The s-PROCESS Nucleosynthesis in Massive Metal-Poor Stars

Details The s-PROCESS Nucleosynthesis in Massive Metal-Poor Stars The s-PROCESS Nucleosynthesis in Massive Metal-Poor Stars

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005omeg.conf..197i&link_type=abstract

ORIGIN OF MATTER AND EVOLUTION OF GALAXIES 2003. Held 17-19 November 2003 in RIKEN, Wako, Saitama, Japan. Edited by M Terasawa,

Physics

Scientific paper

We present the s-process nucleosynthesis in massive stars with a wide range of metallicity, using the recent sets of reaction rates and stellar input physics. The decreasing metallicity makes poisoning effects of primary 16O larger at the late phase of core He burning, at which the s-process occurs actively in solar metallicity stars, and prevents the synthesis of heavy elements from being efficient. However, we find that the s-process proceeds very efficiently via neutron source reaction of 13C(α,n)16O at the end of core H burning phase when the metallicity decreases below Z ~ 10-8. These massive, extremely low metallicity stars may have an important contribution of light s-elements to observed extremely metal-poor stars.

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