Master of Physics (MPhys)

MPhys Physics

Join a physics Department of international renown that offers great choice and flexibility, leading to master's qualification.

  • Duration: 4 years
  • Year of entry: 2025
  • UCAS course code: F305 / Institution code: M20
  • Key features:
  • Scholarships available
  • Accredited course

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Fees and funding

Fees

Tuition fees for home students commencing their studies in September 2025 will be £9,535 per annum (subject to Parliamentary approval). Tuition fees for international students will be £36,500 per annum. For general information please see the undergraduate finance pages.

Policy on additional costs

All students should normally be able to complete their programme of study without incurring additional study costs over and above the tuition fee for that programme. Any unavoidable additional compulsory costs totalling more than 1% of the annual home undergraduate fee per annum, regardless of whether the programme in question is undergraduate or postgraduate taught, will be made clear to you at the point of application. Further information can be found in the University's Policy on additional costs incurred by students on undergraduate and postgraduate taught programmes (PDF document, 91KB).

Scholarships/sponsorships

The University of Manchester is committed to attracting and supporting the very best students. We have a focus on nurturing talent and ability and we want to make sure that you have the opportunity to study here, regardless of your financial circumstances.

For information about scholarships and bursaries please visit our undergraduate student finance pages and our Department funding pages .

Course unit details:
Stars and Stellar Evolution

Course unit fact file
Unit code PHYS30692
Credit rating 10
Unit level Level 3
Teaching period(s) Semester 2
Offered by Department of Physics & Astronomy
Available as a free choice unit? No

Overview

Stars and Stellar Evolution

Pre/co-requisites

Unit title Unit code Requirement type Description
Introduction to Astrophysics and Cosmology PHYS10191 Pre-Requisite Compulsory
Electromagnetism PHYS20141 Pre-Requisite Compulsory
Statistical Mechanics PHYS20352 Pre-Requisite Compulsory

Follow - Up units

PHYS40591 - Radio Astronomy

PHYS40771 - Gravitation

Aims

To apply the fundamental physics laws to understand the physics of stellar structure.

Learning outcomes

On completion successful students will be able to:
 
1. describe the basics of observational classification of stars in terms of spectral type, luminosity class, and the Hertzsprung-Russell diagram
2. assemble a set of equations of stellar structure from the physics of pressure balance, conservation of mass and luminosity, and the transport of energy
3. contrast the different versions of the equation of state in stellar interiors with respect to the contributions to the pressure of radiation, degenerate and non-degenerate gases
4. predict the dominant form of energy transport inside stars, based on the opacity to the transfer of radiation
5. identify the networks of nuclear reactions that operate in stellar cores, with reference to the core temperature, composition, stellar mass, and evolutionary state
6. outline, with respect to the initial mass and composition, the key phases of stellar evolution and the endpoints of such evolution
7. manipulate equations derived from analytical approximations to the stellar structure equations

 

Syllabus

1. Observed properties of stars
Measurement of stellar distances, luminosities, temperatures.  Masses and radii.  The Hertzsprung-Russell diagram.

2. Equations of Stellar structure
Time scales.  Fundamental equations:  mass conservation, hydrostatic equilibrium, energy transport.  The virial theorem.  Radiative transport and convection.

3. Equations of State
Pressure as function of temperature and density for:  Photons, Ideal gas, Degenerate electron gas.  Mean molecular weight.  Ionization.

4. Radiative transfer and opacity                                                                                                       Optical depth. Rosseland Mean Opacity. Opacity mechanisms. Applications to stars 

5. Nuclear fusion in stars                                                                                                                     Energy yields. Cross sections: the Gamow peak, reaction rates, and their temperature dependence. Reaction chains in stars. Neutrinos. 

6. Stellar modelling
Limits to the mass.  Solving the coupled equations.  Simple analytic stellar models:  polytropes and other relations.  Numerical models.  The Eddington luminosity.  Dimensional analysis and mass-radius relations.  The HR diagram.

7. Asteroseismology                                                                                                                               Pressure and gravity waves; helioseismology; application to other stars 

8. Early stellar evolution
The Hayashi line.  Onset of nuclear burning.  Main sequence evolution.  Life times.

9. Post-main sequence evolution
Isothermal cores.  Shell burning.  Degeneracy:  the helium flash.  The RGB and the AGB.  Mass loss.  White dwarfs.  Core collapse.  Supernovae.

Assessment methods

Method Weight
Written exam 100%

Feedback methods

Feedback will be available on students’ individual written solutions to examples sheets and online tests, and model answers will be issued.

Recommended reading

Recommended text 
Prialnik, D. An Introduction to the Theory of Stellar Structure and Evolution 2nd Ed (CUP 2009) 

Useful references 
Kippenhahn, Weiss & Weigert: Stellar Structure and Evolution, 2nd Ed, (Springer 2012) 

Clayton, D.D. Principles of Stellar Evolution and Nucleosynthesis (University of Chicago 1984)

Study hours

Scheduled activity hours
Assessment written exam 1.5
Lectures 23
Independent study hours
Independent study 75.5

Teaching staff

Staff member Role
John Leahy Unit coordinator

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