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Chemical Evolution of R-process Elements in the Hierarchical Galaxy Formation

Published online by Cambridge University Press:  09 May 2016

Yutaka Komiya  and
Toshikazu Shigeyama
Yutaka Komiya
Affiliation:
Research center for the early universe, University of TokyoHongo, 7-3-1, Bunkyo-ku, Tokyo, 113-0033, Japan email: komiya@resceu.s.u-tokyo.ac.jp
Toshikazu Shigeyama
Affiliation:
Research center for the early universe, University of TokyoHongo, 7-3-1, Bunkyo-ku, Tokyo, 113-0033, Japan email: komiya@resceu.s.u-tokyo.ac.jp
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Abstract

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The main astronomical source of r-process elements has not yet been identified. One plausible site is neutron star mergers (NSMs). From the perspective of Galactic chemical evolution, however, it has been pointed out that the NSM scenario is incompatible with observations. Recently, Tsujimoto & Shigeyama (2014) pointed out that NSM ejecta can spread into much larger volume than ejecta from a supernova. We re-examine the chemical evolution of r-process elements under the NSM scenario considering this difference in propagation of the ejecta. We find that the NSM scenario can be compatible with the observed abundances of the Milky Way halo stars.

Keywords

stars: Population IInuclear reactionsnucleosynthesisabundancesGalaxy: evolutionGalaxy: halo
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , Issue S317: The General Assembly of Galaxy Halos: Structure, Origin and Evolution , August 2015 , pp. 318 - 319
Copyright
Copyright © International Astronomical Union 2016 

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