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Our aim is to study the evolution of the orbit of a star under the influence of interactions with an accretion disc in an AGN. The model considered consists of a low-mass compact object orbiting a supermassive black hole and colliding periodically with the accretion disc. Approximate calculations based mostly on the Newtonian theory of gravity have been carried out by several authors, to estimate the effects of circularization of initially eccentric orbits and their dragging into the disc plane. Here, we present the first step towards a more adequate general relativistic approach in which the gravitational field of the nucleus is described by the Kerr metric

A star orbiting around a supermassive rotating black hole: free motion and corrections due to star-disc collisions