ﻻ يوجد ملخص باللغة العربية
Results of $UBVRIJHKLM$ photometry and $VRI$ polarimetry of a young star RW Aur A observed during unprecedented long and deep (up to $Delta V approx 5$ mag) dimming events in 2010-11 and 2014-18 are presented. The polarization degree $p$ of RW Aur A at this period has reached 30 per cent in the $I$ band. As in the case of UX Ori type stars (UXORs), the so-called bluing effect in the colour-magnitude $V$ versus $V-R_{rm c},$ $V-I_{rm c}$ diagrams of the star and a strong anticorrelation between $p$ and brightness were observed. But the duration and the amplitude of the eclipses as well as the value and orientation of polarization vector in our case differ significantly from that of UXORs. We concluded that the dimmings of RW Aur A occurred due to eclipses of the star and inner regions of its disc by the axisymmetric dust structure located above the disc and created by the disc wind. Taking into account both scattering and absorption of stellar light by the circumstellar dust, we explain some features of the light curve and the polarization degree - magnitude dependence. We found that near the period of minimal brightness mass-loss rate of the dusty wind was $> 10^{-9}$ M$_odot$ yr$^{-1}.$
RW Aur is a young binary system showing strong signatures of a recent tidal encounter between the circumprimary disk and the secondary star. The primary star has recently undergone two major dimming events ($Delta$mag $approx$ 2 in V-band), whose ori
Results of UBVRIJHKLM photometry, VRI polarimetry and optical spectroscopy of a young star RW Aur A obtained during 2010-11 and 2014-16 dimming events are presented. During the second dimming the star decreased its brightness to Delta V > 4.5 mag, po
Resolved UBVRI photometry of RW Aur binary was performed on November 13/14, 2014 during the deep dimming of RW Aur with a newly installed 2.5 meter telescope of the Caucasus observatory of Lomonosov Moscow State University at the mount Shatzhatmaz. A
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 jets knots have emerged $approx 350$ yr ago. We argue that at that moment the jet itself has appeared and intensive accretion
RW Aur is a young binary star that experienced a deep dimming in 2010-11 in component A and a second even deeper dimming from summer 2014 to summer 2016. We present new unresolved multi-band photometry during the 2014-16 eclipse, new emission line sp