Kavli Affiliate: Moritz Guenther
| First 5 Authors: Taichi Uyama, Michihiro Takami, Gabriele Cugno, Vincent Deo, Olivier Guyon
| Summary:
We present multi-epoch observations of the RY~Tau jet for H$alpha$ and
[ion{Fe}{2}] 1.644 micron~emission lines obtained with
Subaru/SCExAO+VAMPIRES, Gemini/NIFS, and Keck/OSIRIS in 2019–2021. These data
show a series of four knots within 1$arcsec$ consistent with the proper motion
of $sim0farcs3$~yr$^{-1}$. The spatial intervals between the knots suggest
the time intervals of the ejections of about 1.2, 0.7, and 0.7 years,
significantly shorter than those observed for other few active young stars.
These H$alpha$ images contrast with the archival VLT/SPHERE/ZIMPOL
observations from 2015, which showed only a single knot-like feature at
$sim0farcs25$. The difference between the 2015 and 2019–2021 epochs suggests
an irregular ejection interval within the six-year range. Such variations of
the jet ejection may be related to a short-term ($<$1 year) variability of the
mass accretion rate. We compared the peaks of the H$alpha$ emissions with the
ZIMPOL data taken in 2015, showing the brighter profile at the base
($<0farcs3$) than the 2020–2021 VAMPIRES profiles due to time-variable mass
ejection rates or the heating-cooling balance in the jet. This emission may be
alternatively attributed to stationary shock related to outflow collimation,
but a higher angular resolution is required to confirm its detailed origin.
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