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The Formation of Carbon Stars in the Magellanic Clouds from Mass Transfer in Close Binaries

Published online by Cambridge University Press:  25 May 2016

Ju. Frantsman
Ju. Frantsman*
Affiliation:
Astronomical Institute, Latvian University, Raina Blvd. 19, Riga, LV-1586, LATVIA

Abstract

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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 

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