Abstract
Already in the very early days of the Schrodinger equation it was recognized that quantum theory was required to resolve problems of dense matter. Here a model star of non-relativistic neutrons which interact pairwise by the gravitational 1/r-potential is dealt with as a whole by quantum statistical mechanics. In an appropriate thermodynamic limit the free energy is given by Thomas-Fermi theory. The model neutron star undergoes a phase transition of first order if it cools down below a transition temperature.
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References
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© 1977 Springer-Verlag
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Hertel, P. (1977). The Schrödinger Equation and Cosmic Bodies. In: Thirring, W., Urban, P. (eds) The Schrödinger Equation. Acta Physica Austriaca, vol 17/1977. Springer, Vienna. https://doi.org/10.1007/978-3-7091-7673-3_10
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DOI: https://doi.org/10.1007/978-3-7091-7673-3_10
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