Models of Magnetospheric Accretion onto Young Stars in the Absence of Ionization Equilibrium

The formation of hydrogen emission lines in the magnetospheres of young stars is considered. The magnetosphere is assumed to be formed by a dipole magnetic field whose axis is aligned with the stellar rotation axis. The radiative transfer in spectral lines is considered in the Sobolev approximation with nonlocal radiative coupling. We have taken into account the effect of gas ionization fraction transfer when moving in the magnetosphere, demonstrated its influence on the emission spectrum of the magnetosphere for the first time, and estimated the accretion rate from the \(\mathrm{H\alpha}\) line. We have shown that at low accretion rates \(\dot{M}\lesssim 10^{-9}\ {M_{\odot}}\) yr\({}^{-1}\) this effect can exert a significant influence on the model intensities.