A self-consistent interpretation of the solar flare extreme-ultraviolet to hard X-ray ratio in large events

Details A self-consistent interpretation of the solar flare extreme-ultraviolet to hard X-ray ratio in large events A self-consistent interpretation of the solar flare extreme-ultraviolet to hard X-ray ratio in large events

Mar 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...326..997l&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 326, March 15, 1988, p. 997-1001.

Astronomy and Astrophysics

Astrophysics

18

Electron Beams, Electron Bombardment, Solar Flares, Solar Magnetic Field, Ultraviolet Spectra, X Ray Spectra, H Alpha Line, High Resolution, Line Shape, Nonthermal Radiation, Ohmic Dissipation, Solar Corona, Solar Maximum Mission

Scientific paper

This paper shows quantitatively that when a limiting X-ray yield is considered, a universal area of 10 to the 17th sq cm used in the thick-target electron bombardment model of McClymont and Canfield (1986) cannot explain the observed hard X-ray flux in large solar flare events without recourse to extreme values of the physical parameters of the flaring corona. The return current ohmic heating produced by a beam of flux 10 to the 13th ergs/sq cm/s results in a coronal temperature in excess of 100 million K. In this case, the thermal hard X-ray emission dominates the nonthermal emission and the EUV-to-hard X-ray ratio would not decrease with increasing hard X-ray flux, as observed. Hence, any model that requires a beam flux of 10 to the 13th ergs/sq cm/s is untenable. It is proposed that these apparently contradictory results can be reconciled if the X-ray emitting area is substantially larger than the area of the chromospheric precipitation site.

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