The He II lines in the spectrum of zeta Puppis

Details The He II lines in the spectrum of zeta Puppis The He II lines in the spectrum of zeta Puppis

Sep 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975apj...200..634s&link_type=abstract

Astrophysical Journal, vol. 200, Sept. 15, 1975, pt. 1, p. 634-640.

Astronomy and Astrophysics

Astrophysics

12

Atmospheric Models, Early Stars, Helium Ions, Spectral Line Width, Stellar Atmospheres, Ultraviolet Spectra, Absorption Spectra, Astronomical Models, Hydrogen Atoms, Line Spectra, Mathematical Models, Molecular Rotation, O Stars, Stark Effect, Stellar Spectra, Thermodynamic Equilibrium

Scientific paper

The observed He II line spectrum in zeta Pup is compared with that predicted from model atmospheres in an attempt to establish the parameters (effective temperature, log g) which characterize the model that best represents this star's atmosphere. The study is conducted by compiling equivalent widths of the He II lines in the series (n = 2,3,4,5) and comparing them with predictions from plane-parallel static model atmospheres using a non-LTE theory of line formation. Good agreement between observation and prediction for a model atmosphere with an effective temperature of 50,000 K and log of 4.0 is found for the upper members of the n = 3 and n = 5 series, but discrepancies are found for the two lines of the n = 2 series and the upper members of the n = 4 series. It is shown that the n = 4 level appears to be more overpopulated at moderate atmospheric depths than the non-LTE calculations with plane-parallel layers indicate. It is suggested that this may be due to an overlap of the H and He II lines in the even-even series caused by macroturbulent velocities of the hydrogen and helium atoms.

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