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The “weak” r-process in core-collapse supernovae

Published online by Cambridge University Press:  23 December 2005

Shinya Wanajo  and
Yuhri Ishimaru
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 email: wanajo@resceu.s.u-tokyo.ac.jp
Yuhri Ishimaru
Affiliation:
Academic Support Center, Kogakuin University, 2665-1 Nakano-cho, Hachioji, Tokyo 192-0015, Japan email: kt13121@ns.kogakuin.ac.jp
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Abstract

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While the origin of r-process nuclei remains a long-standing mystery, recent spectroscopic studies of extremely metal-poor stars in the Galactic halo strongly suggest that it is associated with core-collapse supernovae. In addition, recent comprehensive analysis of such stars implies the presence of the “weak” r-process that is responsible for only lighter nuclei with A <130. In this study, we show that the weak r-process nuclei can be produced in the neutrino winds from a typical proto-neutron star of $1.4 M_\odot$. This suggests that the significant fraction of weak r-process elements (Sr, Y, Zr, etc.) originate from typical core-collapse supernovae with the progenitor mass range of ∼ 10–$20 M_\odot$

Keywords

nuclear reactionsnucleosynthesisabundances — supernovae: general
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. 435 - 438
Copyright
© 2005 International Astronomical Union