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A treatment is given of stars of intermediate density such as dense red dwarfs and subdwarfs, using the statistical method of Thomas-Fermi to calculate the free-electron density, the gas pressure, and the opacities. The Thomas-Fermi equation has been generalized to take account of the high temperature and a mixture of elements. By taking ñnite boundary conditions as for metals, it is then possible to integrate the star equations
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Marshak et al. (1940) studied this question.
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