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The Coalescence Instability in Solar Flares

Published online by Cambridge University Press:  04 August 2017

T. Tajima ,
F. Brunel ,
J.-I. Sakai ,
L. Vlahos  and
M. R. Kundu
T. Tajima
Affiliation:
University of Texas
F. Brunel
Affiliation:
University of Texas
J.-I. Sakai
Affiliation:
Toyama University and University of Maryland
L. Vlahos
Affiliation:
University of Maryland
M. R. Kundu
Affiliation:
University of Maryland

Abstract

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The non-linear coalescence instability of current carrying solar loops can explain many of the characteristics of the solar flares such as their impulsive nature, heating and high energy particle acceleration, amplitude oscillations of electromagnetic and emission as well as the characteristics of 2–D microwave images obtained during a flare. The plasma compressibility leads to the explosive phase of loop coalescence and its overshoot results in amplitude oscillations in temperatures by adiabatic compression and decompression. We note that the presence of strong electric fields and super–Alfvenic flows during the course of the instability play an important role in the production of non–thermal particles. A qualitative explanation on the physical processes taking place during the non–linear stages of the instability is given.

Type
Session III
Information
Symposium - International Astronomical Union , Volume 107: Unstable Current Systems and Plasma Instabilities , 1985 , pp. 197 - 210
Copyright
Copyright © Reidel 1985 

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