  Generation and diffusion of the magnetic field on the Sun is a key mechanism
responsible for solar activity on all spatial and temporal scales - from the
solar cycle down to the evolution of small-scale magnetic elements in the quiet
Sun. The solar dynamo operates as a non-linear dynamical process and is thought
to be manifest in two types: as a global dynamo responsible for the solar cycle
periodicity, and as a small-scale turbulent dynamo responsible for the
formation of magnetic carpet in the quiet Sun. Numerous MHD simulations of the
solar turbulence did not yet reach a consensus as to the existence of a
turbulent dynamo on the Sun. At the same time, high-resolution observations of
the quiet Sun from Hinode instruments suggest possibilities for the turbulent
dynamo. Analysis of characteristics of turbulence derived from observations
would be beneficial in tackling the problem. We analyse magnetic and velocity
energy spectra as derived from Hinode/SOT, SOHO/MDI, SDO/HMI and the New Solar
Telescope (NST) of Big Bear Solar Observatory (BBSO) to explore the
possibilities for the small-scale turbulent dynamo in the quiet Sun.
