  We demonstrate that the radial magnetic-field component at the outer boundary
of the sunspot penumbra is about 550 Mx cm$^{-2}$ independent of the sunspot
area and the maximum magnetic field in the umbra. The mean magnetic-field
intensity in sunspots grows slightly as the sunspot area increases up to 500 --
1000 millionth of visual hemisphere (m.v.h.) and may reach about 900 -- 2000 Mx
cm$^{-2}$. The total magnetic flux weakly depends on the maximum field strength
in a sunspot and is determined by the spottedness, i.e. the sunspot number and
the total sunspot area; however, the relation between the total flux and the
sunspot area is substantially nonlinear. We suggest an explicit parametrization
for this relation. The contribution of the magnetic flux associated with
sunspots to the total magnetic flux is small, not achieving more than 20% even
at the maximum of the solar activity.
