Constraint on phase transition with the multimessenger data of neutron stars

Abstract

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 $\mathrm{J}0030+0451$, PSR $\mathrm{J}0437\ensuremath{-}4715$, 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 $1.4\text{ }\text{ }{M}_{\ensuremath{\bigodot}}$ NS and the pressure at around $2{\ensuremath{\rho}}_{\mathrm{sat}}$ are well constrained by the data, where ${\ensuremath{\rho}}_{\mathrm{sat}}$ is the nuclear saturation density. Moreover, strong phase transition at low densities is disfavored, and the $1\ensuremath{\sigma}$ lower bound of transition density is constrained to $1.84{\ensuremath{\rho}}_{\mathrm{sat}}$.