Introduction to Stellar Evolution      

In this lecture it was described how the evolution of single stars is modeled, including the equations of stellar structure, physical data, and simplifying assumptions generally adopted. We then described the evolutionary phases of typical stars of 0.1, 1 and 15 times the mass of the sun. We also touched on the subject of star formation and other research frontiers in stellar astrophysics.

Lecture Notes

1. Two-part series by Iben and Tutukov in Sky and Telescope Magazine, December 1997 and January 1998 issues.
2. Review article by I. Iben, Jr., " Single and Binary Star Evolution," Astrophysical Journal Supplement Series, Vol. 76, pp. 55-114 (May 1991).

1. See special issue of Science, 4 January 2002.

1. How does the Sun Shine? by John N. Bahcall: http://www.nobel.se/physics/articles/fusion/ (This is a review from an historical perspective of the development of understanding of how the Sun shines, including the controversy over the age of the Sun in the 19th century.)
2. "Solar Structure: Models and Inferences from Helioseismology," J.A. Guzik, Proceedings of the SOHO6/GONG98 Workshop Structure and Dynamics of the Interior of the Sun and Sun-Like Stars," Boston, USA, 1-4 June, 1998 (ESA SP-418, October 1998).
3. Our Sun, III. Present and Future, by I. Juliana Sackmann, Arnold Boothroyd, and Kathleen Kraemer, The Astrophysical Journal, Vo. 418, 457, November 20, 1993. (Although this paper is now a little out of date as the solar models do not use the new opacities or include diffusive settling, it is otherwise accurate in its description of how solar models are calculated, and describes the difficulties in determining whether the Earth and inner planets will be engulfed as the Sun becomes a red giant 6 billion years from now.)

1. The End of the Main Sequence, by G. Laughlin, P. Bodenheimer, and F. Adams, The Astrophysical Journal, Vol. 482, pp. 420-432, June 10, 1997. (This paper is rather technical, but it is nicely written and includes some interesting conclusions on the fate of the universe trillions of years from now, when the only stars remaining may be the faintly glowing embers of white dwarfs that have cooled to 63 K.)

1. The Evolution of Massive Stars: The influence of Mass Loss On Population I Stars, Wendee Brunish and J. Truran, the Astrophysical Journal, Vol. 256, p. 247 (May 1, 1982). (This paper describes in detail the evolution of stars of 15, 30 and 40 times the mass of the sun with and without mass loss via winds).

Listed below are the authors of some classic and recently published textbooks on stellar structure, evolution, and nucleosynthesis:
Clayton; Mihalas and Binney (Galactic Astronomy, esp. Ch. 3); Kippenhahn and Weigert; Hansen and Kawaler; Bowers and Deeming; Phillips (The Physics of Stars); Bohm-Vitense (Introduction to Stellar Astrophysics, Vol. 3, Stellar Structure and Evolution); Rose; Prialnik; Bisnovatyi-Kogan; Arnett; Rose; Padmanabhan (Theoretical Astrophysics Vol. II: Stars and Stellar Systems); Cox and Giuli

Katrin Heitmann / LANL / heitmann@lanl.gov / revised January 20