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Abundance Ratios of M82 and Nucleosynthesis of Hypernovae

Published online by Cambridge University Press:  26 May 2016

Hideyuki Umeda ,
Ken'ichi Nomoto ,
Takeshi Go Tsuru  and
Takayoshi Nakamura
Hideyuki Umeda
Affiliation:
Research Center for the Early Universe, School of Science, Univ. of Tokyo, Tokyo, Japan
Ken'ichi Nomoto
Affiliation:
Dept. of Astronomy, School of Science, Univ. of Tokyo, Tokyo, Japan
Takeshi Go Tsuru
Affiliation:
Research Center for the Early Universe, School of Science, Univ. of Tokyo, Tokyo, Japan
Takayoshi Nakamura
Affiliation:
Dept. of Astronomy, School of Science, Univ. of Tokyo, Tokyo, Japan

Abstract

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The abundance in M82 is Si and S rich, and can not be explained by the combination of conventional Type I and II supernova yields. We show that these abundance patterns, as well as the observed hot plasma energy to metal mass ratios can be explained by the hypernova nucleosynthesis. This hypothesis is consistent with the expected age after the star-burst of M82.

Type
Posters
Information
Symposium - International Astronomical Union , Volume 208: Astrophysical Supercomputing using Particle Simulations , 2003 , pp. 461 - 462
Copyright
Copyright © Astronomical Society of the Pacific 2003 

References

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