RMF-CC models with ωρ coupling better match multi-messenger NS data and LQCD/NEP constraints than the baseline, yet standard RMF remains preferred without core phase transitions, requiring high Ksat ~300 MeV.
Role of vector self-interaction in Neutron Star properties
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abstract
Previous studies have claimed that there exist correlations among certain nuclear saturation parameters and neutron star observables, such as the slope of the symmetry energy and the radius of a $1.4M_{\odot}$ neutron star. However, it is not clear whether such correlations are physical or spurious, as they are not observed universally for all equation of state models. In this work, we probe the role of vector self-interaction within the framework of the Relativistic Mean Field model and its role in governing the observable stellar properties and their correlations with nuclear parameters. We confirm that the effect of this term is not only to control the high density properties of the equation of state but also to govern such correlations. We also impose a limit on the maximum strength of the vector self-interaction using recent astrophysical data.
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Relativistic Mean Field Approach with Chiral Symmetry Breaking and Quark Confinement in the light of Astrophysical Observations
RMF-CC models with ωρ coupling better match multi-messenger NS data and LQCD/NEP constraints than the baseline, yet standard RMF remains preferred without core phase transitions, requiring high Ksat ~300 MeV.