Intensities of Balmer Emission Lines in Stellar Spectra

Details Intensities of Balmer Emission Lines in Stellar Spectra Intensities of Balmer Emission Lines in Stellar Spectra

Sep 1931

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1931phrv...38.1195s&link_type=abstract

Physical Review, vol. 38, Issue 6, pp. 1195-1204

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Scientific paper

Contours of the Balmer emission lines in the spectra of fourteen stars of spectral class Be have been measured on twenty-seven spectrograms. In many stars the lines are broad and flat-topped, with steep outer edges, while in others they are double. The contours are explained by Doppler effect caused by the rotation of a nebula surrounding the star. The mean relative total intensities are: β:γ:δ:ɛ=10:6.2:5.2:(5.4). The slow decrement in intensity agrees with the hypothesis that the bright lines are caused mostly by recombination. Lines produced in this way must be strongest (other things being equal) in a medium containing a maximum number of atoms of the next stage of ionization. This agrees with the observed strength of the emission lines of Fe II and of H in the earlier subdivisions of spectral class B.

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