Massive variable stars at very low metallicity?
نویسندگان
چکیده
منابع مشابه
Evolution of massive stars at very low metallicity including rotation and binary interactions
We discuss recent models on the evolution of massive stars at very low metallicity including the effects of rotation, magnetic fields and binarity. Very metal poor stars lose very little mass and angular momentum during the main sequence evolution, and rotation plays a dominant role in their evolution. In rapidly rotating massive stars, the rotationally induced mixing time scale can be even sho...
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At very low metallicity, the effects of differential rotation have a more important impact on the evolution of stars than at high metallicity. Rotational mixing leads to the production of great quantities of helium and of primary N by massive stars. Rotation induces important mass loss and allows stars to locally strongly enrich the interstellar medium in CNO elements. Stars formed from interst...
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Some indirect observations, as the high fraction of Be stars†at low metallicity, or the necessity for massive stars to be important sources of primary nitrogen, seem to indicate that very metal poor stars were fast rotators. As a consequence of this fast rotation, these stars, contrarily to current wisdom, might lose large amounts of mass during their lifetime. In this paper, we review various ...
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Mass loss plays a dominant role in the evolution of massive stars at solar metallicity. After discussing different mass loss mechanisms and their metallicity dependence, we present the possibility of strong mass loss at very low metallicity. Our models at Z = 10−8 show that stars more massive than about 60 M⊙ may lose a significant fraction of their initial mass in the red supergiant phase. Thi...
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Wind models of very massive stars with metallicities in a range from 10−4 to 1.0 solar are calculated using a new treatment of radiation driven winds with depth dependent radiative force multipliers and a comprehensive list of more than two million of spectral lines in NLTE. The models are tested by a comparison with observed stellar wind properties of O stars in the Galaxy and the SMC. Satisfy...
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ژورنال
عنوان ژورنال: Proceedings of the International Astronomical Union
سال: 2010
ISSN: 1743-9213,1743-9221
DOI: 10.1017/s1743921311010519