Soft X-ray diagnostics of electron-heated solar flare atmospheres

Details Soft X-ray diagnostics of electron-heated solar flare atmospheres Soft X-ray diagnostics of electron-heated solar flare atmospheres

Jun 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...341.1075l&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 341, June 15, 1989, p. 1075-1081.

Astronomy and Astrophysics

Astrophysics

53

Solar Atmosphere, Solar Flares, Solar X-Rays, Spectral Line Width, Atmospheric Heating, Calcium, Solar Electrons

Scientific paper

The dependence of the impulsive-phase Ca XIX w line profile on the form of the flare energy input (assumed to be due to the collisional degradation of a beam of high-energy electrons) is considered. The injected flux spectrum has the form of a power law with a low-energy 'knee', and the effects of varying the total energy flux, spectral index, and knee energy on the w line profile during the impulsive phase have been evaluated. Early in the burst, blueshifts of order 400 km/s are noted, and the peak intensity of the blueshifted component together with spatially unresolved hard X-ray burst spectra can be used to determine the beam filling factor.

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