Analysis of the optical spectra of solar flares. IV - The 'blue' continuum of white light flares

Details Analysis of the optical spectra of solar flares. IV - The 'blue' continuum of white light flares Analysis of the optical spectra of solar flares. IV - The 'blue' continuum of white light flares

Nov 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985a%26a...152..165d&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 152, no. 1, Nov. 1985, p. 165-169. CNR-supported research.

Astronomy and Astrophysics

Astrophysics

19

Balmer Series, Solar Flares, Solar Spectra, Visible Spectrum, Emission Spectra, Spectral Line Width, Spectrum Analysis, Stark Effect

Scientific paper

The "blue" continuum emission at λ < 4000 Å of white light flares (WLF) has been interpreted as mainly due to the merging of the Stark broadened profiles of the highest Balmer lines. Stark profiles have been computed according to the deFeiter (1966) method, using the Griem (1962) asymptotic expressions for the electron broadening parameter. A homogeneous and isothermal model for the WLF has been used to compute a grid of emitted spectra; the NLTE hydrogen level populations are from deFeiter (1966). A satisfactory agreement between some computed spectra and those measured for the June 4, 1980 WLF has been found.

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