We present a hydrodynamic model describing the evolution of a supernova remnant within the vicinity of a galactic centre, influenced by the wind of a young nuclear star cluster. The aim of this model is to test the hypothesis that such remnants can deliver mass accreted onto their expanding shells onto supermassive black holes, thereby contributing to their rapid growth. We apply this model to study Sgr A East, the supernova remnant closest to the centre of the Milky Way. Firstly, we explore parameter space using a simplified hydrodynamic code called RING, based on the thin shell approximation. Subsequently, we use the adaptive mesh refinement code FLASH to perform detailed simulations of the most promising scenarios and compare them to the observations of Sgr A East.
