Speaker
Description
We study the physical properties of the interacting processes between the components of two double white dwarf binary stars, V803 Cen and CR Boo, depending on the evolutionary stages for each of the two targets, separately. Both objects are semi-detached binaries, influenced by the mass transfer mechanism. The initial conditions suggest disturbances in the flow parameters, followed by instabilities in the mass transfer. The resulting flow morphology in the interacting area, where the stream from the secondary meets the initial accreting matter onto the primary is examined. As a result, we expect for an unstable accretion disc configuration or non-disc formation to be obtained. In presumptive relation to the two targets activity, we have checked their observational data. We have found the brightness variations in the light curves of both objects for different periods.
