In this course we aim to cover the essential physics of the internal structure of stars -
the basic equations of stellar structure, opacity, and nuclear reactions. We will discuss at a semi-quantitative level
how stars evolve, starting from prior the main sequence and to the ends of their life. We also will compute and analyze stellar models using realistic stellar evolution code.
Special note for 3d year undergraduate students: please think twice before you enroll in this course. The course requires advanced ability to set up and solve problems. Students are usually trained in this by the end of their 4th year, 3d year students have showed before bad performance. This is not about the formal list of pre-requisite courses, its about your overal training as a physicist and your expereince with solving complex physical problems. This is not a pretty-astro-pictures based course.
Lecture notes
Lecture notes are not guaranteed. I will attempt to provide most of them onine here,
but you should make a fair effort to make your own notes
or cooperate with classmates in case you are absent.
I will be not giving out any notes in addition to the posted below.
This class works in CGS units ONLY. No SI units homeworks will be accepted.
Lecture 37: Testing binary evolution. Where is it important? Slides
Due to new copyright changes from Jan 2011, the access to the lecture notes is now restricted. Enrolled students can obtain the password from me. Please consider to protest new policies and tariff by Access Copyright.