Free access article

A&A 449, L17-L20 (2006)
DOI: 10.1051/0004-6361:20064942

Letter

Large amplitude oscillation of a polar crown filament in the pre-eruption phase

H. Isobe^{1, 2} and D. Tripathi<sup>1

1</sup>  Department of Applied Mathematics and Theoretical Physics, University of Cambridge, Wilberforce Road, Cambridge CB3 0WA, UK
    e-mail: [D.H.Isobe;D.Tripathi]@damtp.cam.ac.uk
²  Department of Earth and Planetary Science, University of Tokyo, Hongo, Bunkyo-ku, Tokyo 113-0033, Japan
    e-mail: isobe@eps.s.u-tokyo.ac.jp

(Received 31 January 2006 / Accepted 10 February 2006)

Abstract
Aims.We report observation of a large-amplitude filament oscillation followed by an eruption. This is used to probe the pre-eruption condition and the trigger mechanism of solar eruptions.
Methods.We used the EUV images from the Extreme-Ultraviolet Imaging Telescope on board SOHO satellite and the H images from the Flare Monitoring Telescope at Hida Observatory. The observed event is a polar crown filament that erupted on 15 Oct. 2002.
Results.The filament clearly exhibited oscillatory motion in the slow-rising, pre-eruption phase. The amplitude of the oscillation was larger than 20 km s^-1, and the motion was predominantly horizontal. The period was about 2 h and seemed to increase during the oscillation, indicating weakening of restoring force.
Conclusions.Even in the slow-rise phase before the eruption, the filament retained equilibrium and behaved as an oscillator, and the equilibrium is stable to nonlinear perturbation. The transition from such nonlinear stability to either instabilities or a loss of equilibrium that leads to the eruption occurred in the Alfvén time scale (~1 h). This suggests that the onset of the eruption was triggered by a fast magnetic reconnection that destabilized the pre-eruption magnetic configuration, rather than by the slow shearing motion at the photosphere.

Key words: Sun: corona -- Sun: coronal mass ejections (CMEs) -- Sun: prominences -- Sun: filaments

© ESO 2006

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