1-m spectroscopy of normal OB stars

Details 1-m spectroscopy of normal OB stars 1-m spectroscopy of normal OB stars

Jan 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999mnras.302..145c&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 302, Issue 1, pp. 145-151.

Astronomy and Astrophysics

Astronomy

7

Scientific paper

We have obtained spectra of 70 normal OB stars in the near-IR I (1-μm) band. The strongest features are those due to lines of the hydrogen Paschen series and neutral and ionized helium, which are, for the most part, in absorption. The information content in this spectral range is sufficient for only a rough classification of hot stars into `early O', `late O' and `B' types. Curiously, the leading He i triplet line, He i λ1.0830 μm, is usually not detectable, although in a few stars it is in emission; its behaviour generally correlates with the leading helium singlet line, He i λ 2.058 μ m. These two features appear to be present in emission only in stars with extremes of mass loss or wind extension.

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