The mathematical simulation of the magnetic field coronal loops evolution

The aim of the paper is modeling of the interaction between magnetic star and accretion disk under different coefficient of the disk magnetic diffusivity. It was found that this process goes on with quasi-periodic reconnection of the magnetic field coronal loops and plasmoid ejection. In the case of the ideal disk conductivity the evolution of the coronal magnetic field cames to the periodic outflow of angular momentum from the disk. In the case of the finite disk conductivity the configuration of the magnetic field was formed that total flux angular momentum from disk to corona is not far from zero.