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Propagation of an MHD Shock in the Vicinity of a Magnetic Neutral Sheet

Published online by Cambridge University Press:  14 August 2015

D. J. Mullan  and
R. S. Steinolfson
D. J. Mullan
Affiliation:
Bartol Research Foundation of the Franklin Institute, University of Delaware, Newark, DE 19711
R. S. Steinolfson
Affiliation:
University of Alabama, PO Box 1247, Huntsville, AL 35807

Extract

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The acceleration of solar cosmic rays in association with certain solar flares is known to be highly correlated with the propagation of an MHD shock through the solar corona (Svestka, 1976). The spatial structure of the sources of solar cosmic rays will be determined by those regions of the corona which are accessible to the flare-induced shock. The regions to which the flare shock is permitted to propagate are determined by the large scale magnetic field structure in the corona. McIntosh (1972, 1979) has demonstrated that quiescent filaments form a single continuous feature (a “baseball stitch”) around the surface of the sun. It is known that helmet streamers overlie quiescent filaments (Pneuman, 1975), and these helmet streamers contain large magnetic neutral sheets which are oriented essentially radially. Hence the magnetic field structure in the low solar corona is characterized by a large-scale radial neutral sheet which weaves around the entire sun following the “baseball stitch”. There is therefore a high probability that as a shock propagates away from a flare, it will eventually encounter this large neutral sheet.

Type
Part IV. Solar Transient Phenomena Affecting the Corona and Interplanetary Medium: - Theoretical Considerations
Information
Symposium - International Astronomical Union , Volume 91: Solar and Interplanetary Dynamics , 1980 , pp. 323 - 326
Copyright
Copyright © Reidel 1980 

References

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