2020/05/31 by Cheng-Jun Xia, Toshiki Maruyama, Nobutoshi Yasutake +3 · 36 citations
Physics and Astronomy · #Astrophysical Phenomena and Observations #Astrophysics #Hadron #Mixed phase #Nuclear physics #Particle physics #Phase (matter) #Physics #Pulsars and Gravitational Waves Research #Quantum Chromodynamics and Particle Interactions #Quark #Stars #hep-ph #nucl-th
paper · pdf · doi:10.1103/physrevd.102.023031
published in Physical review. D/Physical review. D. 102(2) (American Physical Society)
openalex publication_date 2020/07/24 · arxiv created 2020/07/25 · arxiv updated 2020/07/29 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We investigate systematically the quark-hadron mixed phase in dense stellar matter and its influence on compact star structures. The properties of quark matter and hadronic matter are fixed based on various model predictions. Beside adopting constant values, the surface tension \mathrm\ensuremathΣ for the quark-hadron interface is estimated with the multiple reflection expansion method and equivparticle model. To fix the structures of quark-hadron pasta phases, a continuous dimensionality of the structure is adopted as proposed by Ravenhall et al. The corresponding properties of hybrid stars are then obtained and confronted with pulsar observations. It is found that the correlation between radius and tidal deformability in traditional neutron stars preserves in hybrid stars. For those permitted by pulsar observations, in almost all cases, the quark phase persists inside the most massive compact stars. The quark-hadron interface plays an important role in hybrid star structures once quark matter emerges. The surface tension \mathrm\ensuremathΣ estimated with various methods increases with density, which predicts stiffer equation of states (EOSs) for the quark-hadron mixed phase and increases the maximum mass of hybrid stars. With or without the emergence of quark matter, the obtained EOSs of hybrid star matter are close to each other at densities n\ensuremath\lesssim0.8 fm^\ensuremath-3, while larger uncertainty is expected at higher densities.