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Comparative study of the loss cone-driven instabilities in the low solar coronaA comparative study of the loss cone-driven instabilities in the low solar corona is undertaken. The instabilities considered are the electron cyclotron maser, the whistler, and the electrostatic upper hybrid. It is shown that the first-harmonic extraordinary mode of the electron cyclotron maser instability is the fastest growing mode for strong magnetized plasma (the ratio of plasma frequency to cyclotron frequency being less than 0.35). For values of the ratio between 0.35 and 1.0, the first-harmonic ordinary mode of the electron cyclotron maser instability dominates the emission. For ratio values greater than 1.0, no direct electromagnetic radiation is expected since other instabilities, which do not escape directly, saturate the electron cyclotron maser (the whistler or the electrostatic upper hybrid waves). It is also shown that the second-harmonic electron cyclotron maser emission never grows to an appreciable level. Thus, it is suggested that the electron cyclotron maser instability can be the explanation for the escape of the first harmonic from a flaring loop.
Document ID
19840053059
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Sharma, R. R. (Maryland Univ. College Park, MD, United States)
Vlahos, L. (Maryland, University College Park, MD, United States)
Date Acquired
August 12, 2013
Publication Date
May 1, 1984
Publication Information
Publication: Astrophysical Journal, Part 1
Volume: 280
ISSN: 0004-637X
Subject Category
SOLAR PHYSICS
Funding Number(s)
CONTRACT_GRANT: NAGW-81
Distribution Limits
Public
Copyright
Other