Neutron Stars in Rastall Gravity
Résumé
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 bound on the non-GR behaviour of the Rastall theory which should be $\lesssim 0.1\%$ level. This work presents the more stringent contraints on the deviations of GR caused by the Rastall proposal.
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