Chemical abundances of $β$ Cephei stars from low- and high-resolution UV spectra

Details Chemical abundances of $β$ Cephei stars from low- and high-resolution UV spectra Chemical abundances of $β$ Cephei stars from low- and high-resolution UV spectra

2004-01-02

arxiv.org/abs/astro-ph/0401009v1

Astronomy and Astrophysics

Astrophysics

4 pages, 2 figures, to appear in Proceedings of IAU Colloquium 193, Variable Stars in the Local Group, ASP Conf. Ser., eds. D.

Scientific paper

In early type stars the ultraviolet spectral region is important for several reasons. Firstly, since the majority of the total flux is emitted here, it provides a rather sensitive indicator of a photospheric temperature and luminosity. Secondly, the UV spectra are dominated by lines of the iron-group elements, which cause the origin of the opacity bump at temperature $2 \times 10^5$ K, where the classical $\kappa$ mechanism drives pulsations of $\beta$ Cep stars. Consequently, the position of the instability domain in the HR diagram strongly depends on the metal abundance (Pamyatnykh 1999). We derive stellar parameters (metallicity, [m/H], effective temperature, $T_{\rm eff}$, stellar diameter, $\theta$) and interstellar extinction, $E(B-V)$, for all $\beta$ Cep stars observed by {\it International Ultraviolet Explorer} satellite. The parameters are derived by means of an algorithmic procedure of fitting theoretical flux distributions to the low-resolution IUE spectra and optical spectrophotometric observations. The errors are estimated by using the bootstrap method (Press et al. 1992). We also show some examples of high-resolution HST/GHRS spectra for one $\beta$ Cep star: $\gamma$ Peg.

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