Volume 405, Number 1, July I 2003
|Page(s)||313 - 323|
|Published online||16 June 2003|
Interpretation of a complex CME event: Coupling of scales in multiple flux systems
CICGE, Observatório Astronómico Prof. Manuel de Barros, Faculdade de Ciências da Universidade do Porto, 4430-146 Vila Nova de Gaia, Portugal
2 LESIA UMR CNRS 8100, Observatoire de Paris, 92195 Meudon, France
3 National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, PR China
4 Institut d'Astrophysique Spatiale, Université de Paris-Sud-CNRS, Bât. 121, 91405 Orsay, France
Corresponding author: D. Maia, firstname.lastname@example.org
Accepted: 7 February 2003
Using multi-wavelength observations, in particular in imagery, recorded by SOHO/LASCO-MDI, Yohkoh/SXT, the Meudon spectroheliograph and the Nançay radioheliograph, and performing a linear force-free field extrapolation, we analyzed the triggering and the development of a complex eruptive event in the chromosphere and in the corona. This event included an X1 class flare and an eruptive filament within an active region, but it also involved a whole active complex spanning over 40 degrees of heliolongitude. It resulted in a fast and decelerating partial halo CME, associated with a Moreton wave and a complex series of metric, decimetric and microwave radio bursts. The presence of a coronal null point combined with the occurrence of two distant and nearly simultaneous radio sources give strong arguments in favor of the generalized breakout model for the triggering of the eruption. The observations are consistent with the occurrence of magnetic reconnection at the null point three minutes before the start of the eruption, which is consistent with other observed CME precursors. The analysis of the subsequent development of the event suggests that large interconnecting loops were ejected together with the CME, and that secondary reconnections at low altitude probably occurred remotely in the active complex. Our results show that the triggering and evolution of this complex CME involved multiple magnetic flux systems over a large coronal volume surrounding the flare site, and that it resulted from the coupling of scales from narrow reconnection current sheets to very large inter active region magnetic connections.
Key words: Sun: coronal mass ejections (CMEs) / Sun: flares / Sun: radio emission / Sun: magnetic fields
© ESO, 2003
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