The Observation Evidence of Gas Flow Features in Symbiotic Stars

The results of 2D gas dynamic calculations of non-adiabatic gas flow in symbiotic stars are submitted. It is shown, that the gas flow in symbiotic stars is characterized by presence of two bow shock waves, located in front of accreting star on the way of its orbital movement and between components of the system, as well as by spiral movement of accreting matter and existence of a steady accretion disk. The including of radiation cooling and heating into the gas dynamic model allowed to determine the fields of density, velocity and temperature of gaseous stream in the system, and, accordingly, to calculate the theoretical profiles of emission lines in framework of Sobolev approximation. The analysis of calculated emission profiles H_$\beta$ allows to determine the contribution of various areas of the flow into the structure of the emission line. The revealed line shape features and connected with them the gas flow ones for symbiotic stars with mass loss M₁<∼10^-7 M_⊕ /year allows to use the results of calculations for interpretation of observation.