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CMEs ‘en rafale’ observations and simulations

Published online by Cambridge University Press:  01 September 2008

Cristiana Dumitrache*
Affiliation:
Astronomical Institute of Romanian Academy, Str. Cutitul de Argint 5, Bucharest 040557, Romania email: crisd@aira.astro.ro
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Abstract

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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).

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2009

References

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