Charged ρ Meson Condensate in Neutron Stars within RMF Models
Department of Theoretical Nuclear Physics, National Research Nuclear University (MEPhI), Kashirskoe sh. 31, Moscow 115409, Russia
Joint Institute for Nuclear Research, Joliot-Curie 6, Dubna 141980, Russia
Department of Physics, Matej Bel University, Tajovského 40, 97401 Banská Bystrica, Slovakia
Author to whom correspondence should be addressed.
Received: 30 November 2017 / Revised: 12 December 2017 / Accepted: 12 December 2017 / Published: 26 December 2017
Knowledge of the equation of state (EoS) of cold and dense baryonic matter is essential for the description of properties of neutron stars (NSs). With an increase of the density, new baryon species can appear in NS matter, as well as various meson condensates. In previous works, we developed relativistic mean-field (RMF) models with hyperons and
-isobars, which passed the majority of known experimental constraints, including the existence of a
neutron star. In this contribution, we present results of the inclusion of
-meson condensation into these models. We have shown that, in one class of the models (so-called KVOR-based models, in which the additional stiffening procedure is introduced in the isoscalar sector), the condensation gives only a small contribution to the EoS. In another class of the models (MKVOR-based models with additional stiffening in isovector sector), the condensation can lead to a first-order phase transition and a substantial decrease of the NS mass. Nevertheless, in all resulting models, the condensation does not spoil the description of the experimental constraints.
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Maslov, K.A.; Kolomeitsev, E.E.; Voskresensky, D.N. Charged ρ Meson Condensate in Neutron Stars within RMF Models. Universe 2018, 4, 1.
Maslov KA, Kolomeitsev EE, Voskresensky DN. Charged ρ Meson Condensate in Neutron Stars within RMF Models. Universe. 2018; 4(1):1.
Maslov, Konstantin A.; Kolomeitsev, Evgeni E.; Voskresensky, Dmitry N. 2018. "Charged ρ Meson Condensate in Neutron Stars within RMF Models." Universe 4, no. 1: 1.
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