Physics
Scientific paper
Aug 1986
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986soph..106..315r&link_type=abstract
Solar Physics (ISSN 0038-0938), vol. 106, Aug. 1986, p. 315-333.
Physics
1
Balmer Series, H Lines, Paschen Series, Solar Prominences, Spectral Energy Distribution, Continuum Modeling, Equilibrium Equations, Stellar Models
Scientific paper
To calculate the Balmer, Paschen, and Brackett line intensities, the authors solved the statistical equilibrium equations for a twenty level plus continuum atom of hydrogen. The integrated line intensities from the Balmer series have been compared with the observations. To evaluate the influence of the pressure, the temperature, the thermal conduction coefficient and the turbulence velocity on the spectrum the results from different models are compared. It is concluded that only the lines arising from the lower levels up to 8 - 10 can give us information about the physical parameters that characterized the solar prominences since the intensities from the higher members of the series depend only on atomic properties because of the small departures from LTE of the upper levels involved.
Fontenla Juan Manuel
Rovira Marta G.
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