Pre-supernova models at very low metallicity
| dc.creator | Hirschi, R. | |
| dc.date | 2006-10-10 | |
| dc.date.accessioned | 2026-07-07T10:23:51Z | |
| dc.date.available | 2026-07-07T10:23:51Z | |
| dc.description | A series of fast rotating models at very low metallicity (Z=1e-8) was computed in order to explain the surface abundances observed at the surface of CEMP stars, in particular for nitrogen. The main results are the following: - Strong mixing occurs during He--burning and leads to important primary nitrogen production. - Important mass loss takes place in the RSG stage for the most massive models. The 85 solar mass model loses about three quarter of its initial mass, becomes a WO star and could produce a GRB. - The CNO elements of HE1327-2326 could have been produced in massive rotating stars and ejected by their stellar winds. | |
| dc.description | 5 pages, 3 figures, Contribution to "Nuclei in the Cosmos IX", June 25-30 2006, CERN, Geneva, to appear in Proceedings of Science | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0610281 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0610281 | |
| dc.identifier | PoSNIC-IX:116,2006 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/175982 | |
| dc.subject | Astrophysics | |
| dc.title | Pre-supernova models at very low metallicity | |
| dc.type | text |