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 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.
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...
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ژورنال
عنوان ژورنال: Symposium - International Astronomical Union
سال: 1997
ISSN: 0074-1809
DOI: 10.1017/s0074180900116833