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Galactic archeology with extremely metal-poor stars

Published online by Cambridge University Press:  01 June 2008

Yutaka Komiya ,
Takuma Suda ,
Asao Habe  and
Masayuki Fujimoto
Yutaka Komiya
Affiliation:
Department of Astronomy, Faculty of Science, Tohoku University, Sendai, Miyagi Prefecture 980-8578, Japan email: [email protected]
Takuma Suda
Affiliation:
Department of Cosmosciences, Hokkaido University, Sapporo, Hokkaido 060-0810, Japan
Asao Habe
Affiliation:
Department of Cosmosciences, Hokkaido University, Sapporo, Hokkaido 060-0810, Japan
Masayuki Fujimoto
Affiliation:
Department of Cosmosciences, Hokkaido University, Sapporo, Hokkaido 060-0810, Japan
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Abstract

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Extremely metal-poor (EMP) stars are thought to be formed in the low-mass protogalaxies as building blocks of the Milky Way and can be probes to investigate the early stage of galaxy formation and star formation in the early universe. We study the formation history of EMP stars in the Milky Way halo using a new model of chemical evolution based on the hierarchical theory of the galaxy formation. We construct the merging history of the Milky Way halo based on the extended Press-Schechter formalism, and follow the star formation and chemical evolution along the merger tree. The abundance trends and number of low-mass stars predicted in our model are compared with those of observed EMP stars. Additionally, in order to clarify the origin of hyper metal poor stars, we investigate the change of the surface metal abundances of stars by accretion of interstellar matter. We also investigate the pre-enrichment of intergalactic matter by the first supernovae.

Keywords

stars: abundances(stars:) binaries: generalstars: chemically peculiarstars: formationstars: luminosity functionstars: mass function
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Issue S255: Low-Metallicity Star Formation: From the First Stars to Dwarf Galaxies , June 2008 , pp. 330 - 335
Copyright
Copyright © International Astronomical Union 2008

References

Abel, T, Bryan, G. L., & Norman, M. L. 2002, Science, 295, 93CrossRefGoogle Scholar
Aoki, W., Beers, T. C., Christlieb, N., Norris, J. E., Ryan, S. G., & Tsangarides, S. 2007 ApJ, 655, 492CrossRefGoogle Scholar
Beers, T. C., Preston, G. W., & Shectman, S. A. 1992, AJ, 103, 1987CrossRefGoogle Scholar
Beers, T. C., Christlieb, N., Norris, J. E., Bessell, M. S., Wilhelm, R., Allende, P. A., Yanny, B., Rockosi, C., Newberg, H. J., Rossi, S., & Lee, Y. S. 2005, Proc. IAUS 228, 175CrossRefGoogle Scholar
Bond, J. R., Cole, S., Efstathiou, G., & Kaiser, N. 1991, ApJ, 379, 440CrossRefGoogle Scholar
Christlieb, N., Green, P. J., Wisotzki, L., & Reimers, D. 2001, A&A, 375, 366Google Scholar
Christlieb, N., Bessell, M. S., Beers, T. C., Gustafsson, B., Korn, A., Barklem, P. S., Karlsson, T., Mizuno-Wiedner, M., Rossi, S. 2002, Nature, 419, 904–906CrossRefGoogle Scholar
Frebel, A., Aoki, W., Christlieb, N., et al. 2005, Nature 434, 871–873CrossRefGoogle Scholar
Fujimoto, M. Y., Sugiyama, K., Iben, I. Jr., & Hollowell, D. 1995, ApJ, 444, 175CrossRefGoogle Scholar
Fujimoto, M. Y., Ikeda, Y., & Iben, I. Jr. 2000, ApJ, 529, L25CrossRefGoogle Scholar
Karlsson, 2006, A&AGoogle Scholar
Karlsson, 2006, ApJl, 641, L41CrossRefGoogle Scholar
Komiya, Y., Suda, T., Minaguchi, H., Shigeyama, T., Aoki, W., & Fujimoto, Y. M. 2006 ApJ 658, 367CrossRefGoogle Scholar
Komiya, Y., Suda, T., & Fujimoto, Y. M. 2008 ApJ submitted.Google Scholar
Komiya, Y., Suda, T., Asao, H., & Fujimoto, Y. M. 2008, in preparation.Google Scholar
Lacey, C., & Cole, S. 1993, MNRAS, 262, 627CrossRefGoogle Scholar
Nishi, R., & Susa, H. 1999, ApJ, 523, L103CrossRefGoogle Scholar
Norris John, E., Christlieb, N., Korn, A. J., Eriksson, K., Bessell, M. S., Beers, Timothy, C., Wisotzki, L., Reimers, D. 2007 ApJ, 670, 774CrossRefGoogle Scholar
Salvadori, S., Schneider, R., & Ferrara, A. 2006, MNRAS, 381, 647CrossRefGoogle Scholar
Schaerer, D 2002, A&A, 382, 28Google Scholar
Somerville, R. S., & Kolatt, T. S. 1999, MNRAS, 305, 1CrossRefGoogle Scholar
Spite, M. et al. 2005, A&A, 430, 655Google Scholar
Suda, T., Aikawa, M., Machida, M. N., Fujimoto, M. Y., & Iben, I. Jr. 2004, ApJ, 611, 476CrossRefGoogle Scholar
Suda, T. et al. 2008, PASJ, in pressCrossRefGoogle Scholar
Tegmark, M., Silk, J., Rees, M. J., Blanchard, A., Abel, T., & Palla, F. 1997, ApJ, 474, 1CrossRefGoogle Scholar
Tumlinson, J. 2006, ApJ, 641, 1CrossRefGoogle Scholar
Tominaga, N., Umeda, H., & Nomoto, K. 2007, ApJ, 660, 516CrossRefGoogle Scholar
Umeda, H. & Nomoto, K. 2003, Nature, 422, 871CrossRefGoogle Scholar