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Current Understanding of the Physics of Type III Solar Radio Bursts

Published online by Cambridge University Press:  14 August 2015

K. Papadopoulos
K. Papadopoulos*
Affiliation:
Science Applications, Inc., 8400 Westpark Drive, McLean, Virginia 22102
*
*Permanent address: Department of Astronomy, University of Maryland, College Park, Md. 20742.

Abstract

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One of the most exciting plasma physics investigations of the recent years has been connected with the understanding of a new strong turbulent plasma state excited by propagating electron beams. This new state is initiated on the linear level by parametric instabilities (OTS, modulational, etc.) and results in a very dynamic state composed of collective clusters of modes called solitons, cavitons, spikons, etc. Introduction of these concepts to the classic beam plasma interaction problem has rendered quasilinear and weak turbulence theories inapplicable over most of the interesting parameter range, and helped explain many paradoxes connected with the propagation of beams in the laboratory and space. Following a brief review of these non-linear notions, we demonstrate how their application to type III solar radiobursts has revolutionized our understanding of their propagation, radio-emission and scaling properties and has guided the in situ observations towards a more complete understanding. A particular burst (May 16, 1971) is analyzed in detail and compared with numerical predictions.

Type
Session V - Solar Bursts - Meter-Decameter Wavelengths
Information
Symposium - International Astronomical Union , Volume 86: Radio Physics of the Sun , 1980 , pp. 287 - 297
Copyright
Copyright © Reidel 1980 

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