Variations in structure and rotations of convection zone with cycle phase and their relationship with dynamics of magnetic fields

To predict solar cycles, it is necessary to understand the physical processes contributing to solar activity. Adequate description and modern models of a solar cycle require detailed knowledge of the internal dynamics of the solar plasma and magnetic field formation in the convection zone of the Sun. Helioseismology using new observation data from the SOHO space observatory made it possible to gain insight into this region that is hard-to-reach for conventional observations and investigate characteristic flows and physical parameters, such as stratification, meridional circulation, differential rotation, helicity, etc. Meridional circulation; zonal flows; local variations in velocity, arising during sunspot formation; and the depth distribution of differential rotation are important factors in constructing the solar cycle pattern. Observation of the photospheric magnetic field indicates its internal nature. The dynamics, formation, and dissipation of this field are manifestations of the global process involving all layers of the Sun, beginning with the convection zone and including the corona. In this work, we briefly reviewed the state of art of the problem of the internal dynamics of solar activity.