PHYS30692 10 Semester 2 Undergraduate Level 3 John Leahy Unit coordinator Department of Physics & Astronomy 1 FHEQ level (Framework for Higher Education Qualifications) ' Masters/Integrated Masters P4 ' European Credit Transfer & Accumulation System Rating : 5.0 <p><span style="color: rgb(60, 60, 60); font-family: Arial, sans-serif;">Stars and Stellar Evolution</span></p> <p><span style="color: rgb(60, 60, 60); font-family: Arial, sans-serif;">Stars and Stellar Evolution</span></p> <p>To apply the fundamental physics laws to understand the physics of stellar structure.</p> <div>On completion successful students will be able to:</div><div>&nbsp;</div><div>1. describe the basics of observational classification of stars in terms of spectral type, luminosity class, and the Hertzsprung-Russell diagram</div><div>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</div><div>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</div><div>4. predict the dominant form of energy transport inside stars, based on the opacity to the transfer of radiation</div><div>5. identify the networks of nuclear reactions that operate in stellar cores, with reference to the core temperature, composition, stellar mass, and evolutionary state</div><div><div>6. outline, with respect to the initial mass and composition, the key phases of stellar evolution and the endpoints of such evolution</div><div>7. manipulate equations derived from analytical approximations to the stellar structure equations</div></div><p>&nbsp;</p> <p><strong>1. Observed properties of stars</strong><br />Measurement of stellar distances, luminosities, temperatures.&nbsp; Masses and radii.&nbsp; The Hertzsprung-Russell diagram.</p><p><strong>2. Equations of Stellar structure</strong><br />Time scales.&nbsp; Fundamental equations:&nbsp; mass conservation, hydrostatic equilibrium, energy transport.&nbsp; The virial theorem.&nbsp; Radiative transport and convection.</p><p><strong>3. Equations of State</strong><br />Pressure as function of temperature and density for:&nbsp; Photons, Ideal gas, Degenerate electron gas.&nbsp; Mean molecular weight.&nbsp; Ionization.</p><p paraeid="{7521a7ab-9d44-4957-b62a-ff14637df798}{79}" paraid="2021315077"><strong>4.&nbsp;Radiative transfer and opacity&nbsp;</strong>&nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; Optical depth. Rosseland Mean Opacity. Opacity mechanisms. Applications to stars&nbsp;</p><p paraeid="{7521a7ab-9d44-4957-b62a-ff14637df798}{89}" paraid="1263353123"><strong>5. Nuclear fusion in stars&nbsp;</strong>&nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; Energy yields. Cross sections: the Gamow peak, reaction rates, and their temperature dependence. Reaction chains in stars. Neutrinos.&nbsp;</p><p><strong>6. Stellar modelling</strong><br />Limits to the mass.&nbsp; Solving the coupled equations.&nbsp; Simple analytic stellar models:&nbsp; polytropes and other relations.&nbsp; Numerical models.&nbsp; The Eddington luminosity.&nbsp; Dimensional analysis and mass-radius relations.&nbsp; The HR diagram.</p><p paraeid="{7521a7ab-9d44-4957-b62a-ff14637df798}{133}" paraid="688276693"><strong>7. Asteroseismology&nbsp;</strong>&nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; &nbsp; Pressure and gravity waves; helioseismology; application to other stars&nbsp;</p><p><strong>8. Early stellar evolution</strong><br />The Hayashi line.&nbsp; Onset of nuclear burning.&nbsp; Main sequence evolution.&nbsp; Life times.</p><p><strong>9. Post-main sequence evolution</strong><br />Isothermal cores.&nbsp; Shell burning.&nbsp; Degeneracy:&nbsp; the helium flash.&nbsp; The RGB and the AGB.&nbsp; Mass loss.&nbsp; White dwarfs.&nbsp; Core collapse.&nbsp; Supernovae.</p> 1 Written exam 100% <p>Feedback will be available on students&rsquo; individual written solutions to examples sheets&nbsp;and&nbsp;online tests, and model answers will be issued.</p> PHYS10191 Introduction to Astrophysics and Cosmology Pre-Requisite Compulsory PHYS20352 Statistical Mechanics Pre-Requisite Compulsory PHYS20342 Electromagnetism 2 Pre-Requisite Compulsory <p>Follow - Up units</p><p>PHYS40591 - Radio Astronomy</p><p>PHYS40771 - Gravitation</p> N <p><strong>Recommended text&nbsp;</strong><br />Prialnik, D. An Introduction to the Theory of Stellar Structure and Evolution&nbsp;2nd&nbsp;Ed&nbsp;(CUP 2009)&nbsp;</p><p paraeid="{fb71f896-50af-47f1-a7b4-80fc9642313d}{110}" paraid="219176035"><strong>Useful references&nbsp;</strong><br />Kippenhahn, Weiss&nbsp;&amp;&nbsp;Weigert:&nbsp;Stellar Structure and Evolution, 2nd&nbsp;Ed, (Springer 2012)&nbsp;</p><p paraeid="{fb71f896-50af-47f1-a7b4-80fc9642313d}{134}" paraid="1404913112">Clayton, D.D. Principles of Stellar Evolution and Nucleosynthesis (University of Chicago 1984)</p> Assessment written exam 1.5 Lectures 23 0 75.5