Stellar Structure and Evolution

Much of our understanding of the Universe relies on understanding and accurately modeling stars. Stars constitute a very important part of the integrated light of galaxies, and are major contributors to the chemical and dynamic evolution of galaxies. In this course, we will discuss the physics describing stellar structure and study how this structure evolves over time in the case of isolated stars.

The objectives are 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 (equations of state, matter-radiation interaction, nucleosynthesis, etc.) governing the structure and evolution of stars and their modeling. They will have an understanding of the changes brought about by the introduction of so-called 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. Equations of 1D stellar structure
3. Equation of state
4. Thermonuclear reactions and nucleosynthesis
5. Opacities and heat transport mechanisms 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