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 کاملPresupernova Evolution of Rotating Massive Stars I: Numerical Method and Evolution of the Internal Stellar Structure
The evolution of rotating stars with zero-age main sequence (ZAMS) masses in the range 8M⊙ to 25M⊙ is followed through all stages of stable evolution. The initial angular momentum is chosen such that the star’s equatorial rotational velocity on the ZAMS ranges from zero to ∼ 70% of break-up. The stars rotate rigidly on the ZAMS as a consequence of angular momentum redistribution during the pre-...
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 کاملThe Evolution of Supernovae in the Winds of Massive Stars
We study the evolution of supernova remnants in the circumstellar medium formed by mass loss from the progenitor star. The properties of this interaction are investigated, and the specific case of a 35 M⊙ star is studied in detail. The evolution of the SN shock wave in this case may have a bearing on other SNRs evolving in wind-blown bubbles, especially SN 1987A.
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ژورنال
عنوان ژورنال: Progress of Theoretical Physics
سال: 1959
ISSN: 0033-068X
DOI: 10.1143/ptp.21.315