Abstract

In the present work we study the gravitational effects of condensed dark matter on strange stars. We consider self-interacting dark matter particles with properties consistent with current observational constraints, and dark matter inside the star is modeled as a Bose-Einstein condensate. We integrate numerically the Tolman-Oppenheimer-Volkoff equations in the two-fluid formalism assuming that strange stars are made of up to 4 percent dark matter. It is shown that for a mass of the dark matter particles in the range 50–160 MeV strange stars are characterized by a maximum mass and radius similar to the ones found for neutron stars.