New presupernova evolutionary models of massive stars are presented. Improvements compared with the previous models are the inclusion of Coulomb interaction in the equation of state, electron capture from the beginning of oxygen burning, and many links between the silicon and iron quasi-equilibrium clusters during silicon burning. The iron core is found to be significantly smaller than in the previous models, especially for stars smaller than 15 M⊙.
All Science Journal Classification (ASJC) codes
- Physics and Astronomy(all)