Abstract
The structure and evolution of stars is the one part of modern astrophysics that can be described as, to a considerable extent, a solved problem. This means we can-
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1. write down a set of four differential equations (see the previous chapter or §7.1) that describe gradients of conditions inside a star,
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2. insert into these equations the necessary physics of nuclear reactions (Chap. 6), transport of energy by radiation, convection, and occasionally conduction (Chaps. 4 and 5), and the relationship among the thermodynamic variables T, ρ, and P, also called the equation of state (Chap. 3).
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3. We can choose reasonable boundary conditions (e.g., see §4.3),
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4. integrate the equations numerically (Chap. 7) to find out what stars should look like, and
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5. compare model stars with real ones.
“And now for something completely different.”
— Monty Python’s Flying Circus (Oct. 1969–Dec. 1974)
“I never know how much of what I say is true.”
— Bette Midler (1980)
#x201C;You’d look pretty simple from ten parsecs too.”
—Attributed to Fred Hoyle in response to a question from someone who was puzzled why we do not seem to understand so simple a thing as a star. (c. 1955)
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2.17 References and Suggested Readings
§2.1: Young Stellar Objects
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§2.5: Helium Flash or Fizzle
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§2.8: Core Collapse and Nucleosynthesis
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§2.9: Variable Stars
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§2.10: Pulsational Variables
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§2.11: Explosive Variables
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§2.12: White Dwarfs, Neutron Stars and Black Holes
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§2.13: Binary Stars
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§2.14: Star Formation
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Hansen, C.J., Kawaler, S.D., Trimble, V. (2004). An Overview of Stellar Evolution. In: Stellar Interiors. Astronomy and Astrophysics Library. Springer, New York, NY. https://doi.org/10.1007/978-1-4419-9110-2_2
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