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We investigate the effect of feeble interaction of dark matter (DM) withhadronic matter on the equation of state (EoS) and structural properties ofneutron stars (NSs) in static conditions. For the purpose we adopt theeffective chiral model for the hadronic sector and for the first time in thecontext of possible existence of DM inside NSs, we introduce DM-SM interactionthrough light new physics mediator. Moreover, the mass of DM fermion, themediator and the coupling are adopted from the self-interaction constraint fromBullet cluster and from present day relic abundance. Within the consideredframework, the work highlights the underlying stiffening of EoS in presence ofDM fermion of mass of the order of a few GeV compared to the no-DM scenario.Consequently, the maximum gravitational mass of NS is obtained consistent withthe bounds from the most massive pulsars which were not satisfied with thehadronic matter EoS alone. The estimates of radius and tidal deformability of1.4 $M_{\odot}$ NS and the tidal deformabilities of the individual componentsof the binary neutron stars (BNS) associated with GW170817 are all in goodagreement with the individual constraints obtained from GW170817 observation ofBNS merger.

Implications of Feebly Interacting Dark Sector on Neutron Star Properties and Constraints from GW170817