Abstract:
For a satisfactory understanding of the solar magnetic phenomena it may be advantageous first to interrelate phenomenologically observations involving different scales of length and time and in different layers of the solar atmosphere as, for example, in Piddington's model (1975a, 1976a, b, c).
As a first step towards the construction of such a phenologically model it is tentatively concluded that a large number of the solar magnetic phenomena may be due to the rise of 'fundamental flux tubes' of magnetic fluxes ~ 10(power 17) - 10(power 18) Mx (FFT's) presumably originating in large (>10 (power 5)km) depths in the convection zone and rising across the observable layers of the solar atomosphere through bends of successively large sizes.
Such a conclusion poses several theoretical questions. As plausible answers to three of these questions it is shown that: (i) FFT's may provide the most efficient convection of energy transferred to them by convective flows in the large depths, (ii) the thermal diffusion and the heating associated with the just mentioned energy transfer may be adequate to raise the FFT from an equilibrium in 'large' depths to 'moderate' (<10 (power 5) km) depths in a time scale comparable to ~ 1y, and (iii) in the large depths the diffusion of the magnetic flux in an FFT might take place on time scales ~3y.
