Neutron Stars in Rastall Gravity
  We calculate static and spherically symmetric solutions for the Rastall
modification of gravity to describe Neutron Stars (NS). The key feature of the
Rastall gravity is the non-conservation of the energy-momentum tensor
proportionally to the space-time curvature. Using realistic equations of state
for the NS interior we place a conservative bound on the non-GR behaviour of
the Rastall theory which should be $\lesssim 1\%$ level. This work presents the
more stringent constraints on the deviations of GR caused by the Rastall
proposal.
