a sigmoid filament. These reconnections covered half of the solar disk and produced CMEs in squall (sequential CMEs).

Keywords

coronal mass ejectionsmagnetic fieldsprominencesinstabilities
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Symposium S257: Universal Heliophysical Processes , September 2008 , pp. 251 - 255
Copyright
Copyright © International Astronomical Union 2009

References

Dumitrache, C. 2007, ASP Serie, 370, 180Google Scholar
Dumitrache, C. 1999, RoAJ, 9, 139Google Scholar
Forbes, T. G. & Priest, E. R. 1982, Sol.Phys. 81, 303CrossRefGoogle Scholar
Weber, W. J. 1979, Sol.Phys., 61, 345CrossRefGoogle Scholar