PHYS3010 Stellar Evolution
Module Overview
This course is a showcase for how the various branches of physics come together to give rise to real life phenomena. Using the example of stars, we will revisit a wide range of different physics and see how the various ingredients interact and thus how all branches of physics play a role in creating the fundamental building blocks of the universe. The emphasis of the course is on the more theoretical aspects of physics. The course is compulsory for ‘with Astronomy’ students but offers a good opportunity for all Physics students who want to obtain a hands-on experience of ‘the bigger picture’ in physics.
Aims and Objectives
Module Aims
The aim of this course is to explore the life-cycles of (isolated) stars: from their birth in dense gas clouds, through their stable life in equilibrium, to their explosive death and afterlife in the form of exotic matter condensates, i.e., white dwarfs, neutron stars, and black holes. Along the way, we will study gravity, thermodynamics, hydrodynamics, the interaction between radiation and matter, degenerate forms of matter, and nuclear reactions.
Learning Outcomes
Knowledge and Understanding
Having successfully completed this module, you will be able to demonstrate knowledge and understanding of:
- demonstrate clear insight into the underlying physical principles associated with all the key stages of stellar evolution from initial star formation within gas clouds in the Galactic plane, through the various stages of “stability,” to the final end products
- describe how astrophysics brings together all branches of physics and thus allows us to understand the ‘big picture’ of physics
- be able to solve order-of-magnitude problems on any part of the syllabus
Syllabus
- Overview of gravitational contraction and star formation, nucleosynthesis, virial theorem, stellar timescales. - Properties of matter and radiation: Ideal gas, electron and neutron degeneracy, blackbody radiation, ionization. - Heat transfer: Radiation transport, conduction, convection. - Thermonuclear fusion: Barrier penetration, reaction rates, hydrogen and helium burning, neutrino emission. - Stellar modelling: Equations of stellar structure, polytropes. - Stellar death: Supernovae, white dwarfs, neutron stars, black holes.
Learning and Teaching
| Type | Hours |
|---|---|
| Preparation for scheduled sessions | 18 |
| Completion of assessment task | 18 |
| Lecture | 36 |
| Revision | 10 |
| Wider reading or practice | 50 |
| Follow-up work | 18 |
| Total study time | 150 |
Resources & Reading list
D. Prialnik (2009). An Introduction to the Theory of Stellar Structure and Evolution.
Assessment
Summative
| Method | Percentage contribution |
|---|---|
| Coursework | 20% |
| Examination (2 hours) | 80% |
Referral
| Method | Percentage contribution |
|---|---|
| Coursework marks carried forward | % |
| Examination | % |
Repeat Information
Repeat type: Internal & External
Linked modules
Pre-requisites: PHYS2001 AND PHYS2003 AND PHYS2006 AND PHYS2023 AND PHYS2024 AND PHYS1005