Twin stars and the stiffness of the nuclear equation of state: ruling out strong phase transitions below $1.7n_0$ with the new NICER radius measurements

TL;DR

This paper investigates how the stiffness of the nuclear equation of state affects neutron star properties, using recent NICER and gravitational wave data to rule out strong phase transitions below 1.7 times nuclear saturation density.

Contribution

It introduces a method to constrain the nuclear equation of state and phase transitions using combined NICER and gravitational wave observations.

Findings

Strong phase transitions below 1.7n_0 are ruled out by NICER data.

Certain effective nucleon masses are incompatible with GW170817 and phase transitions.

NICER measurements further constrain the stiffness of the EoS.

Abstract

We explore the connection between the stiffness of an hadronic equation of state (EoS) with a sharp phase transition to quark matter to its tidal deformability. For this we employ a hadronic relativistic mean field model with a parameterized effective nucleon mass to vary the stiffness in conjunction with a constant speed of sound EoS for quark matter. We compute multiple scenarios with phase transitions according to the four possible cases of a hybrid star EoS with a stable second branch. We demonstrate at the example of GW170817 how the effective nucleon mass can be constrained by using gravitational wave data. We find, that certain values of the effective nucleon mass are incompatible with GW170817 and a phase transition simultaneously. By using the recent NICER measurements of J0030+0451 at the $1\sigma$ level we constrain our results further and find that strong phase transitions with a visible jump in the mass-radius relation are ruled out at densities below 1.7 times saturation density.