1997/10/01 by D. Thomas, L. Greggio, R. Bender · 72 citations
Physics and Astronomy · #Abundance of the chemical elements #Astronomy and Astrophysical Research #Astrophysics #Galaxy #Galaxy formation and evolution #Gamma-ray bursts and supernovae #Initial mass function #Interstellar medium #Metallicity #Nucleosynthesis #Physics #Presolar grains #Star formation #Stars #Stellar evolution #Stellar mass #Stellar, planetary, and galactic studies #Supernova #Type II supernova #astro-ph
paper · pdf · doi:10.1046/j.1365-8711.1998.01289.x
published in Monthly Notices of the Royal Astronomical Society 296(1), 119-149 (Oxford University Press) · Accepted for publication in MNRAS, LaTeX 2.09, requires mn.sty, 20 pages (19 figures) + 7 pages appendix (12 figures), complete ps-file available at ftp://ftp.usm.uni-muenchen.de/pub/daniel/paperI.ps
arxiv created 1997/10/01 · openalex publication_date 1998/05/01 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We analyse two recent computations of type II supernova nucleosynthesis by Woosley & Weaver (1995, hereafter WW95) and Thielemann, Nomoto, & Hashimoto (1996, hereafter TNH96), focusing on the ability to reproduce the observed [Mg/Fe]-ratios in various galaxy types. We show that the yields of oxygen and total metallicity are in good agreement. However, TNH96-models produce more magnesium in the intermediate and less iron in the upper mass range of type II supernovae than WW95-models. To investigate the significance of these discrepancies for chemical evolution, we calculate Simple Stellar Population-yields for both sets of models and different IMF slopes. We conclude that the Mg-yields of WW95 do not suffice to explain the [Mg/Fe] overabundance neither in giant elliptical galaxies and bulges nor in metal-poor stars in the solar neighbourhood and the galactic halo. Calculating the chemical evolution in the solar neighbourhood according to the standard infall-model (e.g. Matteucci & Greggio