The Height Distribution of Hard X-Rays in Impulsive Solar Flares

  • Lyndsay Fletcher

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.

Keywords

Stochastic Simulation Stochastic Differential Equation Loop Density High Energy Emission Previous Theoretical Calculation 
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References

  1. Fletcher, L.: 1996, Astron.Astrophys., in pressGoogle Scholar
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  3. MacKinnon, A.L. and Craig, I.J.D.:1991, Astron.Astrophys. 251, 693ADSGoogle Scholar
  4. Matsushita, K., Masuda, S., Kosugi, T., Inda, M. and Yaji, K.:1992, P.A.S.J/ 44. L89Google Scholar
  5. van den Oord, G.H.J.: 1990, Astron.Astrophys. 234, 496n den OordADSGoogle Scholar

Copyright information

© Kluwer Academic Publishers 1996

Authors and Affiliations

  • Lyndsay Fletcher
    • 1
  1. 1.Sterrenkundig InstituutUniversity of UtrechtUtrechtThe Netherlands

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