  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.
