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A bright coronal downflow seen in multi-wavelength observations: evidence of a bifurcating flux-rope? View all abstracts by submitter

Durgesh Tripathi   Submitted: 2007-07-03 05:23

Aim: To study the origin and characteristics of a bright coronal downflow seen after a coronal mass ejection associated with erupting prominences on 5~March 2000. Methods: This study extends that of Tripathi et al. (2006) based on the Extreme-ultraviolet Imaging Telescope (EIT), the Soft X-ray Telescope (SXT) and the Large Angle Spectrometric Coronagraph (LASCO) observations. We combined those results with an analysis of the observations taken by the H α and the Mk4 coronagraphs at the Mauna Loa Solar Observatory (MLSO). The combined data-set spans a broad range of temperature as well as continuous observations from the solar surface out to 30 Rsun. Results: The downflow started at around 1.6Rsun and contained both hot and cold gas. The downflow was observed in the H α and the Mk4 coronagraphs as well as the EIT and the SXT and was approximately co-spatial and co-temporal providing evidence of multi-thermal plasma. The H α and Mk4 images show cusp-shaped structures close to the location where the downflow started. Mk4 observations reveal that the speed of the downflow in the early phase was substantially higher than the free-fall speed, implying a strong downward acceleration near the height at which the downflow started. Conclusions: The origin of the downflow was likely to have been magnetic reconnection taking place inside the erupting flux rope that led to its bifurcation.

Authors: D. Tripathi, S.K. Solanki, H.E. Mason, D.F. Webb
Projects: None

Publication Status: Accepted for publication in Astronomy and Astrophysics
Last Modified: 2007-07-03 09:43
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