Article ID | Journal | Published Year | Pages | File Type |
---|---|---|---|---|
1779533 | New Astronomy | 2006 | 9 Pages |
Abstract
Low metallicity very massive stars with an initial mass between 140Mâ and 260Mâ can be subdivided into two groups: those between 140Mâ and 200Mâ which produce a relatively small amount of Fe, and those with a mass between 200Mâ and 260Mâ where the Fe-yield ejected during the supernova explosion is enormous. We first demonstrate that the inclusion of the second group into a chemical evolutionary model for the Solar Neighbourhood predicts an early temporal evolution of Fe, which is at variance with observations whereas it cannot be excluded that the first group could have been present. We then show that a low metallicity binary with very massive components (with a mass corresponding to the first group) can be an efficient site of primary 14N production through the explosion of a binary component that has been polluted by the pair instability supernova ejecta of its companion. When we implement these massive binary 14N yields in a chemical evolution model, we conclude that very massive close binaries may be important sites of 14N enrichment during the early evolution of the Galaxy.
Related Topics
Physical Sciences and Engineering
Physics and Astronomy
Astronomy and Astrophysics
Authors
D. Vanbeveren, E. De Donder,