Аннотация:We consider several tracers of magnetic activity that separate cycle-dependent contributions
to the background solar magnetic field from those that are independent of the cycle.
The main message is that background fields include two relative separate populations. The background
fields with a strength up to 100 Mx cm-2 are very poorly correlated with the sunspot
numbers and vary little with the phase of the cycle. In contrast, stronger magnetic fields demonstrate pronounced cyclic behaviour. Small-scale solar magnetic fields demonstrate features of
fractal intermittent behaviour, which requires quantification. We investigate how the observational
estimate of the solar magnetic flux density B depends on resolution D in order to obtain
the scaling lnB_D = -k lnD + a in a reasonably wide range. The quantity k demonstrates cyclic
variations typical of a solar activity cycle. k depends on the magnetic flux density, i.e. the ratio
of the magnetic flux to the area over which the flux is calculated, at a given instant. The
quantity a demonstrates some cyclic variation, but it is much weaker than in the case of k. The
scaling is typical of fractal structures. The results obtained trace small-scale action in the solar
convective zone and its coexistence with the conventional large-scale solar dynamo based on
differential rotation and mirror-asymmetric convection. Here we discuss the message for solar
dynamo studies hidden in the above results.