Stellar Structure and Evolution

Much of our understanding of the Universe relies on understanding and accurately modeling stars. Stars account for a very large portion of the total light emitted by galaxies, and they are major contributors to the chemical and dynamical evolution of galaxies. In this course, we will explore the physics underlying stellar structure and examine 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 through the end of their nuclear life, for stars of all masses and chemical compositions.

By the end of this course, students will be familiar with the classical physical processes (equation of state, matter-radiation interaction, nucleosynthesis, etc.) that govern the structure and evolution of stars and their modeling. They will have a basic understanding of the changes introduced by the inclusion of so-called non-standard matter transport processes in these models. Finally, they will have a basic understanding of stellar pulsations.

Astrophysics

Radiation Transfer and Stellar Atmospheres

Assessment consists of ongoing evaluation and a final exam

1. Introduction to Stellar Physics
2. The 1D Equations of Stellar Structure
3. Equation of State
4. Thermonuclear Reactions and Nucleosynthesis
5. Opacities and Heat Transfer Mechanisms in Stellar Interiors
6. Detailed Analysis of Stellar Evolution: Low-Mass, Intermediate-Mass, and Massive Stars
7. Stellar Physics and Evolution Beyond the Classical Model
8. Introduction to the Physics of Stellar Variability