Abstract
Using time-dependent numerical simulations and Solar Maximum Mission (SMM) observations of a solar flare on 1985 January 23, we examine the ability of an electron-beam-heated model to reproduce the rise phase of a flare as observed in soft X-ray lines of CaXIX. For a spectral index of 6, only models with a low-energy cutoff of 20 keV reproduce the observed peak emission in the CaXIX line complex. None of the models reproduces the temporal behavior of the soft X-ray emission.
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References
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© 1991 Springer-Verlag
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Mariska, J.T. (1991). Numerical simulations of electron-beam-heated solar flares. In: Uchida, Y., Canfield, R.C., Watanabe, T., Hiei, E. (eds) Flare Physics in Solar Activity Maximum 22. Lecture Notes in Physics, vol 387. Springer, Berlin, Heidelberg. https://doi.org/10.1007/BFb0032631
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DOI: https://doi.org/10.1007/BFb0032631
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