The Fe I and Fe II lines emission in solar flares.

Details The Fe I and Fe II lines emission in solar flares. The Fe I and Fe II lines emission in solar flares.

Oct 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989bsold..10...98b&link_type=abstract

Byulletin Solnechnye Dannye Akademie Nauk USSR, No. 1989/10, p. 98 - 103

Physics

Solar Flares: Iron, Solar Flares: Line Profiles, Solar Flares: Balmer Lines

Scientific paper

Two flare models are calculated which interpret the observed profiles of Balmer lines Hα, Hβ, Hδ and iron lines. It is shown that the models with a temperature increase only in the chromosphere (above the temperature minimum region) do not provide an agreement between theoretical and observed profiles of Balmer and iron lines. An agreement is achieved only for the models which have an increased temperature in the photospheric layers to the depth of N = 8×1023cm-2. A conclusion is made that the iron lines emission is present only in flares with deep penetration of the heating process. The Balmer lines of such flares have wide profiles with extended wings.

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