The yields of r-process elements and chemical evolution of the Galaxy

Abstract

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 $M_{ms}\le 18M_{\odot }$ are infertile sources and the SNe II with 20$M_{\odot }\le M_{ms}\le 40M_{\odot }$are the dominant source of r-process nucleosynthesis in the Galaxy. The ratio of these stars 20$M_{\odot }\le M_{ms}\le 40M_{\odot }$ 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

arXiv comment7 pages, 6 figures, Accepted for publication in Astrophysics and Space Science

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Cited by in corpus (2)

• Geodynamics and Rate of Volcanism on Massive Earth-like Planets
• Ba & Eu Abundances in M15 giant stars