Helium-Rich Stellar Atmosphere Models for B Stars
نویسندگان
چکیده
منابع مشابه
Full evolutionary models for PG 1159 stars . Implications for the helium - rich O ( He ) stars .
Aims. We present full evolutionary calculations appropriate to post-AGB PG1159 stars for a wide range of stellar masses. Methods. We take into account the complete evolutionary stages of PG1159 progenitors starting from the Zero Age Main Sequence. We consider the two kinds of Born Again Scenarios, the very late thermal pulse (VLTP) and the late thermal pulse (LTP), that give rise to hydrogen-de...
متن کاملCombined Stellar Structure and Atmosphere Models for Massive Stars Ii. Spectral Evolution on the Main Sequence
In Schaerer et al. (1995, Paper I) we have presented the rst \combined stellar structure and atmosphere models" (CoStar) for massive stars, which consistently treat the entire mass loosing star from the center out to the outer region of the stellar wind. The models use up-to-date input physics and state-of-the-art techniques to model both the stellar interior and the spherically expanding non{L...
متن کاملCombined stellar structure and atmosphere models for massive stars III. Spectral evolution and revised ionising fluxes of O3–B0 stars
We provide an extensive set of theoretical spectral energy distributions of massive stars derived from our “combined stellar structure and atmosphere models”. The calculations cover the entire main sequence evolution for initial masses Mi = 20 – 120 M⊙, corresponding to O3–B0 stars of all luminosity classes. We predict detailed line blanketed UV spectra along the main sequence evolution. The ma...
متن کاملCombined stellar structure and atmosphere models for massive stars III. Spectral evolution and revised ionizing fluxes of O3-B0 stars
We provide an extensive set of theoretical spectral energy distributions of massive stars derived from our “combined stellar structure and atmosphere models”. The calculations cover the entire main sequence evolution for initial masses Mi = 20 – 120M , corresponding to O3–B0 stars of all luminosity classes. We predict detailed line blanketed UV spectra along the main sequence evolution. The maj...
متن کاملOn the helium stratification in the atmosphere of magnetic helium peculiar stars
High resolution spectra of the Hei587.6, 667.8 706.5 and 728.1 nm lines have been obtained to test the prediction (notably by Vauclair et al. 1991) that helium abundance should decrease with depth in helium rich stars and increase in helium weak stars. A sample of B-type main sequence stars, with expected solar abundances and non stratified atmospheres, have also been observed in order to compa...
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ژورنال
عنوان ژورنال: International Astronomical Union Colloquium
سال: 1985
ISSN: 0252-9211
DOI: 10.1017/s0252921100090886