Formation of Balmer lines in the spectra of bright prominences. II - Results of calculations

Details Formation of Balmer lines in the spectra of bright prominences. II - Results of calculations Formation of Balmer lines in the spectra of bright prominences. II - Results of calculations

Jan 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980velen.......97s&link_type=abstract

Leningradskii Universitet, Vestnik, Matematika, Mekhanika, Astronomiia, Jan. 1980, p. 97-102. In Russian.

Physics

Balmer Series, Hydrogen Atoms, Solar Prominences, Electron Energy, H Alpha Line, Optical Thickness, Populations, Solar Activity, Solar Physics, Spectral Line Width

Scientific paper

In the present paper, a method proposed by Seliakov (1979) is applied to the calculation of the populations of hydrogen atom levels and Balmer line profiles of prominences. The calculations are carried out for optical thicknesses in the H-alpha line ranging from 1 to 40, electron temperatures ranging from 6000 to 10,000 K, and logarithmic electron densities from 9 to 11. It is shown that the electron density does not affect the observed spectral characteristics. The line halfwidths are defined only by the optical thickness, while the total intensities depend also on the electron temperature.

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