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Particle Acceleration in the Process of Eruptive Opening and Reconnection of Magnetic Fields

Published online by Cambridge University Press:  14 August 2015

Z. Švestka ,
S. F. Martin  and
R. A. Kopp
Z. Švestka
Affiliation:
SRL Utrecht, Holland, and UCSD, Calif., U.S.A.
S. F. Martin
Affiliation:
San Fernando Observatory, CSUN, Calif., U.S.A.
R. A. Kopp
Affiliation:
Los Alamos Scientific Lab., New Mexico, U.S.A.

Extract

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In a series of papers on the flare of 29 July 1973 (Nolte et al., 1979; Martin, 1979; Švestka et al., 1979) it has been shown that Hα “post-flare” loops are the cooled aftermath of previously hot coronal loops which were visible in x-rays in the same position earlier in the flare. Kopp and Pneuman (1976) have proposed that these post-flare loops are formed by a process of successive magnetic field reconnections of previously distended magnetic field lines as illustrated in Figure 1. Each successive reconnection of the magnetic field yields a closed magnetic loop that forms above and concentric with previously formed loops. A shock wave created during each sudden reconnection travels down both legs of each loop and provides energy for ionizing chromospheric mass at the footpoints of the loop. Subsequent condensation of the ionized mass at the tops of the loops renders them visible as this mass falls to the chromosphere.

Type
Part III. Solar Transient Phenomena Affecting the Corona and Interplanetary Medium: Dynamics Deduced from Observations
Information
Symposium - International Astronomical Union , Volume 91: Solar and Interplanetary Dynamics , 1980 , pp. 217 - 221
Copyright
Copyright © Reidel 1980 

References

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