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Far-UV radiation from hot subdwarf stars in early-type galaxies

Published online by Cambridge University Press:  05 March 2015

Zhanwen Han  and
Xuefei Chen
Zhanwen Han
Affiliation:
Key Laboratory for the Structure and Evolution of Celestial Objects, Yunnan Observatory, Kunming, 650011, China email: zhanwenhan@ynao.ac.cn, cxf@ynao.ac.cn
Xuefei Chen
Affiliation:
Key Laboratory for the Structure and Evolution of Celestial Objects, Yunnan Observatory, Kunming, 650011, China email: zhanwenhan@ynao.ac.cn, cxf@ynao.ac.cn
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Far-ultraviolet (FUV) excess is crucial to our understanding of early-type galaxies and it is widely believed that the FUV radiation originates mainly from hot subwarf stars. Hot subdwarf stars may form from binary interactions or from single star evolution. In the binary channel, a star near the tip of the first giant branch (FGB) may get its envelope removed by its companion via stable Roche lobe overflow or common envelope ejection, and then evolves to a hot subdwarf star (Han et al.2002, 2003, 2007). Such a process does not depend much on metallicity.

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 10 , Highlights H16: Highlights of Astronomy , August 2012 , pp. 124
Copyright
Copyright © International Astronomical Union 2015 

References

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