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Equations of State

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Stellar Interiors

Part of the book series: Astronomy and Astrophysics Library ((AAL))

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 nearly any 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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3.9 References and Suggested Readings

Introductory Remarks

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§3.3: Ideal Monatomic Gas

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§3.4: The Saha Equation

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Author information

Authors and Affiliations

  1. Astrophysics and Planetary Sciences, University of Colorado, Boulder, CO, 80309-0440, USA

    Carl J. Hansen

  2. Departments of Physics and Astronomy, Iowa State University, Ames, IA, 50011, USA

    Steven D. Kawaler

  3. Department of Astronomy, University of Maryland, College Park, MD, 20740, USA

    Virginia Trimble

  4. Department of Physics, University of California, Irvine, Irvine, CA, 92717, USA

    Virginia Trimble

Authors
  1. Carl J. Hansen
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  2. Steven D. Kawaler
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  3. Virginia Trimble
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© 2004 Springer Science+Business Media New York

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Hansen, C.J., Kawaler, S.D., Trimble, V. (2004). Equations of State. In: Stellar Interiors. Astronomy and Astrophysics Library. Springer, New York, NY. https://doi.org/10.1007/978-1-4419-9110-2_3

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  • DOI: https://doi.org/10.1007/978-1-4419-9110-2_3

  • Publisher Name: Springer, New York, NY

  • Print ISBN: 978-1-4612-6497-2

  • Online ISBN: 978-1-4419-9110-2

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