This is a 3 credit course. This course is an introduction to the physics of stars.

**3 Exams (60%)**- There will be two exams during the term and one as the final exam.
**Homework (40%)**- Homework problems are assigned associated with each lecture. Those of the previous week are due on Wednesday.
**Final Exam**- The final is Friday 30 April at 8:00. This will be the third of the exams.

Date | Topic | Chapters | Problems |
---|---|---|---|

11 Jan | Introduction | - | |

13 Jan | Stellar Basics | 1.1-1.2 | Calculate the distance to Proxima Centauri. |

15 Jan | HR Diagram | 1.3-1.4 | Ex 1.2,1.3 (1.1, 1.2) |

18 Jan | MLK Day | No Class | |

20 Jan | Equilibrium | 2.1-2.3 | Ex 2.1, 2.2 |

22 Jan | Dynamics | 2.4-2.5 | Ex 2.3, 2.4 |

25 Jan | Evolution Equation | 2.6-2.7 | |

27 Jan | Timescale | 2.8 | |

29 Jan | Equation of State | 3.1-3.2 | Show the Pressure Integral is dimensionally correct and prove Equation 3.9 |

1 Feb | Pressure | 3.3-3.4 | Ex 3.1 |

3 Feb | Radiation | 3.5-3.6 | Ex 3.2 |

5 Feb | Radiative Transfer | 3.7 | Ex 3.3 |

8 Feb | Nuclear Reactions | 4.1-4.2 | Prove Equation 4.6 |

10 Feb | Hydrogen Burning | 4.3-4.4 | |

12 Feb | He, C, O, Si Burning | 4.5-4.7 | Ex 4.1,4.2 |

15 Feb | Heavy Elements | 4.8-4.10 | |

17 Feb | Review | 1-4 | |

19 Feb | Exam 1 | 1-4 | |

22 Feb | Simple Stellar Model I | 5.1-5.3 | Ex 5.1,5.2,5.3,5.4 |

24 Feb | Limits | 5.4-5.5 | Ex 5.5,5.6 |

26 Feb | Simple Stellar Model II | 5.6-5.7 | Ex 5.7 |

1 Mar | Thermal Stability | 6.1-6.2 | |

3 Mar | Dynamic Stability | 6.3-6.4 | Show that for an adiabatic process, stable hydrostatic equilibrium corresponds to a minimum state of the total energy; Show that there is a critical temperature above which partially ionized hydrogen will always be dynamically staple, and find this temperature (Ex 6.2, 6.3) |

5 Mar | Convection | 6.5-6.7 | Ex 6.2 (6.4) |

8 Mar | T-rho Evolution | 7.1-7.2 | |

10 Mar | The Main Sequence | 7.3-7.4 | Ex 7.1, 7.2, 7.3 |

12 Mar | Late Evolution and Problems | 7.5-7.6 | Ex 7.6 |

15-19 Mar | Spring Break | No Class | |

22 Mar | Review | 5-7 | |

24 Mar | Exam II | 5-7 | |

26 Mar | Pre-Main Sequence | 8.1 (9.1) | |

29 Mar | Main Sequence Phase | 8.2-8.3 (9.2-9.3) | Ex 8.2 (9.1) |

30 Mar | Red Giants | 8.4 (9.4) | Ex 8.3 (9.2) |

2 Apr | Core Helium Burning | 8.5-8.6 (9.5-9.6) | Ex 8.4,8.5 (Estimate the mass loss timescale and compare it with the thermal timescale of a star; Show that the rate of energy supply required for the mass loss at a rate given by equation 9.27 is a small fraction of the luminosity; Find the relation between the mass loss timescale and the nuclear timescale of the star and show that usually the mass loss timescale is less than the nuclear timescale; Assuming that the mass loss rate may be parametrized and in equation 9.27 show that for a main sequence star the mass loss rate is proportional to the luminosity to some exponent alpha and evaluate alpha. |

5 Apr | Star Death | 8.7-8.8 (9.7-9.8) | Ex 8.6 (9.3) |

7 Apr | Massive Stars | 8.9-8.10 (9.9-9.10) | |

9 Apr | Supernova | 9.1 (10.1) | |

12 Apr | Supernova Explosions | 9.2 (10.2) | Ex 9.1,9,2 (10.1,10.2) |

14 Apr | Stellar Nucleosynthesis | 9.3-9.4 (10.3-10.4) | Derive the espression of the light curve L(t) of a supernova powered by the decay of Ni-56 and Co-56 assuming that one solar mass of Ni-56 was initially expelled in the explosion (Ex 10.3) |

16 Apr | Black Holes | 9.5-9.6 (10.5-10.6,11.2) | |

19 Apr | Star Formation | 10.1-10.2 (12.1-12.2) | Ex 10.1 (12.1) |

21 Apr | Initial Mass | 10.3-10.4 (12.3-12.4) | Ex 10.2,10.3 (12.2,12.3) |

23 Apr | Global Stellar Evolution | 10.5 (12.5) | Ex 10.4 (12.4) |

26 Apr | Review | 8-10 (9,10-12) | - |

30 Apr | Final | 8-10 (9,10-12) | - |

Last modified: Sun Mar 22 19:07:17 EDT 2009