2020/09/30 by Shao-Peng Tang, Jin-Liang Jiang, Wei-Hong Gao +2
Earth and Planetary Sciences · Physics and Astronomy · #Astrophysics #Equation of state #Excited state #Gamma-ray bursts and supernovae #Gravitational wave #High-pressure geophysics and materials #Neutron star #Nuclear physics #Particle physics #Phase transition #Physics #Pulsars and Gravitational Waves Research #Quantum mechanics #astro-ph.HE #gr-qc #nucl-th
paper · pdf · doi:10.1103/physrevd.103.063026
published as Phys. Rev. D 103, 063026 (2021) · 9 pages, 5 figures, published in PRD
openalex publication_date 2021/03/19 · arxiv created 2021/03/20 · arxiv updated 2021/03/23 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
The equation of state (EoS) of the neutron star (NS) matter remains an enigma. In this work we perform the Bayesian parameter inference with the gravitational wave data (GW170817) and mass-radius observations of some NSs (PSR J0030+0451, PSR J0437\ensuremath-4715, and 4U 1702-429) using the phenomenologically constructed EoS models to search for a potential first-order phase transition. Our phenomenological EoS models take the advantages of current widely used parametrizing methods, which are flexible enough to resemble various theoretical EoS models. We find that the current observation data are still not informative enough to support/rule out phase transition, due to the comparable evidences for models with and without phase transition. However, the bulk properties of the canonical 1.4 M_\ensuremath\bigodot NS and the pressure at around 2\ensuremathρsat are well constrained by the data, where \ensuremathρsat is the nuclear saturation density. Moreover, strong phase transition at low densities is disfavored, and the 1\ensuremathσ lower bound of transition density is constrained to 1.84\ensuremathρsat.