Eruption of a Quiescent Filament on February 18, 2003

Details Eruption of a Quiescent Filament on February 18, 2003 Eruption of a Quiescent Filament on February 18, 2003

Jan 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005hia....13..142b&link_type=abstract

Highlights of Astronomy, Vol. 13, as presented at the XXVth General Assembly of the IAU - 2003 [Sydney, Australia, 13 - 26 July

Astronomy and Astrophysics

Astronomy

Scientific paper

Eruption process of a quiescent filament on Feb. 18 2003 which initiated a CME was recorded by H-alpha full disk telescope in Huairou Solar Observing Station (HSOS) and Extreme ultraviolet Imaging Telesccope (EIT) Michelson Doppler Imager (MDI) and Large Spectrametric Coronagraph (LASCO) on board Solar and Heliosphere Observatory (SOHO). The eruption reveal a typical process of energy releasing and dense plasma ejection caused by magnetic instability. Filament eruptions flares and CMEs are believed to be same physical process of magnetic eruption and reconnection in three different stages. This feature was shown clearly in the eruption of the quiescent filament since the simple and regular magnetic field in photosphere. The helical structure which imply the non-potential magnetic field inside filament can be found in early stage when the filament detached from photosphere. The H-alpha emission appear in the magnetic foot points of the filament in the photosphere which was connected by the post-eruption loops. The weak field under the filament maybe the main reason why the H-alpha emission is not bright enough to be thought as a flare. The evolution of the possible magnetic configuration is described.

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