Mechanism, Dynamics and Evolution of Small-Scale Dynamo on the Sun

Dynamo processes on the Sun are a key for understanding various observed phenomena on different scales. Even during the deepest activity minima the Sun is covered by a carpet of small-scale magnetic structures, generated by local turbulent dynamo. Such `magnetic carpet' can be a source of atmospheric heating and solar wind. We present a series of 3D radiative MHD simulations of the small-scale dynamo for realistic solar conditions and various properties of seed field. Our simulation results reveal the dynamo mechanism of amplification of initially extremely weak seed fields (0.001-10 milliGauss) to kiloGauss bipolar structures, which operates in a shallow subsurface turbulent layer of the Sun. We discuss turbulent properties of the solar magnetoconvection and energy exchange on different scales, leading to the processes of generation and amplification of the magnetic fields. A detailed comparison of the simulation results with observations from space (IRIS, Hinode and SDO) and ground-based observatories (NST/BBSO) allows us to develop a multi-wavelength approach to calibration of observational data and reconstruction of magnetic field topologies on the Sun.