Astronomy and Astrophysics – Astrophysics
Scientific paper
2006-08-26
Astrophys.SpaceSci.306:33-39,2006
Astronomy and Astrophysics
Astrophysics
7 pages, 6 figures, Accepted for publication in Astrophysics and Space Science
Scientific paper
10.1007/s10509-006-9229-2
The supernova yields of r-process elements are obtained as a function of the mass of their progenitor stars from the abundance patterns of extremely metal-poor stars on the left-side [Ba/Mg]-[Mg/H] boundary with a procedure proposed by Tsujimoto and Shigeyama. The ejected masses of r-process elements associated with stars of progenitor mass $M_{ms}\leq18M_{\odot}$ are infertile sources and the SNe II with 20$M_{\odot}\leq M_{ms}\leq 40M_{\odot}$are the dominant source of r-process nucleosynthesis in the Galaxy. The ratio of these stars 20$M_{\odot}\leq M_{ms}\leq40M_{\odot}$ with compared to the all massive stars is about $\sim$18%. In this paper, we present a simple model that describes a star's [r/Fe] in terms of the nucleosynthesis yields of r-process elements and the number of SN II explosions. Combined the r-process yields obtained by our procedure with the scatter model of the Galactic halo, the observed abundance patterns of the metal-poor stars can be well reproduced
Chen Yan-Ping
Chen Zhe
Cui Wen-Yuan
Zhang Bo
Zhang Jiang
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