Dynamics of magnetic flux tubes and IR-variability of Young Stellar Objects

TL;DR

This paper models the dynamics of magnetic flux tubes in T Tauri star disks, showing how their rise and outflows can explain IR variability in young stellar objects.

Contribution

It introduces a detailed simulation of magnetic flux tube behavior considering drag and heat exchange, linking flux tube dynamics to IR variability in young stars.

Findings

Weak magnetic flux tubes rise slowly and form coronae.

Moderately magnetized tubes create outflows and influence disk structure.

Strong flux tubes drive high-velocity outflows and periodic IR variability.

Abstract

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.