The dynamics of an erupting prominence

Free access article

Issue		A&A Volume 381, Number 2, January II 2002


Page(s)		683 - 693
Section		The Sun
DOI		http://dx.doi.org/10.1051/0004-6361:20011513

A&A 381, 683-693 (2002)
DOI: 10.1051/0004-6361:20011513

The dynamics of an erupting prominence

K.-L. Klein and Z. Mouradian

Observatoire de Paris, Section de Meudon, DASOP & CNRS-UMR 8645, 92195 Meudon, France
e-mail: zadig.mouradian@obspm.fr

(Received 11 May 2001 / Accepted 19 October 2001)

Abstract
H $\alpha$ full disk observations and radio interferometry at decimetre and metre wavelengths are used to probe the dynamics of ejecta and electron acceleration during a solar eruptive event on 1990 September 14. An erupting prominence and a moving type IV radio source are shown to trace a common magnetic structure during its rise from ~10 Mm to 3 $R_\odot$ above the limb. The height-time plot excludes a purely ballistic flight in the height range (0.5-3) $R_\odot$ , but is consistent with both constant acceleration and constant velocity at heights $\geq$ 0.5 $R_\odot$ . A plasma model of the radio emission is used to infer the mass and energetics of the ejected material. Electrons are accelerated in the surroundings of the rising structure, and in two flares up to 70° away from the prominence. Radio observations provide evidence for large-scale interconnecting loops, but a physical connection between the eruption and the remote flares cannot be demonstrated.

Key words: Sun: activity -- corona -- CMEs -- filaments -- flares -- radio radiation

Offprint request: K.-L. Klein, ludwig.klein@obspm.fr

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