2022A&A...668A..25V -
Astronomy and Astrophysics, volume 668A, 25 (2022/12-1)
Disk Evolution Study Through Imaging of Nearby Young Stars (DESTINYS): Scattered light detection of a possible disk wind in RY Tau.
VALEGARD P.-G., GINSKI C., DOMINIK C., BAE J., BENISTY M., BIRNSTIEL T., FACCHINI S., GARUFI A., HOGERHEIJDE M., VAN HOLSTEIN R.G., LANGLOIS M., MANARA C.F., PINILLA P., RAB C., RIBAS A., WATERS L.B.F.M. and WILLIAMS J.
Abstract (from CDS):
Context. Disk winds are an important mechanism for accretion and disk evolution around young stars. The accreting intermediate-mass T-Tauri star RY Tau has an active jet and a previously known disk wind. Archival optical and new near-infrared observations of the RY Tau system show two horn-like components stretching out as a cone from RY Tau. Scattered light from the disk around RY Tau is visible in the near-infrared, but not seen at optical wavelengths. In the near-infrared, dark wedges separate the horns from the disk, indicating that we may see the scattered light from a disk wind. Aims. We aim to test the hypothesis that a dusty disk wind could be responsible for the optical effect in which the disk around RY Tau is hidden in the I band, but visible in the H band. This could be the first detection of a dusty disk wind in scattered light. We also want to constrain the grain size and dust mass in the wind and the wind-launching region. Methods. We used archived Atacama-Large-Millimetre-Array (ALMA) and Spectro-Polarimetric High-contrast Exoplanet REsearch (SPHERE) I band observations combined with newly acquired SPHERE H band observations and available literature to build a simple geometric model of the RY Tau disk and disk wind. We used Monte Carlo radiative transfer modelling MCMax3D to create comparable synthetic observations that test the effect of a dusty wind on the optical effect in the observations. We constrained the grain size and dust mass needed in the disk wind to reproduce the effect from the observations. Results. A model geometrically reminiscent of a dusty disk wind with small micron to sub-micron-sized grains elevated above the disk can reproduce the optical effect seen in the observations. The mass in the obscuring component of the wind has been constrained to 1 × 10–9M⊙ ≤ M ≤ 5 × 10–8M⊙, which corresponds to a mass-loss rate in the wind of about ∼1 × 10–8M⊙ yr–1. Conclusions. A simple model of a disk wind with micron to sub-micron-sized grains elevated above the disk is able to prevent stellar radiation to scatter in the disk at optical wavelengths while allowing photons to reach the disk in the near-infrared. Estimates of mass-loss rate correspond to previously presented theoretical models and points towards the idea that a magneto-hydrodynamic-type wind is the more likely scenario.
Abstract Copyright:
© P.-G. Valegård et al. 2022
Journal keyword(s):
protoplanetary disks - radiative transfer - stars: individual: RY Tau - stars: winds, outflows
Simbad objects:
9
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