Abstract
On the basis of the Thomas-Fermi approximation as a semi-classical mean-field method, by constructing hyperon-nucleon interaction, we find a phenomenological equation of state (EOS) for \(\beta\)-stable baryonic matter. Our findings have profound consequences for neutron stars (NS) properties and compositions. Among these consequences, strange hyperons in the baryonic structure produce a strong softening of the EOS and also reduce the corresponding maximum mass of neutron stars. We also study hadron-quark phase transition in the interior of neutron stars by using the MIT bag model for the quark phase. We have found that NS have a large population of baryons but they are not dense enough to form a pure quark phase structure in the interior.
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