Our knowledge of the physical conditions and processes in stars, as well as their structure and evolution, is based on the study of the electromagnetic radiation emitted by these objects. The most important tool for this is spectral analysis. The outer layers of a star, from which the radiation originates, are called the “stellar atmosphere.” In order to interpret the observations, a theoretical understanding of the physical processes associated with the emission of light is required. In addition, the lecture deals with the structure and evolution of stars, i.e., the properties of stellar matter (equation of state, opacity, ionization, degeneracy), energy transport mechanisms (convection, radiation transport, heat conduction), and energy production through nuclear fusion. As solutions to the corresponding equations, we obtain models of the structure of stars. Based on this, simulations for the evolution of stars from their birth to their end (supernova explosions, white dwarfs, and neutron stars) are discussed. The formation of chemical elements (nucleosynthesis) is also part of the lecture. Finally, the evolution of entire groups, clusters, and populations of stars is considered.
- Kursleiter*in: Prof. Dr. Carsten Denker