  We use a top-down holographic model for strongly interacting quark matter to
study the properties of neutron stars. When the corresponding Equation of State
(EoS) is matched with state-of-the-art results for dense nuclear matter, we
consistently observe a first order phase transition at densities between two
and seven times the nuclear saturation density. Solving the
Tolman-Oppenheimer-Volkov equations with the resulting hybrid EoSs, we find
maximal stellar masses in the excess of two solar masses, albeit somewhat
smaller than those obtained with simple extrapolations of the nuclear matter
EoSs. Our calculation predicts that no quark matter exists inside neutron
stars.
