In previous sections we analyzed the effects of first-order and second-order phase transitions on the EOS of dense matter. Now let us discuss possible impact of these effects on neutron star structure. Unfortunately, the existence of exotic phases cannot be strictly proven by the present theory. Therefore, the question Is a specific exotic phase present in a neutron star core? can be answered only by unambiguous identification of signatures of this phase in neutron star observations.
We will pay special attention to the behavior of global stellar parameters just after the formation of a new phase in the stellar core. The general relativistic theory was developed by Haensel et al. (1986a) and Zdunik et al. (1987); its simpler Newtonian version had been presented earlier by Schaeffer et al. (1983).
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