Structure of the accretion disk in symbiotic stars - The isothermal case

Details Structure of the accretion disk in symbiotic stars - The isothermal case Structure of the accretion disk in symbiotic stars - The isothermal case

Jun 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995azh....72..367b&link_type=abstract

Astronomicheskij Zhurnal, vol. 72, p. 367

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Symbiotic Stars, Accretion Disks, Isothermal Processes, Gas Dynamics, Radiant Cooling, Gas Flow, Shock Wave Profiles, Flow Characteristics

Scientific paper

Results of two-dimensional gas dynamic computations of gas flow in symbiotic stars are presented, with radiation cooling of gas in the forming accretion disk taken into consideration. As computations show, radiation cooling does not change qualitatively the picture of the flow in the vicinity of the accreting star. The structure of the accretion disk with lagging and leading spiral shock waves remains also unchanged. Radiation cooling affects to a great extent numerical values of flow parameters. As a result, the coefficient of accretion efficiency increases from 0.15 to 0.8. It is shown that alteration of the parameters of the binary does not significantly affect the picture of the flow or the structure of the accretion disk. Therefore, the computed structure of the flow seems to be typical for symbiotic stars.

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