| dc.contributor.author | Rauscher, T. | |
| dc.contributor.author | Heger, A. | |
| dc.contributor.author | Hoffman, R. D. | |
| dc.contributor.author | Woosley, S.E. | |
| dc.date.accessioned | 2013-06-18T09:45:43Z | |
| dc.date.available | 2013-06-18T09:45:43Z | |
| dc.date.issued | 2001-05-21 | |
| dc.identifier.citation | Rauscher , T , Heger , A , Hoffman , R D & Woosley , S E 2001 , ' Nucleosynthesis in massive stars revisited ' , Nuclear Physics A , vol. 688 , no. 1-2 , pp. 193C-196C . | |
| dc.identifier.issn | 0375-9474 | |
| dc.identifier.uri | http://hdl.handle.net/2299/10811 | |
| dc.description.abstract | We have performed the first calculations to follow the evolution of all stable nuclei and their radioactive progenitors in a finely-zoned stellar model computed from the onset of central hydrogen burning through explosion as a Type II supernova. Calculations were done for 15 M-circle dot, 20 M-circle dot, and 25 M-circle dot Pop I stars using the most recently available set of experimental and theoretical nuclear data, revised opacity tables, and taking into account mass loss due to stellar winds. Here results are presented for one 15 M-circle dot model. | en |
| dc.format.extent | 4 | |
| dc.language.iso | eng | |
| dc.relation.ispartof | Nuclear Physics A | |
| dc.subject | R-PROCESS | |
| dc.subject | MODEL CALCULATIONS | |
| dc.subject | SUPERNOVAE | |
| dc.subject | NUCLEI | |
| dc.subject | REACTION-RATES | |
| dc.subject | ENVIRONMENTS | |
| dc.subject | CROSS-SECTION | |
| dc.subject | P-PROCESS | |
| dc.title | Nucleosynthesis in massive stars revisited | en |
| dc.contributor.institution | Centre for Astrophysics Research (CAR) | |
| dc.contributor.institution | School of Physics, Engineering & Computer Science | |
| dc.description.status | Peer reviewed | |
| rioxxterms.type | Journal Article/Review | |
| herts.preservation.rarelyaccessed | true | |
