Neutron Star Stability in Light of the Neutron Decay Anomaly
  A recent proposal suggests that experimental discrepancies on the lifetime of
neutrons can be resolved if neutrons decay to dark matter. At the same time it
has been demonstrated that such a decay mode would soften the nuclear equation
of state resulting in neutron stars with a maximum mass much below currently
observed ones. In this paper we demonstrate that appropriate dark matter-baryon
interactions can accommodate neutron stars with mass above 2 solar masses. We
also show that dark matter self-interactions could also help neutrons stars
reach 2 solar masses provided that dark matter is of asymmetric nature.
