2008/04/01 by Georges Meynet, Sylvia Ekstrom, Sylvia Ekström +4
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics and Star Formation Studies #Background radiation #Interstellar medium #Rotation (mathematics) #Solar mass #Star (game theory) #Stars #Stellar evolution #Stellar, planetary, and galactic studies #Universe #astro-ph
paper · pdf · doi:10.1017/s1743921308023119
11 pages, 7 figures, IAU Symp. 252, L. CUP, Deng, K.L. Chan, C. Chiosi, eds
openalex publication_date 2008/04/01 · arxiv created 2008/06/25 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
Abstract Mass loss and axial rotation are playing key roles in shaping the evolution of massive stars. They affect the tracks in the HR diagram, the lifetimes, the surface abundances, the hardness of the radiation field, the chemical yields, the presupernova status, the nature of the remnant, the mechanical energy released in the interstellar medium, etc. . . In this paper, after recalling a few characteristics of mass loss and rotation, we review the effects of these two processes at different metallicities. Rotation probably has its most important effects at low metallicities, while mass loss and rotation deeply affect the evolution of massive stars at solar and higher than solar metallicities.