Modelling the spectral energy distributions of the accretion disks of young stars with fossil magnetic field

This work focuses on the study of the thermal structure and observational appearance of the accretion discs of young stars that possess fossil magnetic fields. We analyse the influence of magnetohydrodynamics (MHD) effects on the disc temperature and its spectral energy distribution (SED). The simulations indicate that, with low accretion rates of $\dot{M} < 10^{-8}$ $M_{\odot}$/yr, Ohmic heating leads to an increase in the disc temperature by 100 K near the inner boundary. This effect causes an increase in the radiation flux of the disc in the mid-infrared range.