Instructor: Course Objectives: Assessment: Practicalities: Syllabus: Coursework: Midterm Exam: Final Exam: Project: 
Tiziana Di Matteo Office: Wean Hall 8305 phone: 4122681888 email: tiziana'at'phys.cmu.edu In this course we will apply fundamental physical laws to model in the internal structure of stars. We will cover the equations of stellar structure the microphysics of the equation of state, nuclear reactions, and opacity. We will review how stars evolve and what the endpoints of stellar evolution are (neutron stars and black holes). Finally we will examine the structure and components of our Milky Way. It will be based on weekly problem sets distributed on Mondays and due the following Monday before class (total of 40%  homework will be posted on this page). In addition we will have a midterm exam (30%) a project worth 30% and a final takehome exam (weighted as 4 homework  10%). Classes are Mondays/Wednesdays/Fridays at 3:30 4:20pm in Wean Hall 8427. Attendance is required, please email me if you are not going to come to class. Feel free to stop by my office for questions/problems etc. 1 Overview of the problem of stellar structure 2 Astronomical nomenclature and observed properties of stars 3 Derivation of stellar structure equations (mass, hydrostatic eq. and energy) 4 The Virial theorem, global energetics and stellar timescales 5 Ideal gas law for a mixture of gases 6 Equation of State I: Density of states (QM) and occupation numbers(Stat.m) 7 Equation of State II: Internal energy and pressure 8 Maxwell distribution, Perfect gas, Quantum concentration 9 FermiDirac distribution, degenerate electrons in the Sun core  Helium flash 10Planck Distribution, radiation pressure in stars 11Boltzmann law and Sahaequation. Stellar Spectra 12 Limitations of the Saha equation. Specific heats, Polytropes 13 LaneEmden equation Numerical Solutions  Tabulated functions 14 Massradius relation. Eddingtonstandard model and white dwarfs 15 Energy Transport in stars  Heat transfer due to random motions 16 Radiative transfer  Rosseland mean opacity  Eddington limit 17 Electron conduction (white dwarfs)  Sources of opacity  Kramer's law 18 Convective energy Transport  Schwarzchild criterion 19 Convection in low and high mass (MS) stars  Mixing length theory 20 Nuclear fusion in stars: Overview 21 MidTerm Exam 22 Thermonuclear reactions in stars: intro and quantum tunnelling 23 Cross section to nuclear reactions, Gamow Peak 24 Major nuclear burning stages nuclear burning 25 The solar neutrino problem 26 Star formation  Jeans criterion  collapse and fragmentation 27 Protostars  Hayashi tracks  Observations and calculations 28 Project  setting up the stellar evolution code 30 Project Ideas  Stars in the Solar Neighbourhood, The age of clusters, etc.. 31 Research Talk  Guest Speaker: Brigitte Koenig (PITT) 32 Endpoints of stellar evolution 33 White dwarfs  degeneracy  Luminosity and cooling times 34  Neutron stars  Photodissociation  Neutronization  Maximum mass Pulsars 35  Black Holes  Fundamental GR predictions  event horizon  collapse 36  Black Holes in astrophysics  star mass and supermassive black holes 37  Constituents of a galaxy  Morphological classification  Luminosity function 38  The structure of the Milky Way  Photometric and Kinematic model 39  Oort constants: rotation curve of the Milky Way  dark matter Problem Set 1 Due Monday, September 12th Problem Set 2 Due Monday, September 19th Problem Set 3 Due Monday, September 26th Problem Set 4 Due Wednesday, October 5th Problem Set 5 Due Wednesday, October 12th Problem Set 6 Due Wednesday, October 26th Problem Set 7 Due Wednesday, November 2nd Problem Set 8 Due Wednesday, November 9th MONDAY OCTOBER 17th  3:30  5:30pm  in W 7316 TAKEHOME: Friday December 9th  Due Monday December 12th Part I  Due Friday, November 18th Part II  Grading Sheet  Due Friday, December 9th Research articles: Low mass stars M5 Globular Cluster HR diagram 

