Abstract
Conservation of momentum provides the next basic differential equation of the stellar-structure problem. We will derive this in several steps of gradually increasing generality. The first assumes mechanical equilibrium (Sect. 2.1), the equation of motion for spherical symmetry follows in Sect. 2.4, while in Sect. 2.5 even the assumption of spherical symmetry is dropped. In Sect. 2.6 we briefly discuss general relativistic effects in the case of hydrostatic equilibrium.
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Notes
- 1.
Throughout this book we will use the terms perfect and ideal gas synonymously, as they describe the same physical concept.
References
Zeldovich, Ya. B., Novikov, I.D. (1971): Relativistic Astrophysics, Vol. I “Stars and Relativity” (University of Chicago Press, Chicago)
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© 2012 Springer-Verlag Berlin Heidelberg
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Kippenhahn, R., Weigert, A., Weiss, A. (2012). Conservation of Momentum. In: Stellar Structure and Evolution. Astronomy and Astrophysics Library. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-642-30304-3_2
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DOI: https://doi.org/10.1007/978-3-642-30304-3_2
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