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Paper: Hot Subdwarf Stars and the ZAHeMS
Volume: 481, 6th Meeting on Hot Subdwarf Stars and Related Objects
Page: 225
Authors: Brown, D.
Abstract: The precise evolutionary mechanism for the production of hot subdwarf stars remains unsolved, though there are many plausible explanations. One general group of hypotheses proposes that sdB/EHB stars are the result of various processes typical of their single-star progeny, quite possibly very much affected by chemical environment and stellar wind mass loss. An alternative set of hypothesis proposes that such hot subdwarf/EHB objects are the result of binary interactions. Following the methodology of Han et al. (2002, 2003) in their binary population synthesis study of the evolutionary channels of sdB stars in the Galactic field for Z=0.02, this study has conducted a binary population synthesis investigation at various metallicities in order to examine the production of hot subwarf stars in different environments. Although it is found that metallicity is not a major factor in the production of such helium burning stars, there are a number of second-order effects. Results yield some hot subdwarf stars placed in areas below the ZAHeMS (in the log10g,log10 Teff diagram) which could give some information on the production of low-mass sdBs.
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