ИСТИНА

Modern studies of the solar small-scale magnetic field suggest that helicity in the convective shell can play a significant role both in the global solar dynamo cycle and in the frequency of flare phenomena. However, there is no clear understanding of how magnetic and hydrodynamic helicities accumulate in a turbulent plasma flow, how they are transported along the spectrum, and what maintains the helicity balance. According to recent research Kazantsev-type dynamo models show that in short-time-correlated turbulence the magnetic helicity grows on small scales, followed by its sign separation. In this report, we investigate this issue using the shell approach: we demonstrate the growth of small-scale helicity in complex shell MHD models, compare the generation with the results of the Kazantsev approach, and qualitatively study the transfer of growing helicity along the spectrum towards large-scale turbulence. To do this, by parallelizing the process, we numerically implement and statistically analyze the processes that describe the transport of energies and helicity when a seed magnetic field is added to the initially stabilized hydrodynamic Kolmogorov spectrum. In this case, both the linear mode of generation, which is compared with the linear Weinstein-Kichatinov model, and the nonlinear mode of process stabilized due to the reverse influence of the magnetic field on the velocity field are investigated. This work was supported by the BASIS Foundation grant no. 21-1-3-63-1.