Pre-supernova models at very low metallicity

Hirschi, R.

Abstract

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.

Citation

Hirschi, R. (2006, June). Pre-supernova models at very low metallicity

• Presentation Conference Type: Poster
• Start Date: Jun 25, 2006
• End Date: Jun 30, 2006
• Deposit Date: Jul 7, 2023
• Publicly Available Date: Jul 7, 2023
• Keywords: Astrophysics
• Publisher URL: https://indico.cern.ch/event/408148/page/4555-program-documents-links
• Related Public URLs: https://arxiv.org/abs/astro-ph/0610281v1