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Rapid Acceleration of a Coronal Mass Ejection in the Low Corona and Implications for Propagation View all abstracts by submitter

Peter Gallagher   Submitted: 2003-03-25 12:24

A high-velocity Coronal Mass Ejection (CME) associated with the 2002 April 21 X1.5 flare is studied using a unique set of observations from the Transition Region and Coronal Explorer (TRACE), the Ultraviolet Coronagraph Spectrometer (UVCS), and the Large-Angle Spectrometric Coronagraph (LASCO). The event is first observed as a rapid rise in GOES X-rays, followed by two simultaneous brightenings which appear to be connected by an ascending loop-like feature. While expanding, the appearance of the feature remains remarkably constant as it passes through the TRACE 195-A passband and LASCO fields-of-view, allowing its height-time behaviour to be acurately determined. The acceleration is consistent with an exponential rise with an e-folding time of ~138-s and peaks at ~1500 m s-2 when the leading-edge is at ~1.7 R from Sun center. The acceleration subsequently falls off with an e-folding time of over 1000-s. At distances beyond ~3.4 R, the height-time profile is approximately linear with a constant velocity of ~2500 km s-1. These results are briefly discussed in light of recent kinematic models of CMEs.

Authors: Gallagher, P. T., Lawrence, G. R., Dennis, B. R.

Publication Status: ApJL (accepted)
Last Modified: 2003-03-25 12:25
Go to main E-Print page  An Explanation for Non-Power-law Behavior in the Hard X-ray Spectrum of the July 23, 2002 Solar  Propagating EUV disturbances in the Solar corona: two-wavelength observations  Edit Entry  Download Preprint  Submitter's Homepage Delete Entry 

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