The diffusion of hydrogen radiation in prominences

Details The diffusion of hydrogen radiation in prominences The diffusion of hydrogen radiation in prominences

Oct 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979azh....56.1037i&link_type=abstract

Astronomicheskii Zhurnal, vol. 56, Sept.-Oct. 1979, p. 1037-1041. In Russian.

Astronomy and Astrophysics

Astronomy

Diffuse Radiation, Diffusion Theory, H Lines, Solar Prominences, Balmer Series, Computerized Simulation, Electron Density (Concentration), Integral Equations, Optical Thickness, Resonance Scattering, Solar Spectra, Spectral Energy Distribution

Scientific paper

The mutually dependent integral equations for the diffusion of H alpha, H beta, H gamma, P alpha, P beta and B alpha line radiation in a vertical slab in the solar radiation field are solved by a computer method using the Fourier representation of the unknown source functions. Expressions for the electron concentration and the populations of the third, fourth and fifth quantum levels of the hydrogen atom as a function of optical depth are used to obtain an integral source function, which is determined in the form of a Fourier series. It is found that the populations of the fourth and fifth levels remain constant while the population of the third level increases towards the center of the prominence, and comparisons with the predictions of a two-level model reveal the effects of level interdependences in increasing the population of the third level and decreasing those of the fourth and fifth. It is also concluded that the first Balmer line emissions of prominences are due to quasi-resonance scattering of photospheric radiation.

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