Chemical abundances of $β$ Cephei stars from low- and high-resolution UV spectra
| dc.creator | Daszy{ń}ska-Daszkiewicz, Jadwiga | |
| dc.creator | Niemczura, Ewa | |
| dc.date | 2004-01-02 | |
| dc.date.accessioned | 2026-07-07T02:11:46Z | |
| dc.date.available | 2026-07-07T02:11:46Z | |
| dc.description | 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 $κ$ mechanism drives pulsations of $β$ 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, $θ$) and interstellar extinction, $E(B-V)$, for all $β$ 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 $β$ Cep star: $γ$ Peg. | |
| dc.description | 4 pages, 2 figures, to appear in Proceedings of IAU Colloquium 193, Variable Stars in the Local Group, ASP Conf. Ser., eds. D. W. Kurtz & K. Pollard | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0401009 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0401009 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/7215 | |
| dc.subject | Astrophysics | |
| dc.title | Chemical abundances of $β$ Cephei stars from low- and high-resolution UV spectra | |
| dc.type | text |