Neutron stars in $f(\mathtt{R,L_m})$ gravity with realistic equations of state: joint-constrains with GW170817, massive pulsars, and the PSR J0030+0451 mass-radius from ${\it NICER}$ data

TL;DR

This paper explores neutron stars within a modified gravity framework, demonstrating that the model can better fit observational data on neutron star masses and radii than general relativity, using realistic equations of state.

Contribution

The study introduces and solves hydrostatic equilibrium equations in $f(R,L_m)$ gravity with realistic equations of state, providing joint constraints from multiple astrophysical observations.

Findings

The model accommodates massive pulsars more effectively than GR.

It explains observed neutron star radii consistent with GW170817 and NICER data.

Mass-radius relations align with observational constraints for typical neutron star masses.

Abstract

In this work we investigate neutron stars (NS) in $f(\mathtt{R,L_m})$ theory of gravity for the case $f(\mathtt{R,L_m}) = \mathtt{R} + \mathtt{L_m} + \sigma\mathtt{R}\mathtt{L_m}$, where $\mathtt{R}$ is the Ricci scalar and $\mathtt{L_m}$ the Lagrangian matter density. In the term $\sigma\mathtt{R}\mathtt{L_m}$, $\sigma$ represents the coupling between the gravitational and particles fields. For the first time the hydrostatic equilibrium equations in the theory are solved considering realistic equations of state and NS masses and radii obtained are subject to joint constrains from massive pulsars, the gravitational wave event GW170817 and from the PSR J0030+0451 mass-radius from NASA's Neutron Star Interior Composition Explorer (${\it NICER}$) data. We show that in this theory of gravity, the mass-radius results can accommodate massive pulsars, while the general theory of relativity can hardly do it. The theory also can explain the observed NS within the radius region constrained by the GW170817 and PSR J0030+0451 observations for masses around $1.4~M_{\odot}$.