Stellar evolution with SMC chemical abundances
Abstract
Core hydrogen burning mass loss is taken into account in evolutionary computations for massive stars, of 20-100 solar masses, with chemical abundances of the Small Magellanic Cloud. After core hydrogen burning, models are considered for members of close binary systems and are followed during their Roche lobe overflow stage according to an early case B of mass transfer. During the core helium burning stage of the Roche lobe overflow, remnant mass loss rates comparable to those of WR stars are included in order to study WR star formation and evolution. Comparisons with similar galactic computations are included.
- Publication:
-
IAU Colloq. 59: Effects of Mass Loss on Stellar Evolution
- Pub Date:
- 1981
- DOI:
- 10.1007/978-94-009-8500-1_39
- Bibcode:
- 1981ASSL...89..279H
- Keywords:
-
- Abundance;
- B Stars;
- Magellanic Clouds;
- Mass Transfer;
- Stellar Evolution;
- Stellar Mass Ejection;
- Helium;
- Hertzsprung-Russell Diagram;
- Hydrogen;
- Stellar Winds;
- Astrophysics