

Paper: 
Gaseous Flows in Inner Regions of Circumbinary Disks
of T Tauri Stars 
Volume: 
459, 6th International Conference of Numerical Modeling of Space Plasma Flows (ASTRONUM 2011) 
Page: 
55 
Authors: 
Bisikalo, D. V.; Sytov, A. Y.; Fateeva, A. M.; Kaygorodov, P. V. 
Abstract: 
We present results of 2D and 3D numerical
simulations of the matter flow in the circumbinary disk of a
binary T Tauri star. It is shown that two bow shocks caused by the
supersonic motion of the binary components in the gas of the disk
are formed in the system. These bow shocks significantly change
the flow pattern. In particular, in the inner region of the system
the velocity distribution is far from the Keplerian one and the
flow structure is mainly governed by the bow shocks. Presence of
the stationary bow shocks leads to formation of a gap, rarefied
region in the circumbinary disk having a radius of ∼3 A (A
is the average binary separation) for systems with the zero
eccentricity and ∼3.2 A for systems with the larger
eccentricity. The angular momentum is removed from the system
mainly due to the bow shocks. As a consequence two spiral flows
form. Matter flows into the system only from the headon collision
point. The flow toward the low mass component is ∼ 1.5 times
higher than the same flow toward the massive component. At the
same time the interaction of the flow structure elements leads to
redistribution of the angular momentum and, consequently, to the
higher rate of accretion onto the massive component
(M_{1}/M_{2} ∼ 1.4). 



