1998/10/05 by Takuji Tsujimoto, T. Tsujimoto, Toshikazu Shigeyama +1
Physics and Astronomy · #Abundance (ecology) #Astronomy and Astrophysical Research #Gamma-ray bursts and supernovae #Initial mass function #Metallicity #Nucleosynthesis #Stars #Stellar evolution #Stellar nucleosynthesis #Stellar, planetary, and galactic studies #Supernova #astro-ph
paper · pdf · doi:10.1023/a:1002144201050
published as Astrophys.Space Sci. 265 (1999) 49-50 · 5 pages including 3 figures, to appear in ApJ Letters
arxiv created 1998/10/05 · openalex publication_date 1999/07/01 · arxiv updated 2009/12/01 · openalex created_date 2019/06/27 · openalex updated_date 2026/08/05
The supernova yields of several heavy elements including alpha-, iron-group, and r-process elements are obtained as a function of the mass of their progenitor main-sequence stars Mms from the abundance patterns of extremely metal-poor stars with a procedure recently proposed by Shigeyama and Tsujimoto (1998). The ejected masses of alpha- and iron-group elements increase with Mms, whereas more Eu is ejected from supernovae with lower Mms. For these several heavy elements, it is shown that the average abundance ratios weighted by the Salpeter initial mass function coincide with the ratios observed in stars with -2<[Fe/H]<-1 within 0.1 dex. It follows that the correlations of stellar abundance ratios with the metallicity are twofold. One is the abundance ratios for [Fe/H] <-2.5 imprinted by the nucleosynthesis in individual supernovae on the timescale 107yr and the other for [Fe/H]>-2 results from the mixing of the products from a whole site of the nucleosynthesis, taking place on the timescale longer than 109yr.