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The Yields of r-Process Elements and Chemical Evolution of the Galaxy.
- Source :
- Astrophysics & Space Science; Nov2006, Vol. 306 Issue 1/2, p33-39, 7p, 6 Graphs
- Publication Year :
- 2006
-
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 <subscript>ms</subscript> ≤ 18 M <subscript>⊙</subscript> are infertile sources and the SNe II with 20 M <subscript>⊙</subscript> ≤ M <subscript>ms</subscript> ≤ 40 M <subscript>⊙</subscript> are the dominant source of r-process nucleosynthesis in the Galaxy. The ratio of these stars 20 M <subscript>⊙</subscript> ≤ M <subscript>ms</subscript> ≤ 40 M <subscript>⊙</subscript> with compared to the all massive stars is about∼ 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. [ABSTRACT FROM AUTHOR]
Details
- Language :
- English
- ISSN :
- 0004640X
- Volume :
- 306
- Issue :
- 1/2
- Database :
- Complementary Index
- Journal :
- Astrophysics & Space Science
- Publication Type :
- Academic Journal
- Accession number :
- 23302422
- Full Text :
- https://doi.org/10.1007/s10509-006-9229-2