After the basic introduction, the students will learn how stars are forming and what physical conditions are required for that.
In the next section the students will learn about the basic equation of
stellar structure and how to solve them. The next section introduces the
students to the radiative transfer equation its applications. The
following sections focuses on the stellar interior and the
nucleosynthesis. The subjects of the following lectures are the
photosphere, chromosphere, the corona and stellar wind of low-mass
stars and their evolution of low-mass stars after they have left the
main sequence. The next subject is the evolution of high mass-stars
including neutron stars and black wholes. The final chapters focus of
brown dwarfs and planets.
- Trainer/in: Sébastien Pezzagna