Mass-Radius Relationship of Neutron Stars Admixed with Fermionic Asymmetric Dark Matter

Abstract

In this work, we have investigated the mass-radius relationships of non-rotating and rotating configurations of pure hadronic stars mixed with self-interacting fermionic Asymmetric Dark Matter (ADM) within the two-fluid formalism of stellar structure equations in general relativity. We have taken the nuclear matter Equation of State (EoS) that is obtained from the density dependent M3Y effective nucleon-nucleon interaction. The mass of the dark matter particles is considered to be 1 GeV. The EoS of self-interacting dark matter is taken from two-body repulsive interactions of the scale of strong interactions with the dark matter mediator mass to be 100 MeV. We explore the conditions of equal and different rotational frequencies of nuclear matter and dark matter and find that the maximum mass of differentially rotating stars with self-interacting dark matter to be ∼ 1.94M ⊙ with radius ∼ 10.4 kms.