Abstract
We confront admixture of dark matter inside neutron star using gravitational wave constraints coming from binary neutron star merger. We consider a relativistic mean field model including $\sigma-\omega-\rho$ meson interaction with NL3 parameterization. We study fermionic dark matter interacting with nucleonic matter via Higgs portal mechanism. We show that admixture of dark matter inside the neutron star soften the equation state and lower the value of tidal deformability. Gravitational wave GW170817 observation puts an upper bound on tidal deformability of a binary neutron star with low spin prior at 90\% confidence level, which disfavors stiff equation of state such as Walecka model with NL3 parameterization. However, we show that Walecka model with NL3 parameterization with a fermionic dark matter component satisfy the tidal deformability bound coming from the GW170817 observation.
Highlights
Compact objects like neutron stars (NS) are nature’s laboratory which can shed light directly or indirectly on the different branches of physics such as low energy nuclear physics, QCD under extreme conditions, the general theory of relativity etc
We show that the Walecka model with NL3 parametrization with a fermionic dark matter component satisfies the tidal deformability bound coming from the GW170817 observation
One can see from this plot that equation of state (EoS) given by the NL3 parametrization without dark matter component can be excluded at 90% confidence level using the upper bound on tidal deformability of a binary system
Summary
Compact objects like neutron stars (NS) are nature’s laboratory which can shed light directly or indirectly on the different branches of physics such as low energy nuclear physics, QCD under extreme conditions, the general theory of relativity etc. [32] authors have considered possible effects of a self-interacting dark matter core on the maximum mass of a neutron star, mass-radius relation and on the NS tidal deformability parameter. They have computed radial density and pressure profiles of the baryonic and dark matter components for different nuclear EoS and different dark matter fractions. [35], the authors have considered the Walecka relativistic mean field model including σ − ω interaction for the nucleonic part [2,3,5,6] and fermionic dark matter inside the neutron star.
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