Structure and spectrum of quiescent prominences. II - Hydrogen and helium spectra

Details Structure and spectrum of quiescent prominences. II - Hydrogen and helium spectra Structure and spectrum of quiescent prominences. II - Hydrogen and helium spectra

Dec 1976

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976apj...210..827h&link_type=abstract

Astrophysical Journal, vol. 210, Dec. 15, 1976, pt. 1, p. 827-835.

Astronomy and Astrophysics

Astrophysics

42

Abundance, Chromosphere, H Lines, Helium, Solar Prominences, Solar Spectra, Atmospheric Composition, Emission Spectra, Hydrogen, Solar Atmosphere, Solar Corona, Spectrum Analysis, Stellar Models

Scientific paper

Theoretical emission-line intensities for hydrogen and helium in models of quiescent prominences have been computed and are compared with the absolute intensities measured by Landman and Illing (1976). The models required to match the observations have electron temperatures in the range from 7500 to 9500 K and gas pressures equal to or slightly greater than the coronal value. The calculations indicate a probable lower limit of 0.05 to the helium-to-hydrogen number ratio for the prominence studied.

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