Abstract
Matsushita et al. (1992) used the Hard X-ray Telescope on board the Yohkoh satellite to image hard X-ray (HXR) emission in 100 impulsive flares, and found that low energy emission comes from higher in the corona than high energy emission. This confirmed observations by Takakura et al (1986) with the Hinotori imager. The HXR emission is thought to be bremsstrahlung of non-thermal electrons, but the observed heights are much greater than found in previous theoretical calculations. This led to speculation that a super-hot (< 108K) plasma was present in impulsive flare loop-tops. However, using a stochastic simulation of electron transport we show that the inferred height distribution can be explained by a non-thermal model.
This is a preview of subscription content, log in via an institution to check access.
Access this chapter
Tax calculation will be finalised at checkout
Purchases are for personal use only
Similar content being viewed by others
References
Fletcher, L.: 1996, Astron.Astrophys., in press
Gardiner, C.W.:1985 in H.Haken (ed.), Handbook of Stochastic Methods
MacKinnon, A.L. and Craig, I.J.D.:1991, Astron.Astrophys. 251, 693
Matsushita, K., Masuda, S., Kosugi, T., Inda, M. and Yaji, K.:1992, P.A.S.J/ 44. L89
van den Oord, G.H.J.: 1990, Astron.Astrophys. 234, 496n den Oord
Author information
Authors and Affiliations
Editor information
Editors and Affiliations
Rights and permissions
Copyright information
© 1996 Kluwer Academic Publishers
About this chapter
Cite this chapter
Fletcher, L. (1996). The Height Distribution of Hard X-Rays in Impulsive Solar Flares. In: Uchida, Y., Kosugi, T., Hudson, H.S. (eds) Magnetodynamic Phenomena in the Solar Atmosphere. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-0315-9_133
Download citation
DOI: https://doi.org/10.1007/978-94-009-0315-9_133
Publisher Name: Springer, Dordrecht
Print ISBN: 978-94-010-6627-3
Online ISBN: 978-94-009-0315-9
eBook Packages: Springer Book Archive