  Speckle interferometry of the young binary system RW Aur was performed with
the 6-m telescope of the Special Astrophysical Observatory of the Russian
Academy of Sciences using filters with central wavelengths of 550 nm and 800 nm
and pass-band halfwidths of 20 nm and 100 nm, respectively. The angular
separation of the binary components was 1.448"{\pm}0.005 and the position angle
of the system was 255.9{\deg}{\pm}0.3{\deg} at the observation epoch (JD 2 454
255.9). We find using published data that these values have been changing with
mean rates of +0.002"/yr and +0.02{\deg}/yr, respectively, over the past 70
years. This implies that the direction of the orbital motion of the binary
system is opposite to the direction of the disk rotation in RW Aur A. We
propose a physical model to explain the formation of circumstellar accretion
disks rotating in the reverse direction relative to young binary stars
surrounded by protoplanetary disks. Our model can explain the characteristic
features of the matter flow in RW Aur A: the high accretion rate, small size of
the disk around the massive component, and reverse direction of rotation.
