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Acceleration, Transport of and Radiation by Electrons in Impulsive Phase of Flares

Published online by Cambridge University Press:  19 July 2016

Vahé Petrosian
Vahé Petrosian*
Affiliation:
Center for Space Science and Astrophysics and Department of Applied Physics Stanford University Stanford, CA 94305 USA

Abstract

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I review here results of works that we have carried out over the past few years in connection with various manifestations of the impulsive phase of solar flares. The primary goal of this work has been the determination of the characteristics of the accelerated electrons. We take into account various possible interactions that electrons suffer as they traverse the flare plasma and evaluate the expected radiation via several mechanisms. The comparison of these with the observed x-ray, gamma-ray and radio emissions allows us to set constraints on the characteristics of the accelerated electrons and on some properties of the flare plasma. I will describe some of the results we have derived from comparisons with SMM and other observations of flares during the past solar cycle. In particular, I will show that we can set limits on the range and distribution of the accelerated electron spectrum and pitch angle distribution, and on the column depth and field convergence rate of the flaring loop. More complete data and high spatial resolution and polarization observations could be very useful for furthering this kind of work.

Type
VIII. Solar Flares
Information
Symposium - International Astronomical Union , Volume 142: Basic Plasma Processes on the Sun , 1990 , pp. 391 - 402
Copyright
Copyright © Kluwer 1990 

References

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