Strange stars admixed with dark matter: equiparticle model in a two fluid approach

TL;DR

This paper investigates the structure and stability of strange stars mixed with dark matter using a two-fluid model, incorporating phenomenological quark models and dark matter interactions, and compares results with recent astrophysical observations.

Contribution

It introduces a two-fluid approach to model strange stars with dark matter, considering both fermionic and bosonic dark sectors with in-medium effects and repulsive interactions.

Findings

Stable strange star configurations compatible with NICER data.

Dark matter halos can form around strange stars at low dark particle masses.

Bosonic dark matter models help prevent stellar collapse.

Abstract

In this work, we explore the possible scenario of strange stars admixed with fermionic or bosonic dark matter. For the description of the ``visible'' sector, we use a specific phenomenological quark model that takes into account in-medium effects for the quark masses through a suitable baryonic density dependence, in which the free parameters are chosen from the analysis of the stellar matter stability window (parametrizations presenting lower energy per baryon than iron nuclei). In the case of the dark sector, we investigate the predictions of fermionic and bosonic models. In the former, we consider a spin $1/2$ dark particle, and the latter is described by a dark scalar meson. Both models present a repulsive vector interaction, particularly important for the bosonic model since it helps avoid the collapse of the star due to the lack of degeneracy pressure. Our results point out possible stable strange stars configurations in agreement with data from the NASA NICER measurements of the pulsars PSR J0030+0451 and PSR J0740+6620, including the latest observational data, as well as the observed HESS J1731-347 mass-radius relationship. As another feature, we find stars with dark matter halo configurations for lower values of the dark particle mass.