Asymmetric Dark Stars and Neutron Star Stability
  We consider gravitationally bound states of asymmetric dark matter (ADM
stars), and the impact of ADM capture on the stability of neutron stars. We
derive and interpret the equation of state for ADM with both attractive and
repulsive interactions, and solve the Tolman-Oppenheimer-Volkoff equations to
find equilibrium sequences and maximum masses of ADM stars. Gravitational wave
searches can utilize our solutions to model exotic compact objects (ECOs). Our
results for attractive interactions differ substantially from those in the
literature, where fermionic ADM with attractive self-interactions was employed
to destabilize neutron stars more effectively than non-interacting fermionic
ADM. By contrast, we argue that fermionic ADM with an attractive force is no
more effective in destabilizing neutron stars than fermionic ADM with no
self-interactions.
