Article contents
The Formation of Carbon Stars in the Magellanic Clouds from Mass Transfer in Close Binaries
Published online by Cambridge University Press: 25 May 2016
Abstract
The presence of the carbon stars in the MC with luminosities higher or lower than predicted for thermally-pulsing (TP) AGB stars, can be explained by processes that happen during the early AGB (E–AGB) stage. I examine this assumption by means of a population simulation technique. I find that there must be TP–AGB C and S stars in the MC that formed as a result of mass transfer in binary systems. Their presence may influence the age determinations of MC clusters.
- Type
- Part 5. Stellar Populations and Surveys
- Information
- Symposium - International Astronomical Union , Volume 190: New Views of the Magellanic Clouds , 1999 , pp. 381 - 382
- Copyright
- Copyright © Astronomical Society of the Pacific 1999
References
- 1
- Cited by