The jet of the young star RW Aur A and related problems

Abstract

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.

arXiv commentaccepted by The Astrophysical Bulletin

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Cited by in corpus (10)

• Multiple Stellar Fly-Bys Sculpting the Circumstellar Architecture in RW Aurigae
• ASTRONIRCAM - infrared camera-spectrograph for Sternberg institute 2.5 METER TELESCOPE
• Analysis of colour and polarimetric variability of RW Aur A in 2010-2018
• Exploring the dimming event of RW Aur A through multi-epoch VLT/X-Shooter spectroscopy
• Laboratory modeling of jets from young stars using plasma focus facilities
• Optical dimming of RW Aur associated with an iron rich corona and exceptionally high absorbing column density
• Time-Variable Jet Ejections from RW Aur A, RY Tau and DG Tau
• The dimming of RW Auriga. Is dust accretion preceding an outburst?
• RW Aur B: a modest UX Ori type companion of the famous primary
• RW Aur A : SpeX Spectral Evidence for Differentiated Planetesimal Formation, Migration and Destruction in an 3 Myr Old Excited CTTS System