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Chemical evolution of the Galactic halo and the Origin of Precious Metals

Published online by Cambridge University Press:  23 December 2005

Yuhri Ishimaru ,
Shinya Wanajo ,
Wako Aoki ,
Sean G. Ryan  and
Nikos Prantzos
Yuhri Ishimaru
Affiliation:
Academic Support Center, Kogakuin University, 2665-1 Nakano-cho, Hachioji, Tokyo 192-0015, Japan email: kt13121@ns.kogakuin.ac.jp
Shinya Wanajo
Affiliation:
Research Center for the Early Universe, Graduate School of Science, University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-8654, Japan
Wako Aoki
Affiliation:
National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
Sean G. Ryan
Affiliation:
Department of Physics and Astronomy, The Open University, Milton Keynes, UK
Nikos Prantzos
Affiliation:
Institut d'Astrophysique de Paris, 98 bis, Boulevard Arago, 75014, Paris, France
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Abstract

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Observed large scatters in abundances of neutron-capture elements in metal-poor stars may suggest incomplete mixing of the interstellar medium at the beginning of the Galaxy. Comparing predictions by an inhomogeneous chemical evolution model and new observational results with Subaru HDS, we attempt to constrain the origins of r-process elements.

Keywords

Nuclear reactionsnucleosynthesisabundancesstars: abundancesGalaxy: evolutionGalaxy: halo
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 1 , Symposium S228: From Lithium to Uranium: Elemental Tracers of Early Cosmic Evolution , May 2005 , pp. 489 - 490
Copyright
© 2005 International Astronomical Union