http://arxiv.org/abs/1712.09094
We simulate the dynamics of slender magnetic flux tubes (MFTs) in the accretion disks of T Tauri stars. The dynamical equations of our model take into account the aerodynamic and turbulent drag forces, and the radiative heat exchange between the MFT and ambient gas. The structure of the disk is calculated with the help of our MHD model of the accretion disks. We consider the MFTs formed at the distances $0.027-0.8$ au from the star with various initial radii and plasma betas $\beta_0$. The simulations show that the MFT with weak magnetic field ($\beta_0=10$) rise slowly with speeds less than the sound speed. The MFTs with $\beta_0=1$ form outflowing magnetized corona of the disk. Strongly magnetized MFTs ($\beta_0=0.1$) can cause the outflows with velocities $20-50$ km s$^{-1}$. The tubes rise periodically over times from several days to several months according to our simulations. We propose that periodically rising MFTs can absorb stellar radiation and contribute to the IR-variability of Young Stellar Objects.
S. Khaibrakhmanov, A. Dudorov and A. Sobolev
Wed, 27 Dec 2017
40/56
Comments: accepted for publication in RAA