Compact bifluid hybrid stars: Hadronic Matter mixed with self-interacting fermionic Asymmetric Dark Matter

TL;DR

This paper models hybrid stars composed of hadronic matter and self-interacting fermionic dark matter, analyzing their masses and radii under various rotational conditions using general relativity.

Contribution

It introduces a two-fluid formalism for hybrid stars with self-interacting dark matter and provides detailed calculations of their structural properties.

Findings

Maximum mass of differentially rotating hybrid stars is approximately 1.94 solar masses.

Rotational frequencies influence the mass-radius relationship of the hybrid stars.

Self-interacting dark matter significantly affects the star's maximum mass and radius.

Abstract

The masses and radii of non-rotating and rotating configurations of pure hadronic stars mixed with self-interacting fermionic Asymmetric Dark Matter are calculated within the two-fluid formalism of stellar structure equations in general relativity. The Equation of State (EoS) of nuclear matter is obtained from the density dependent M3Y effective nucleon-nucleon interaction. We consider dark matter particle mass of 1 GeV. The EoS of self-interacting dark matter is taken from two-body repulsive interactions of the scale of strong interactions. 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 $\sim 1.94 M_\odot$ with radius $\sim 10.4$ kms.