Physics
Scientific paper
May 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm..sh41c01k&link_type=abstract
American Geophysical Union, Spring Meeting 2001, abstract #SH41C-01 INVITED
Physics
7513 Coronal Mass Ejections, 7531 Prominence Eruptions
Scientific paper
Numerous quantitative comparisons[1-4] of observational data to a flux-rope model of coronal mass ejections (CMEs) show that flux-rope CMEs are common events with specific geometrical and dynamical properties. In the model, a CME corresponds to a flux rope with foot points that remain anchored in the photosphere as it erupts. Comparisons of model results for various drive mechanisms[5] to observed CMEs show that flux injection (an increase in poloidal flux) provides the best match. With flux-injection, the CME is driven during and after the onset of eruption. Thus, acceleration time-scales are on the order of hours in agreement with observed CMEs, many or which are neither ``quasi-static'' nor ``impulsive.'' This contrasts with the photospheric-shearing paradigm in which there is a loss of equilibrium resulting in a characteristic velocity profile that does not match the observations in detail. Photospheric signatures of eruption are also studied; the model predicts no significant ``twisting up'' of the magnetic field at the photosphere during flux injection. [1] Chen, J. et al., 1997, ApJ, 490, L191 [2] Wood, B.E. et al., 1998, ApJ, 512, 484. [3] Chen, J. et al., 2000, ApJ, 533, 481 [4] Krall, J. et al., 2001, ApJ, submitted [5] Krall, J. et al., 2000, ApJ, 539, 964 Work supported by ONR.
Chen Jiahua
Krall Jonathan
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