Abstract
The equations of state appropriate to the interiors of most stars are simple in one major respect: they may be derived using the assumption that the radiation, gas, fluid, or even solid, is in a state of local thermodynamic equilibrium or LTE. By this we mean that at a particular position in the star complete thermodynamic equilibrium is as very nearly true as we could wish. It is only near the stellar surface or in highly dynamic events, such as in supernovae, where this assumption may no longer be valid.
The worth of a State, in the long run, is the worth of the individuals composing it.
— John Stuart Mill (1806–1873)
What is Matter?—Never mind.
What is Mind?—no matter.
— from Punch (1855)
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References and Suggested Readings
Introductory Remarks
▹ Cox, J.P. 1968, Principles of Stellar Structure, in two volumes (New York: Gordon and Breach)
▹ Kippenhahn, R., and Weigert, A. 1990, Stellar Structure and Evolution (Berlin: Springer-Verlag).
▹ Landau, L.D., and Lifshitz, E.M. 1958, Statistical Physics (London: Pergamon)
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§3.3 Ideal Monatomic Gas
▹ Chandrasekhar S. 1939, An Introduction to the Study of Stellar Structure (Chicago: University of Chicago Press).
▹ Chiu, H.-Y. 1968, Stellar Physics, Vol. 1. (Waltham, MA: Blaisdell)
▹ Cox, J.P. 1968, Principles of Stellar Structure, in two volumes (New York: Gordon and Breach).
§3.4 The Saha Equation
▹ Cox, J.P. 1968, Principles of Stellar Structure, in two volumes (New York: Gordon and Breach)
▹ Kippenhahn, R., and Weigert, A. 1990, Stellar Structure and Evolution (Berlin: Springer-Verlag).
§3.4 Fermi-Dirac Equations of State
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▹ Antia, H.M. 1993, Ap.J.Supply 84, 101
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§3.4 “Almost Perfect” Equations of State
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§3.8 Exercises
▹ Allen, C.W. 1973, Astrophysical Quantities 3d ed. (London: Athlone)
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© 1994 Springer-Verlag New York, Inc.
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Hansen, C.J., Kawaler, S.D. (1994). Equations of State. In: Stellar Interiors. Astronomy and Astrophysics Library. Springer, New York, NY. https://doi.org/10.1007/978-1-4684-0214-8_3
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DOI: https://doi.org/10.1007/978-1-4684-0214-8_3
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