  Comparing the images of the jet of the young star RW Aur A, separated by a
period of 21.3 years, we found that the outermost jet's knots have emerged
$\approx 350$ yr ago. We argue that at that moment the jet itself has appeared
and intensive accretion onto the star has began due to the rearrangement of its
protoplanetary disk structure caused by the tidal effect of the companion RW
Aur B. More precisely, we assume that the increase of accretion is a response
to changing conditions in the outer disk regions, which followed after the
sound wave, generated by these changes, crossed the disk in a radial direction.
The difference in the parameters of the blue and red lobes of the RW Aur A jet,
according to our opinion, is a result of the asymmetric distribution of the
circumstellar matter above and below the disk, due to a fly-by of the
companion. It was found from the analysis of RW Aur historical light curve that
deep and long $(\Delta t>150$ days) dimmings of RW Aur A observed after 2010
yr, had no analogues in the previous 110 years. We also associate the change in
the character of the photometric variability of the star with the rearrangement
of the structure of inner $(r<1$ a.u.) regions of its protoplanetary disk and
discuss why these changes began only 350 years after the beginning of the
active accretion phase.
