Filament activity and photospheric magnetic evolution related to flares

Free access article

Issue		A&A Volume 367, Number 3, March I 2001


Page(s)		1022 - 1032
Section		The Sun
DOI		http://dx.doi.org/10.1051/0004-6361:20000551

A&A 367, 1022-1032 (2001)
DOI: 10.1051/0004-6361:20000551

Filament activity and photospheric magnetic evolution related to flares

Y. Jiang^{1, 2} and J. Wang¹

¹ Beijing Astronomical Observatory, National Astronomical Observatories, Chinese Academy of Science, Beijing 100012, PR China
² Yunnan Astronomical Observatory, Chinese Academy of Science, Kunming 650011, PR China
e-mail: jych@ourstar.bao.ac.cn

(Received 20 March 2000 / Accepted 25 August 2000 )

Abstract
Three successive activations of an active-region filament were observed over a period of eight hours. Each disturbance showed distinctive characteristics and was followed by a flare of different properties. The filament had one end rooted in strong ${\delta}$ -sunspots. During the first activation, the filament rose up at the rooting end and detached from the ${\delta}$ -sunspots while its main body remained in place and separated into two twisted threads. During the second activation, only one thread was disturbed and finally disappeared; twisted threads, however, appeared during the third activation. The evolution of photospheric magnetic fields, associated with the filament disturbances, was characterized by squeezing and shearing of ${\delta}$ -sunspots, flux cancellation and emergence beneath the two ends of the filaments. Our data suggests that magnetic reconnection in the photospheric layer is the likely cause of filament destabilisation.

Key words: Sun: prominences -- Sun: filaments -- Sun: activity -- Sun: flares -- Sun: magnetic fields

Offprint request: Y. Jiang, jyc@cosmos.ynao.ac.cn

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