Other
Scientific paper
May 2005
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agusmsh53a..07s&link_type=abstract
American Geophysical Union, Spring Meeting 2005, abstract #SH53A-07
Other
7513 Coronal Mass Ejections, 7524 Magnetic Fields, 7531 Prominence Eruptions
Scientific paper
Coronal mass ejections usually occur in association with eruptive prominences or flares. The kinematics of flare-associated CMEs are generally characterised by fast speeds with little or no observable acceleration beyond the occulting disk. On the other hand, CMEs associated with eruptive prominences tend to attain lower speeds and have discernible acceleration beyond the occulting disk. It has been suggested that the two classes of CMEs correspond to a common magnetic flux-rope geometry but differ in the amount of magnetic energy that drives the eruption. The acceleration profiles are also critically influenced by the Alfven speed in the erupting flux rope. This paper analyzes a number of eruptive solar prominences in H-alpha which were associated with CMEs in the frame-work of flux-rope model in order to specifically understand the dynamics of erupting prominences. The geometrical properties of prominences viz. the footpoint separation and the apex height are the key parameters of this model which influence the acceleration and the height at which maximum acceleration of the prominence occurs. The comparative study of model and observations using Hα and SECCHI observations will shed new light on the geometrical relationship between the flux rope, the prominence, and the bright rim of the CME during the eruption.
Chen Jiahua
Krall Jonathan
Srivastava Namita
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