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Chemodynamical evolution of galaxies with hypernovae

Published online by Cambridge University Press:  01 July 2007

Chiaki Kobayashi
Chiaki Kobayashi*
Affiliation:
National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka-shi, Tokyo 181-8588, Japan; email: chiaki@th.nao.ac.jp
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Abstract

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We simulate the formation and evolution of galaxies with a hydrodynamical model including supernova and hypernova feedback. The large contribution of hypernovae is required from the observed abundance ratios in the Milky Way Galaxy. The hypernova feedback suppress star formation efficiently, which results in the cosmic star formation rate history peaked at z ~ 4. It also drives galactic outflows efficiently in low mass galaxies, and these winds eject heavy elements into the intergalactic medium. The ejected baryon and metal fraction is larger for less massive galaxies, which results in the mass-metallicity relation of galaxies. We also simulate the chemodynamical evolution of the Milky Way Galaxy, and show the difference of the stellar populations in the bulge and disk.

Keywords

galaxies: abundancesgalaxies: evolutionmethods: n-body simulations
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S245: Formation and Evolution of Galaxy Bulges , July 2007 , pp. 23 - 26
Copyright
Copyright © International Astronomical Union 2008

References

Kobayashi, C., 2004, MNRAS, 347, 740CrossRefGoogle Scholar
Kobayashi, C., Springel, V., & White, S. D. M. 2007, MNRAS, 376, 1465 (K07)Google Scholar
Kobayashi, C., Umeda, H., Nomoto, K., Tominaga, N., & Ohkubo, T. 2006, ApJ, 653, 1145Google Scholar