NASA NTRS · 19810046952
X-ray line widths and coronal heating
Abstract
Preliminary results of spectroscopy and imaging of a solar active region and flare plasma in soft X-ray emission lines are presented. Observed X-ray line widths in a nonflaring active region are broader than the Doppler width corresponding to the local electron temperature. An analysis of 41 soft X-ray flares within a single active region reveals a preference for flares to occur at locations that already show enhanced X-ray emission and to favor magnetic complexity over high gradient. However, flares do not appear to be directly responsible for the heating and X-ray production of the active regions.
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Acton, L. W., Wolfson, C. J., Joki, E. G., Culhane, J. L., Rapley, C. G., Bentley, R. D., Gabriel, A. H., Phillips, K. J. H., Hayes, R. W., Antonucci, E.. 1981-03-15. X-ray line widths and coronal heating. https://ntrs.nasa.gov/citations/19810046952
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