Hostname: page-component-6bf8c574d5-m789k Total loading time: 0 Render date: 2025-03-07T17:20:41.870Z Has data issue: false hasContentIssue false
  • English
  • Français

Evolution of Coronal Magnetic Structures

Published online by Cambridge University Press:  14 August 2015

R. S. Steinolfson  and
S. T. Wu
R. S. Steinolfson
Affiliation:
The University of Alabama in Huntsville Huntsville, Alabama 35805, U.S.A.
S. T. Wu
Affiliation:
The University of Alabama in Huntsville Huntsville, Alabama 35805, U.S.A.

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Several classes or types of coronal transients are believed to originate near the solar surface at the base of pre-existing coronal magnetic loops. These loops often lie beneath an overlying open-field region in a typical coronal- or helmet-streamer configuration. Recent experimental results indicate that these pre-existing magnetic loops may be torn open by the explosive force of the solar phenomena responsible for the transient. Numerical solutions of the time-dependent, two-dimensional, dissipationless, MHD equations of motion (the equations are discussed by Steinolfson et al. (1978)) are used to examine the formation of a coronal streamer magnetic structure and the evolution of the streamer following an explosive solar event in the closed-field region.

Type
Part VI. Coronal and Interplanetary Responses to Short Time Scale Phenomena: - Theoretical Considerations
Information
Symposium - International Astronomical Union , Volume 91: Solar and Interplanetary Dynamics , 1980 , pp. 483 - 486
Copyright
Copyright © Reidel 1980 

References

Endler, F.: 1971, , Google Scholar
Pneuman, G. W., and Kopp, R. A.: 1971, Solar Phys., 18, pp. 258–270.Google Scholar
Steinolfson, R. S., Wu, S. T., Dryer, M., Tandberg-Hanssen, E.: 1978, Astrophys. J., 225, pp. 259–274.Google Scholar
Weber, W. J.: 1978, , .Google Scholar