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Spatial and temporal evolution of soft and hard X-ray emission in a solar flare

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Abstract

We study the spatial and temporal characteristics of the 3.5 to 30.0 keV emission in a solar flare on April 10, 1980. The data were obtained by the Hard X-ray Imaging Spectrometer aboard the Solar Maximum Mission Satellite. It is complemented in our analysis with data from other instruments on the same spacecraft, in particular that of the Hard X-ray Burst Spectrometer.

Key results of our investigation are: (a) Continuous energy release is needed to substain the increase of the emission through the rising phase of the flare, before and after the impulsive phase in hard X-rays. The energy release is characterized by the production of hot (5 × 107 ≲ T ≲ 1.5 × 108 K) thermal regions within the flare loop structures. (b) The observational parameters characterizing the impulsive burst show that it is most likely associated with non-thermal processes (particle acceleration). (c) The continuous energy release is associated with strong chromospheric evaporation, as evidenced in the spectral line behavior determined from the Bent Crystal Spectrometer data. Both processes seem to stop just before flare maximum, and the subsequent evolution is most likely governed by the radiative cooling of the flare plasma.

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Authors and Affiliations

  1. Observatorio de Física Cósmica - CNIE, 1663, San Miguel, Argentina

    Marcos E. Machado

  2. Space Research Laboratory of the Astronomical Institute at Utrecht, Utrecht, The Netherlands

    André Duijveman

  3. Laboratory for Astronomy and Solar Physics, NASA Goddard Space Flight Center, Greenbelt, Maryland, U.S.A.

    Brian R. Dennis

Authors
  1. Marcos E. Machado
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  2. André Duijveman
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  3. Brian R. Dennis
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Machado, M.E., Duijveman, A. & Dennis, B.R. Spatial and temporal evolution of soft and hard X-ray emission in a solar flare. Sol Phys 79, 85–106 (1982). https://doi.org/10.1007/BF00146975

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  • DOI: https://doi.org/10.1007/BF00146975

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