The Helium Lines in Stellar Spectra

Details The Helium Lines in Stellar Spectra The Helium Lines in Stellar Spectra

Dec 1928

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1928natur.122..994s&link_type=abstract

Nature, Volume 122, Issue 3087, pp. 994-995 (1928).

Astronomy and Astrophysics

Astrophysics

7

Scientific paper

ALL the lines of neutral helium that can be observed in stellar spectra belong to some of the subordinate series. The ultimate lines (1S - mP) are in the far ultra-violet and cannot be photographed through the earth's atmosphere. The diffuse series of both the triplet system (2p3 - md3) and the singlet system (2P - mD) have nearly identical lower energy levels, the excitation potentials being 20.81 volts and 21.12 volts respectively (cf. H. N. Russell, Astroph. Jour., 61, 223; 1925). Accordingly, the corresponding lines of these two series should show identical intensity curves with respect to temperature, the intensity ratio of the triplet line to the singlet line remaining constant (cf. R. H. Fowler and E. A. Milne, Mon. Not. R.A.S., 83, 415; 1923).

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