Formation of Balmer lines in the spectra of bright prominences. I - The calculation method

Details Formation of Balmer lines in the spectra of bright prominences. I - The calculation method Formation of Balmer lines in the spectra of bright prominences. I - The calculation method

Oct 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979velen......103s&link_type=abstract

Leningradskii Universitet, Vestnik, Matematika, Mekhanika, Astronomiia, Oct. 1979, p. 103-109. In Russian.

Other

Balmer Series, Solar Prominences, Solar Spectra, Integral Equations, Iterative Solution, Radiative Transfer, Solar Granulation

Scientific paper

An iterative method is proposed for determining the hydrogen atom populations and Balmer line profiles of solar prominences. The prominences are represented as plane layers perpendicular to the photosphere, and the electron temperature and density are assumed to be constant. Photospheric radiation is described by the Planck function with superposed Balmer line profiles. The radiative transfer equations are solved exactly in the Balmer lines and approximately in other series.

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