Majority of galactic centers contain a supermassive black hole (mass $10^5$--$10^{9,5}\,$$\mathrm{M_\odot}$), surrounded by a central stellar cluster. There is a probability of $10^{-5}$--$10^{-4}$ /galaxy/year that a star from such a cluster is scattered and brought in the proximity of the black hole, where it is disrupted by black hole's tidal force. Fate of the stellar debris depends on its total energy. Parts of the debris with positive energy are unbound and escape from the gravitational potential of the black hole. On the other hand, debris with negative total energy is bound and returns in the black hole's vicinity, where it forms an accretion disk, which may emit radiation for months to years. A key issue in understanding stellar tidal disruption events, disk formation and their light curves, is the amount of matter, which either falls in the black hole, forms a disk or escapes in the interstellar space. In my master's thesis I numerically modeled tidal disruption events. Simulations of tidal disruption events were done with the PHANTOM code, which is based on smoothed particle hydrodynamics method. In the calculations of the supermassive black hole's gravitational field I took into account relativistic corrections to the Newtonian potential. I carried out an analysis of the stellar debris after disruption. I focused on the mass fraction of the bound and unbound matter as well as their temporal dependance. Computations were performed for different types of trajectories (elliptic, parabolic, hyperbolic) and for different values of the penetration factor.
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