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We present a model of a viscously evolving accretion disc around a magnetizedneutron star. The model features the varying outer radius of the hot ionizedpart of the disc due to cooling and the varying inner radius of the disc due tointeraction with the magnetosphere. It also includes hindering of accretion onthe neutron star because of the centrifugal barrier and irradiation of theouter disc and companion star by X-rays from the neutron star and disc. Whensetting inner boundary conditions, we take into account that processes at theinner disc occur on a time scale much less than the viscous time scale of thewhole disc. We consider three types of outflow from the disc inner edge: zerooutflow, one based on MHD calculations, and a very efficient propellermechanism. The light curves of an X-ray transient after the outburst peak canbe calculated by a corresponding, publicly available code. We compare observedlight curves of the 2013 burst of Aql X-1 in X-ray and optical bands withmodeled ones. We find that the fast drop of the $0.3-10$ keV flux can be solelyexplained by a radial shrinking of the hot disc. At the same time, models withthe neutron star magnetic field $>10^8$ G have better fits because theaccretion efficiency behaviour emphasizes the 'knee' on the light curve. Wealso find that a plato emission can be produced by a disc-reservoir withstalled accretion.

Physical modeling of viscous disc evolution around magnetized neutron star. Aql X-1 2013 outburst decay