منابع مشابه
Evolution of the Most Massive Stars
We discuss the physics of the ΩΓ– Limit, i.e. when the star is unbound as a result of both rotation and radiation pressure. We suggest that the ΩΓ– Limit is what makes the Humphreys–Davidson Limit. Stellar filiations are discussed, with an emphasis on the final stages, in particular on the final masses, their angular momentum and the chemical yields with account of rotation. A possible relation...
متن کاملEvolution of Collisionally Merged Massive Stars
We investigate the evolution of collisionally merged stars with mass of ∼ 100M⊙ which might be formed in dense star clusters. We assumed that massive stars with several tens M⊙ collide typically after ∼ 1Myr of the formation of the cluster and performed hydrodynamical simulations of several collision events. Our simulations show that after the collisions, merged stars have extended envelopes an...
متن کاملHydrodynamics of Supernova Evolution in the Winds of Massive Stars
Core-Collapse supernovae arise from stars greater than 8 M⊙. These stars lose a considerable amount of mass during their lifetime, which accumulates around the star forming wind-blown bubbles. Upon the death of the star in a spectacular explosion, the resulting SN shock wave will interact with this modified medium. We study the evolution of the shock wave, and investigate the properties of this...
متن کاملThe Evolution of Surface Parameters of Rotating Massive Stars
We summarize the present status of the predictions of massive star models for the evolution of their surface properties. After discussing luminosity, temperature and chemical composition, we focus on the question whether massive stars may arrive at critical rotation during their evolution, either on the main sequence or in later stages. We find both cases to be possible and briefly discuss obse...
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ژورنال
عنوان ژورنال: Proceedings of the International Astronomical Union
سال: 2006
ISSN: 1743-9213,1743-9221
DOI: 10.1017/s1743921307010228