Bosonic dark matter in neutron stars and its effect on gravitational wave signal

We study an impact of self-interacting bosonic dark matter (DM) on various observable properties of neutron stars (NSs). The analysis is performed for asymmetric DM with masses from few MeV to GeV, the self-coupling constant of order O (1 ) and various DM fractions. Allowing a mixture between DM and baryonic matter, the formation of a dense DM core or an extended dark halo has been explored. We find that both distribution regimes crucially depend on the mass and fraction of DM for sub-GeV boson masses in the strong coupling regime. From the combined analysis of the mass-radius relation and the tidal deformability of compact stars including bosonic DM, we set a stringent constraint on DM fraction. We conclude that observations of 2 M_⊙ NSs together with Λ_1.4≤580 constraint, set by LIGO/Virgo Collaboration, favor sub-GeV DM particles with low fractions below ∼5 %.