Quarkyonic stars with isospin-flavor asymmetry

Abstract

We suggest an extension to isospin asymmetric matter of the quarkyonic model from McLerran and Reddy. This extension allows us to construct the $\beta$-equilibrium between quarks, nucleons and leptons. The concept of the quarkyonic matter originates from the large number of color limit for which nucleons are the correct degrees of freedom near the Fermi surface -- reflecting the confining forces -- while deep inside the Fermi sea quarks naturally appear. In isospin asymmetric matter, we suggest that this new concept can be implemented within a global isoscalar relation between the shell gaps differentiating the nucleon and the quark sectors. In addition, we impose the conservation of the isospin-flavor asymmetry in the nucleon and the quark phases. Within this model, several quarkyonic stars are constructed on top of the SLy4 model for the nucleon sector, producing a bump in the sound speed, which implies that quarkyonic stars are systematically bigger and have a larger maximum mass than the associated neutron stars. They also predict lower proton fraction at $\beta$-equilibrium, which potentially quenches fast cooling in massive compact stars.

arXiv comment11 pages, 9 figures

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Cited by in corpus (14)

• On the Sound Speed in Neutron Stars
• An updated nuclear-physics and multi-messenger astrophysics framework for binary neutron star mergers
• Investigating Signatures of Phase Transitions in Neutron-Star Cores
• Impact of large-mass constraints on the properties of neutron stars
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• Interacting $ud$ and $uds$ quark matter at finite densities and quark stars
• Isospin asymmetry in holographic baryonic matter
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