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An Interpretation of the Millisecond Time Variation in Hard X-Ray Solar Flares

Published online by Cambridge University Press:  04 August 2017

V. Krishan  and
M. R. Kundu
V. Krishan
Affiliation:
Indian Institute of Astrophysics, Bangalore 560034, India
M. R. Kundu
Affiliation:
Astronomy Program, University of Maryland College Park, Maryland, USA 20742

Abstract

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Recent observations of the fast time variability in the hard X-ray emission from solar flares are interpreted. The fast spikes are assumed to be superimposed on the thermal X-ray emission. The rise and fall of a spike are caused by disruptions in the plasma. The rise time represents the impulsive heating time and the decay or fall time represents a quick cooling of the plasma due to the accelerating growth rate of the m=1 tearing mode. The estimated characteristic time durations of the spike are found to be in good agreement with the observed ones.

Type
Session IV
Information
Symposium - International Astronomical Union , Volume 107: Unstable Current Systems and Plasma Instabilities , 1985 , pp. 299 - 301
Copyright
Copyright © Reidel 1985 

References

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