Stellar Structure and Evolution

A large part of our understanding of the Universe relies on the understanding and accurate modeling of stars. Stars make up a very important part of the integrated light of galaxies, and are major contributors to the chemical and dynamical evolution of galaxies. In this course, we will look at the physics describing stellar structure, and study how this structure evolves over time in the case of isolated stars.

The aim is to provide the physical keys to understanding the structure and evolution of stars and their observational properties from the pre-main-sequence phase to the end of their nuclear life, for stars of all masses and chemical compositions.

At the end of this course, students will be familiar with the classical physical processes (equation of state, matter-radiation interaction, nucleosynthesis, etc.) governing the structure and evolution of stars and their modeling. They will also understand the modifications brought about by the introduction of non-standard matter transport processes into these models. Finally, they will have a basic understanding of stellar pulsations.

Astrophysics

Radiation Transfer and Stellar Atmospheres

Assessment takes the form of continuous assessment and a final exam.

1. Introduction to stellar physics
2. 1D stellar structure equations
3. Equation of state
4. Thermonuclear reactions and nucleosynthesis
5. Opacities and heat transport in stellar interiors
6. Detailed analysis of stellar evolution: low-mass, intermediate-mass and massive stars
7. Physics and stellar evolution beyond the classical model
8. Introduction to the physics of stellar variability