ИСТИНА

Components of a visual young binary RW Aur AB recently had a close encounter. It is assumed that subsequent enhancement of the disk accretion rate onto RW Aur A, the appearance of its HH-229 jet and dusty disk wind are the consequences of rearrangement of inner regions of RW Aur A's protoplanetary disk caused by the fly-by of the companion RW Aur B. However nothing was known about the effect of the fly-by on the inner regions of RW Aur B's disk. We present here results of our photometric, olarimetric and spectral observations of RW Aur B, and conclude that activity of the star differ significantly from that of RW Aur A. Posssible reasons of the difference are discussed.