# GW170817 constraints on the properties of a neutron star in the presence of WIMP dark matter

## TL;DR

This paper investigates how WIMP dark matter influences neutron star properties, using observational constraints from GW170817 to explore the effects on mass, radius, and other characteristics within a relativistic mean field framework.

## Contribution

It introduces a model incorporating DAMA/LIBRA suggested WIMP dark matter into neutron star equations-of-state and compares predictions with GW170817 data.

## Key findings

- Dark matter affects neutron star mass-radius relations
- Dark matter influences the moment of inertia and tidal deformability
- Results are consistent with GW170817 observations

## Abstract

The properties of a neutron star are studied in the presence of dark matter. We have considered a relatively light Weakly Interacting Massive Particle (WIMP) as a dark matter candidate with properties suggested by the results of the DAMA/LIBRA collaboration, realized for instance within the framework of the Next-to-Minimal Supersymmetric Standard Model. The dark matter particle interacts with the baryonic matter of a neutron star through Higgs bosons. The dark matter variables are essentially fixed using the results of the DAMA/LIBRA experiment, which are then used to build the Lagrangian density for the WIMP-nucleon interaction inside a neutron star. We have used the effective field theory motivated relativistic mean field model to study the equations-of-state in the presence of dark matter. The predicted equations-of-state are used in the Tolman-Oppenheimer-Volkoff equations to obtain the mass-radius relations, the moment of inertia, and effects of the tidal field on a neutron star. The calculated properties are compared with the corresponding data of the GW170817 event.