In the framework of classical mechanics, the problem of numerical modeling of the evolution of a cluster of a finite number of gravitating bodies with allowance for gravitational accretion is considered. Numerical simulation showed that the characteristic shape of the curve of the "rotation curve" of stars of certain galaxies is determined only by the current configuration of the orbits of bodies and their masses. This means that there is no need to introduce some "dark matter" into consideration, and there is also no need to modify Newton's classical law on the gravitational interaction of two material bodies. When modeling the dynamics of a finite number of gravitating bodies, the possibility of a collision of bodies was taken into account, and the impact is assumed to be absolutely inelastic. Exterior, with respect to the cluster of bodies under consideration, the force actions of any nature were excluded. Of all the internal force factors acting in the cluster, only gravitational interaction is considered. The problems of determining the natural initial conditions for solving the Cauchy problem for a given time interval are touched upon.
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[v1] 2018-08-30 11:42:35
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