Abstract
We study the interface effects of quark-hadron mixed phase in compact stars. The properties of nuclear matter are obtained based on the relativistic-mean-field model. For the quark phase, we adopt perturbation model with running quark masses and coupling constant. At certain choices of parameter sets, it is found that varying the quark-hadron interface tension will have sizable effects on the radii ($\Delta R \approx 600$ m) and tidal deformabilities ($\Delta \Lambda/\Lambda \approx 50\%$) of hybrid stars. These provide possibilities for us to constrain the quark-hadron interface tension with future gravitational wave observations as well as the ongoing NICER mission.
Highlights
With the first observation of gravitational waves from the binary neutron star merger event GW170817 [1,2], astrophysics has entered the multimessenger era
We investigate the interface effects of a quark-hadron mixed phase in hybrid stars
The properties of nuclear matter are obtained based on the relativistic mean-field model
Summary
With the first observation of gravitational waves from the binary neutron star merger event GW170817 [1,2], astrophysics has entered the multimessenger era. The sizes of the geometrical structures increase with the surface tension and will approach to the limit of Maxwell construction scenarios at σ > σc, i.e., bulk separation of quark and hadron phases, which suggests the nonexistence of a MP inside hybrid stars Such kind of structural differences due to the quarkhadron interface effects are expected to affect many physical processes in hybrid stars. It is found that the maximum mass, tidal deformabilities, and radii of hybrid stars increase with σ These provide possibilities for us to constrain the quark-hadron interface tension with future gravitational wave observations as well as the ongoing NICER mission. II, we present our theoretical framework, where the properties of nuclear matter and quark matter were obtained The properties of their mixed phases and the interface effects are investigated in Sec. III, where both the Gibbs and Maxwell constructions are adopted and examined for the properties of hybrid stars in Sec. III A.
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