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EMP stars with high mass IMF and hierarchical galaxy formation

Published online by Cambridge University Press:  09 March 2010

Yutaka Komiya ,
Takuma Suda ,
Asao Habe  and
Masayuki Y. Fujimoto
Yutaka Komiya
Affiliation:
National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo, 181-8588, Japan
Takuma Suda
Affiliation:
Astrophysics Group, EPSAM, Keele University, Keele, Staffordshire ST5 5BG, UK
Asao Habe
Affiliation:
Department of Cosmoscience, Hokkaido University, Sapporo, Hokkaido 060-0810, Japan
Masayuki Y. Fujimoto
Affiliation:
Department of Cosmoscience, Hokkaido University, Sapporo, Hokkaido 060-0810, Japan
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Abstract

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Extremely metal-poor (EMP) stars in the Galactic halo are stars formed in the very early stage of the chemical evolution of the Galaxy. In previous study, we proposed that typical mass of EMP stars are massive, based on observations of carbon-enhanced EMP stars. In this study, we build a merger tree of the Galaxy semi-analytically and follow the chemical evolution along the merger tree. We also consider the effect of binary and high-mass initial mass function(IMF). Resultant theoretical metallicity distribution function (MDF) and abundance distribution are compared with observed metal-poor halo stars.

Keywords

stars: abundancesstars: Population IIGalaxy: evolutionGalaxy: halo
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S265: Chemical Abundances in the Universe: Connecting First Stars to Planets , August 2009 , pp. 128 - 129
Copyright
Copyright © International Astronomical Union 2010

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