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Solar Second Harmonic Plasma Emission and the Head-on Approximation

Published online by Cambridge University Press:  25 April 2016

A. J. Willes ,
P. A. Robinson  and
D. B. Melrose
A. J. Willes
Affiliation:
Department of Theoretical Physics and Research Centre for Theoretical Astrophysics, School of Physics, University of Sydney, NSW 2006, Australia. a.willes@physics.usyd.edu.au
P. A. Robinson
Affiliation:
Department of Theoretical Physics and Research Centre for Theoretical Astrophysics, School of Physics, University of Sydney, NSW 2006, Australia. a.willes@physics.usyd.edu.au
D. B. Melrose
Affiliation:
Department of Theoretical Physics and Research Centre for Theoretical Astrophysics, School of Physics, University of Sydney, NSW 2006, Australia. a.willes@physics.usyd.edu.au
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Abstract

The coalescence of two Langmuir waves, L and L′, produces emission at twice the plasma frequency in type II and type III solar radio bursts. The analysis of the coalescence process is usually simplified by assuming the head-on approximation, where the wavevectors of the coalescing waves satisfy kL′ ≈ −kL, corresponding to the two Langmuir waves meeting head on. However, this is not always a valid approximation, particularly when the peak of the Langmuir spectrum lies at small wavenumbers, for narrow band spectra, and for spectra with broad angular ranges. Realistic Langmuir wave spectra are used to investigate the effects of relaxing the head-on approximation.

Keywords

radiation mechanismsnonthermal — Sunradio radiation — Suncorona
Type
Solar and Solar System
Information
Publications of the Astronomical Society of Australia , Volume 12 , Issue 2 , August 1995 , pp. 197 - 201
Copyright
Copyright © Astronomical Society of Australia 1995

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