2018/05/31 by Michał Marczenko, David Blaschke, D. Blaschke +3 · 63 citations
Physics and Astronomy · #Astrophysics #Deconfinement #Hadron #High-Energy Particle Collisions Research #Neutron star #Nuclear physics #Nucleon #Particle physics #Physics #Pulsars and Gravitational Waves Research #Quantum Chromodynamics and Particle Interactions #Quark #astro-ph.HE #hep-ph #nucl-th
paper · pdf · doi:10.1103/physrevd.98.103021
published in Physical review. D/Physical review. D. 98(10) (American Physical Society) · version accepted for publication in Phys. Rev. D
arxiv created 2018/11/12 · openalex publication_date 2018/11/26 · arxiv updated 2018/12/05 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We investigate the equation of state for the recently developed hybrid quark-meson-nucleon model under neutron-star conditions of \ensuremathβ-equilibrium and charge neutrality. The model has the characteristic feature that, at increasing baryon density, the chiral symmetry is restored within the hadronic phase by lifting the mass splitting between chiral partner states, before quark deconfinement takes place. Most important for this study are the nucleon (neutron, proton) and N(1535) states. We present different sets for two free parameters, which result in compact star mass-radius relations in accordance with modern constraints on the mass from PSR J0348+0432 and on the compactness from GW170817. We also consider the threshold for the direct Urca process for which a new relationship is given, and suggest as an additional constraint on the parameter choice of the model that this process becomes operative at best for stars with masses above the range for binary radio pulsars, M>1.4 M_\ensuremath\bigodot.