Exploring the Distribution and Impact of Bosonic Dark Matter in Neutron Stars

Author:

Rafiei Karkevandi Davood12ORCID,Shahrbaf Mahboubeh34ORCID,Shakeri Soroush12ORCID,Typel Stefan56ORCID

Affiliation:

1. Department of Physics, Isfahan University of Technology, Isfahan 84156-83111, Iran

2. ICRANet-Isfahan, Isfahan University of Technology, Isfahan 84156-83111, Iran

3. Incubator of Scientific Excellence—Centre for Simulations of Superdense Fluids, University of Wroclaw, 50-204 Wroclaw, Poland

4. Frankfurt Institute for Advanced Studies, Ruth-Moufang-Str. 1, D-60438 Frankfurt am Main, Germany

5. Fachbereich Physik, Institut für Kernphysik, Technische Universität Darmstadt, Schlossgartenstraße 9, D-64289 Darmstadt, Germany

6. GSI Helmholtzzentrum für Schwerionenforschung GmbH, Theorie, Planckstraße 1, D-64291 Darmstadt, Germany

Abstract

The presence of dark matter (DM) within neutron stars (NSs) can be introduced by different accumulation scenarios in which DM and baryonic matter (BM) may interact only through the gravitational force. In this work, we consider asymmetric self-interacting bosonic DM, which can reside as a dense core inside the NS or form an extended halo around it. It is seen that depending on the boson mass (mχ), self-coupling constant (λ) and DM fraction (Fχ), the maximum mass, radius and tidal deformability of NSs with DM admixture will be altered significantly. The impact of DM causes some modifications in the observable features induced solely by the BM component. Here, we focus on the widely used nuclear matter equation of state (EoS) called DD2 for describing NS matter. We show that by involving DM in NSs, the corresponding observational parameters will be changed to be consistent with the latest multi-messenger observations of NSs. It is seen that for mχ≳200 MeV and λ≲2π, DM-admixed NSs with 4%≲Fχ≲20% are consistent with the maximum mass and tidal deformability constraints.

Publisher

MDPI AG

Reference91 articles.

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