# Hybrid Stars in the Framework of the Local Nambu - Jona-Lasinio Model for Quark Matter

## TL;DR

This paper models hybrid neutron stars with quark cores using the local Nambu-Jona-Lasinio model and finds stable configurations with maximum masses around 2.05 solar masses, emphasizing the narrow density range for stability.

## Contribution

It introduces a combined approach using the NJL model for quark matter and an extended RMF model for hadron matter to analyze hybrid star stability and properties.

## Key findings

- Stable hybrid stars exist within a narrow central density range.
- Maximum hybrid star mass is approximately 2.05 solar masses.
- Quark cores in stable stars are very small, about 0.6 km in radius.

## Abstract

The integral parameters of neutron stars are studied taking into account the hadron-quark phase transition, which leads to the formation of a core of quark matter in the central part of a star. The quark matter is described using the local Nambu - Jona-Lasinio (NJL) model. The thermodynamic characteristics of the hadron matter are calculated in the framework of an extended version of the relativistic mean field (RMF) model that includes the contribution of the scalar-isovector $\delta$-meson effective field. A Maxwell construction is used to determine the parameters of the phase transition. It is shown that for the equation of state examined here, stable hybrid stars correspond to a narrow range of values for the central density. In our model hybrid stars lie on the same branch as neutron stars, so that a branch with a third family is not formed. It is shown that for the equation of state examined here, stable hybrid stars correspond to a narrow range of values for the central density $\rho_c\in(1.71 \div 1.73]\cdot 10^{15}$ g/cm$^3$. In our model hybrid stars lie on the same branch as neutron stars, so that a branch with a third family is not formed. The maximum mass of a stable hybrid star is found to be $M_{max} = 2.05 M_\odot$. The configuration with the maximum mass has a quark core with mass $M_{core} \approx 10^{-3} M_\odot$ and radius $R_{core} \approx 0.6$ km.

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Source: https://tomesphere.com/paper/1903.02957