Two-Dimensional Hydrodynamical Modeling of Mass Transfer in Semidetached Binaries with Asynchronously Rotating Components

Details Two-Dimensional Hydrodynamical Modeling of Mass Transfer in Semidetached Binaries with Asynchronously Rotating Components Two-Dimensional Hydrodynamical Modeling of Mass Transfer in Semidetached Binaries with Asynchronously Rotating Components

Dec 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003arep...47.1027n&link_type=abstract

Astronomy Reports, vol. 47, Issue 12, p.1027-1037

Astronomy and Astrophysics

Astronomy

1

Scientific paper

We have modeled the mass transfer in the three semidetached binaries U Cep, RZ Sct, and V373 Cas taking into account radiative cooling both implicitly and explicitly. The systems have asynchronously rotating components and high mass-transfer rates of the order of 10-6 M &sun;/yr; they are undergoing various stages of their evolution. An accreting star rotates asynchronously if added angular momentum is redistributed over the entire star over a time that exceeds the synchronization time. Calculations have indicated that, in the model considered, mass transfer through the point L1 is unable to desynchronize the donor star. The formation of an accretion disk and outer envelope depends on the component-mass ratio of the binary. If this ratio is of the order of unity, the flow makes a direct impact with the atmosphere of the accreting star, resulting in the formation of a small accretion disk and a relatively dense outer envelope. This is true of the disks in U Cep and V373 Cas. When the component-mass ratio substantially exceeds unity (the case in RZ Sct), the flow forms a large, dense accretion disk and less dense outer envelope. Taking into account radiative cooling both implicitly and explicitly, we show that a series of shocks forms in the envelopes of these systems.

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