Actions for The Propagation of Solar Energetic Particles in Magnetic Channels

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The Propagation of Solar Energetic Particles in Magnetic Channels

Author
Mcdonald, F. B.
Published
Aug 1, 1985.
Physical Description
1 electronic document
Additional Creators
Burlaga, L. F.
Online Version

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Summary
The existence of interplanetary flow systems produced by the entrainment of interplanetary transients, consisting of flare produced shocks, high speed solar wind streams and coronal mass ejection, has been established. This entrainment process produces enhanced regions of the interplanetary magnetic field that should be connected back to the solar corona. These compressed regions can provide a preferred magnetic channel for the propagation of solar cosmic rays. The characteristics of these events appear to be different from those previously reported by the NASA/University of New Hampshire team and the University of Chicago in their study of a large number of events in the region beyond 1 AU. These new events have a very flat energy spectra (with gamma = approx. 1.5) that frequently extend to energies above 100 MeV and have a significant enhancement of MeV electrons.
Other Subject(s)
Collection
NASA Technical Reports Server (NTRS) Collection.
Note
Document ID: 19850026507.
Accession ID: 85N34820.
SH-3.2-4.
19th Intern. Cosmic Ray Conf - Vol. 4; p 346; NASA-CP-2376-VOL-4.
Terms of Use and Reproduction
No Copyright.
View MARC record | catkey: 16201289