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Infrared hydrogen emission lines in the spectra of Be stars

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Abstract

For the interpretation of observed hydrogen emission lines in the spectrum of γ Cas calculations of the relative intensities of spectral lines of the Balmer, Paschen, Brackett and Pfund series are carried out, by using the theory of moving stellar envelopes.

It is shown that in the spectra of Be stars, which have opaque envelopes and therefore a slow Balmer decrement, infrared hydrogen lines must be relatively strong.

It is also found that the observed relative line intensities of γ Cas are in qualitative agreement with those calculated for the case of a simple model-envelope which consists of low and high opacity regions.

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Authors and Affiliations

  1. W. Struve Tartu Astrophysical Observatory, Tôravere, U.S.S.R.

    L. Luud & M. Ilmas

Authors
  1. L. Luud
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  2. M. Ilmas
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Luud, L., Ilmas, M. Infrared hydrogen emission lines in the spectra of Be stars. Astrophys Space Sci 40, 135–139 (1976). https://doi.org/10.1007/BF00651193

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  • DOI: https://doi.org/10.1007/BF00651193

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