Stellar Atmospheres
Cool layer in a Sun-like star. Image credit: ESA
During the first part of the course you will build on the concepts taught during the bachelor course Astrophysical Spectra (or equivalent) and study how spectral lines and continua are formed in stellar atmospheres. Particular attention will be given to the concept of scattering. You will apply the theory to write a computer program that can solve radiative transfer problems that involve scattering. In the second part of the course you will learn about modern radiation-magnetohydrodynamical simulations of stellar atmospheres. You will perform a simulation with an existing stellar atmosphere code, analyse the resulting atmosphere model, and use the code developed in the first part of the course to compute how light escapes from the model.
The course is given during daytime and is part of the Master’s Programme in Astronomy. It can also be taken as a free-standing course, provided that you meet the entry requirements. The course is taught in English.
Teaching Format
Instruction is given in the form of lectures, exercise classes as well as a set of computer exercises. Participation in the computer exercises is mandatory.
Assessment
A written individual report about the computer exercises and a final written exam.
Examiner
Jorrit Leenaarts
Radiative Transfer in Stellar Atmospheres, 2003 by Robert J. Rutten:
http://www.staff.science.uu.nl/~rutte101/Radiative_Transfer.html
