# Properties of Neutron Stars with hyperon cores in parameterized hydrostatic conditions

## TL;DR

This study models neutron stars with hyperon cores using a parameterized hydrostatic approach, showing that even with a softer equation of state, such stars can reach observed maximum masses and align with gravitational wave data.

## Contribution

It introduces a parameterized TOV framework to analyze hyperon-rich neutron stars, demonstrating their compatibility with observed mass and radius constraints.

## Key findings

- Hyperon-inclusive EoS can produce neutron stars with masses around 2 solar masses.
- The model's radius estimates agree with gravitational wave observations.
- Softer EoS with hyperons still support massive neutron stars.

## Abstract

Models of neutron stars (NSs) with hyperon cores are constructed with an effective chiral model in mean-field approximation. The hyperon couplings are fixed by reproducing their experimentally determined binding energies. The impact of these couplings on population of different particles and the equation of state (EoS) are studied in this work. The global properties of NSs like gravitational mass, radius, baryonic mass and central density are calculated using parameterized Tolman-Oppenheimer-Volkoff equations (PTOV) with special emphasis on two effects of pressure - one contributing to total mass density and the other to self gravity of the star. We find that with PTOV solutions in static conditions, a softer EoS (including hyperons) can also lead to massive stellar configurations of NSs, which are in well agreement with the observed maximum mass bound of $\approx 2 M_{\odot}$ (PSR J0348-0432). Estimates of $R_{1.4}$ and $R_{1.6}$, obtained with the PTOV equations are consistent with the recent findings of the same from the data analysis of gravitational waves (GW170817) observation. Keywords: Neutron Star; Hyperons; Equation of State; parameterized Tolman-Oppenheimer-Volkoff equations