Quarkyonic matter state of neutron stars

Abstract

This work extends our previous study of isospin symmetric quarkyonic matter to quarkyonic neutron matter which might be relevant to the inner cores of neutron stars. The vector-isovector $\rho$ mesons are introduced to the model mainly to account for isospin density interactions, just like $\omega$ meson for baryon density interactions. The modified Lagrangian still preserves approximate chiral symmetry which could be significantly broken at lower density. And new free parameters are fixed by adopting the experimental constraints on the symmetry energy and its slope at saturation density. Eventually, the pressure, mass-radius relation, and tidal deformability are explored in advance for the quarkyonic neutron stars. While the pressure and tidal deformability are well consistent with experimental and observational restrictions, the mass-radius relation is unable to reproduce the observed two solar mass of PSR J0740+6620.

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Cited by in corpus (5)

• Extended NJL model for baryonic matter and quark matter
• Bayesian inference of strangeon matter using the measurements of PSR J0437-4715 and GW190814
• Quarkyonic matter and quarkyonic stars in an extended RMF model
• Quarkyonic picture of isospin QCD
• First-order QCD transition in a primordial magnetic field