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A theory of cold static superdense stars composed of two or more components is presented. In this theory the number of each independent component is treated as a conserved number in contrast to the usual theories of neutron stars in which only the total baryon number is treated so. With the help of the variational principle and the equations of general relativity, simultaneous equations for stellar structure are derived. These equations are solved numerically for a stellar model in which protons and neutrons are treated as independent components by neglecting the β-decay.
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Kodama et al. (1972) studied this question.
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