Slide 1 Modelling SN Type II: evolution up to collapse From Woosley et al. (2002) Woosley Lectures 11 and 12 Slide 2 Slide 3 Hydrogen Burning Slide 4 Temperature sensitivity…

Nuclear Astrophysics II Lecture 5 Fri. June 1, 2012 Prof. Shawn Bishop, Office 2013, Ex. 12437 [email protected] http://www.nucastro.ph.tum.de/ * Where to from here?…

Units to cover: 62, 63, 64 Homework: Unit 60: Problems 12, 16, 18, 19 Unit 61 Problems 11, 12, 17, 18, 20 Unit 62 Problems 17, 18, 19 Unit 63, Problems 17, 19 Internal Structure…

Lecture 10 Nucleosynthesis During Helium Burning and the s-Process So, typical temperatures are 2 x 108 K (higher in shell burning later) when densities are over 1000 gm…

Nuclear Astrophysics II Lecture 5 Fri. June 1, 2012 Prof. Shawn Bishop, Office 2013, Ex. 12437 [email protected] http://www.nucastro.ph.tum.de/ * Where to from here?…

Lecture 10 Nucleosynthesis During Helium Burning and the s-Process So, typical temperatures are 2 x 108 K (higher in shell burning later) when densities are over 1000 gm…