Disk Wind as A Source of Photometric Activity in Young Stars in The Optical and Infrared Regions of The Spectrum

The article investigates the influence of the dust component in magneto-centrifugal disk winds on circumstellar extinction and the infrared thermal emission of T Tauri stars. The study is based on MHD wind models developed by Safier. The stellar spectrum includes an accretion hotspot, whose luminosity is scaled according to the accretion rate and stellar parameters. Radiative transfer in the wind and circumstellar disk is calculated using the Monte Carlo method implemented in the RADMC3D code. The simulation results are applied to T Tauri stars exhibiting UX Ori-type variability. It is shown that when such stars are observed at small angles to the disk plane, an increase in the accretion rate can cause a reduction in their optical brightness while simultaneously enhancing their infrared (IR) emission. The results are also highly sensitive to the magnetic field topology in the disk’s wind-launching region.