Pre-supernova models at very low metallicity

Details Pre-supernova models at very low metallicity Pre-supernova models at very low metallicity

2006-10-10

arxiv.org/abs/astro-ph/0610281v1

PoSNIC-IX:116,2006

Astronomy and Astrophysics

Astrophysics

5 pages, 3 figures, Contribution to "Nuclei in the Cosmos IX", June 25-30 2006, CERN, Geneva, to appear in Proceedings of Scie

Scientific paper

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.

Affiliated with

Also associated with

No associations

Rating

Pre-supernova models at very low metallicity does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Pre-supernova models at very low metallicity, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Pre-supernova models at very low metallicity will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-437214