Formation of Transient Coronal Holes during Eruption of a Quiescent Filament and its Overlying Sigmoid

Details Formation of Transient Coronal Holes during Eruption of a Quiescent Filament and its Overlying Sigmoid Formation of Transient Coronal Holes during Eruption of a Quiescent Filament and its Overlying Sigmoid

2009-01-07

arxiv.org/abs/0901.0784v1

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

8 pages, 5 figures, accepted by Chjaa

Scientific paper

By using H$\alpha$, He I 10830, EUV and soft X-ray (SXR) data, we examined a filament eruption that occurred on a quiet-sun region near the center of the solar disk on 2006 January 12, which disturbed a sigmoid overlying the filament channel observed by the $\emph{GOES-12}$ SXR Imager (SXI), and led to the eruption of the sigmoid. The event was associated with a partial halo coronal mass ejection (CME) observed by the Large Angle and Spectrometric Coronagraphs (LASCO) on board the Solar and Heliospheric Observatory ($\emph{SOHO}$), and resulted in the formation of two flare-like ribbons, post-eruption coronal loops, and two transient coronal holes (TCHs), but there were no significantly recorded $\emph{GOES}$ or H$\alpha$ flares corresponding to the eruption. The two TCHs were dominated by opposite magnetic polarities and were located on the two ends of the eruptive sigmoid. They showed similar locations and shapes in He I 10830, EUV and SXR observations. During the early eruption phase, brightenings first appeared on the locations of the two subsequent TCHs, which could be clearly identified on He I 10830, EUV and SXR images. This eruption event could be explained by the magnetic flux rope model, and the two TCHs were likely to be the feet of the flux rope.

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