Massive Neutron Stars with Hadron-Quark Transition Core : phenomenological approach by "3-window model"

TL;DR

This paper introduces a phenomenological 3-window model to construct an equation of state for the hadron-quark transition in neutron stars, demonstrating that such stars can exceed two solar masses, aligning with recent observations.

Contribution

It presents a novel 3-window phenomenological approach to model the hadron-quark transition in neutron stars, enabling the prediction of massive neutron stars exceeding two solar masses.

Findings

Neutron stars with hadron-quark transition cores can surpass two solar masses.

The 3-window model successfully reproduces observed massive neutron stars.

The approach provides a new framework for studying dense matter in neutron stars.

Abstract

By a new approach introducing a "3-window model" and constructing phenomenologically an equation of state for the hadron-quark (HQ) transition region, possible maximum mass of neutron stars (NSs) is discussed. It is found that neutron stars (NSs) with HQ transition core are able to have a mass exceeding two-solar mass, consistent with massive NSs recently observed.