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

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dc.creatorChen, Zhe
dc.creatorZhang, Jiang
dc.creatorChen, YanPing
dc.creatorCui, WenYuan
dc.creatorZhang, Bo
dc.date2006-08-26
dc.date.accessioned2026-07-07T10:23:29Z
dc.date.available2026-07-07T10:23:29Z
dc.descriptionThe 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
dc.description7 pages, 6 figures, Accepted for publication in Astrophysics and Space Science
dc.identifierhttps://arxiv.org/abs/astro-ph/0608568
dc.identifierhttp://arxiv.org/abs/astro-ph/0608568
dc.identifierAstrophys.SpaceSci.306:33-39,2006
dc.identifierdoi:10.1007/s10509-006-9229-2
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/175847
dc.subjectAstrophysics
dc.titleThe yields of r-process elements and chemical evolution of the Galaxy
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