Abstract
Many astrophysical phenomena are associated with gas motion at relativistic velocities. The source of such currents are active galactic nuclei, microquasars, pulsars, gamma bursts, black holes, neutron stars, and gravitational waves. To study such phenomena, it is necessary to perform simulation within the scope of special relativistic hydrodynamics. One of the difficulties of modeling relativistic flows is the different scale of processes, which requires the use of both parallel computing and adaptive meshes.
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