AST 383D

COMPONENTS OF THE COURSE

OUTLINE

1. BASIC CONSIDERATIONS

   astrophysical context of the study of stellar structure and evolution (1)

   • why is it important?
   • what are the OBSERVABLES?
   
   mathematical context: basic equations for constructing highly idealized stellar structure models: timescales: virial theorem (3)

   basic equations of stellar evolution: the non-eternal stars (1)

   a walk through the Hertzsprung-Russell zoo (1)
    

2. CONSTITUTIVE PHYSICS

   equations of state of matter (3)

   heat transfer by radiation and conduction, a discussion of opacities (2)

   convective energy transport (2)

   energy sources and sinks: nuclear reactions, gravitational contraction, neutrinos, bfe-particles (2)
    

3. CONSTRUCTION OF NUMERICAL MODELS

   simple models: polytropes, homology transformation (1)

   building a better mule: towards more realistic models, but still leaving out all the physics we can get away with -- and more (1)
    

4. INTERPRETATION OF THE RESULTS OF THE NUMERICAL MODELS

   star formation (1)

   main sequence evolution (1)

   post-main sequence evolution (3)

   binary star evolution (1)

   supernovae (1)
    

5. "LOOK, MA, NO PHYSICS. . ."

   the three Big Uglies: rotation, convection, and magnetic fields (2)

   mass loss (1)
    

6. APPLICATIONS

   cosmochronology (3)

   to be determined (3)
    

7. REPORTS ON STUDENT PROJECTS

   assuming six teams, one report per class period (6)

GRADES

Class participation: 5% -- based on participation in discussions

Stellar seminar attendance: 5% -- based on attendance (5%-1% x (no. absences)) Note for those who might have observing runs or meetings: If you must be absent, notes in your handwriting (copied from someone else) will be accepted in lieu of attendance.

Course notes: 15% -- your graduate course notes will be your most handy reference material later in your career: this is my way of guaranteeing that your stellar evolution notes will be first-rate.

Exam 1: 25% -- derivation and analytical problems in stellar structure and evolution.

Exam 2: 25% -- derivation and analytical problems in stellar structure and evolution.

Term Project (Numerical Experiments): 25% -- a project of your choice, built around the calculation of evolutionary sequences using a simplified numerical code provided, and mastering the relevant literature.

REMEMBER: You will get out of this course exactly what you put into it.

GENERAL REFERENCES

1. Clayton, D.D. 1968, Principles of Stellar Evolution and Nucleosynthesis -- probably the best graduate-level text available, discussions generally clear, physical, without too much detail. Through discussion of nucleosynthesis, but too much for this course. Designed for one-year course.

2. Schwarzschild, M. 1958, Structure and Evolution of the Stars-- no modern applications, but discussion of input physics timeless, clear and brief as appropriate to a one-term survey course.

3. Cox, J.P. and Giuli, R. T. 1968, Principles of Stellar Structure (2 volumes) -- the bible -- as a reference work -- but far too detailed to be generally useful for first-time learning. Fair summary of single star evolution in Volume 2, detailed discussion of pulsation theory

4. Chiu and Muriel (eds,) 1972, Stellar Evolution -- excellent review papers.

5. Chiu, H.Y. 1968, Stellar Physics -- standard discussion of basics, particular specialty -- discussion of quantum physics, weak interactions.

6. Chandrasekhar, S. 1939, An Introduction to the Study of Stellar Structure -- still-useful discussions of polytropes, degeneracy, white dwarfs.

7. Stein, R.F. and Cameron, A.G.W. (eds.) 1966, Stellar Evolution -- good reviews, particularly Stein's article on analytical models.

READING LIST

*recommended

+Trimble, Reviews of Modern Physics,	54, 1183, 1983.
	55, 511, 1983.
Woosley and Weaver, Ann. Rev. Astr. Ap.,	24, 205, 1986.

Nuclear Astrophysics, Fowler, Caughlin, and Zimmerman, Ann. Rev., 13, 69, 1975.