Course 7: Nuclear theory for astrophysics
Motivation and background.
The course aims at teaching modern theoretical approaches that are used in studies of nucleosynthesis processes in stellar evolution and stellar explosions, with an emphasis on the role of nuclei far from stability.
1. Thermonuclear rates and reaction networks
1.1. Thermonuclear reaction rates
1.2. Nuclear reaction networks
1.3. Burning processes in stellar environments
2. Nuclear astrophysics with radioactive beams
2.1 Charged-particle cross section
2.2 Gamow window
2.3 Relevant energy ranges for cross section measurements
3. Cross section predictions and reaction rates
3.1 Thermonuclear rates from statistical model calculations
4. Weak-interaction rates
4.1 Electron capture and beta-decay
4.2 Neutrino-induced reactions
5. Explosive burning processes
5.1 Explosive H-burning
5.2 Explosive He-burning
5.3 Explosive C- and Ne-burning
5.4 Explosive O-burning
5.5 Explosive Si-burning
5.6 The r-process
6. Core collapse supernovae
6.1 General picture
6.2 Weak-interaction rates and presupernova evolution
6.3 The role of electron capture during collapse
6.4 Neutrino-induced processes during a supernova collapse
6.5 Type II supernovae nucleosynthesis
6.6 Supernova remnants
6.7 The role of radioactive decays
7. The r-process
7.1 The role of nuclear physics
7.2 Working of the r-process and required environment properties
7.3 Sites of r-process in nature
8. Nuclear processes in explosive binary systems
8.1 Nova explosions
8.2 X-ray bursts
8.3 X-ray pulsars
8.4 Black hole and neutron star accretion disks
Syllabus of 30+30+60 hours (lectures+exercises+work on projects).