X-ray line widths and coronal heating

Details X-ray line widths and coronal heating X-ray line widths and coronal heating

Mar 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981apj...244l.137a&link_type=abstract

Astrophysical Journal, Part 2 - Letters to the Editor, vol. 244, Mar. 15, 1981, p. L137-L140. Research supported by the Lockheed

Astronomy and Astrophysics

Astrophysics

50

High Temperature Plasmas, Solar Corona, Solar Flares, Solar Maximum Mission, Solar Wind, Solar X-Rays, Spectral Line Width, Coronal Loops, Doppler Effect, Emission Spectra, X Ray Imagery, X Ray Spectroscopy

Scientific paper

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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