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 nonconservation 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-general relativity behavior of the Rastall theory which should be $\ensuremath{\lesssim}1%$ level. This work presents the more stringent constraints on the deviations of general relativity caused by the Rastall proposal.

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