  We examine the generation of a magnetic field in a solar-like star and its
effects on the internal distribution of the angular velocity. We suggest that
the evolution of a rotating star with magnetic fields leads to an equilibrium
value of the differential rotation. This equilibrium is determined by the
magnetic coupling, which favours a constant rotation profile, and meridional
circulation which tends to build differential rotation. The global equilibrium
stage is close to solid body rotation between about 0.7 and 0.2 R_sun, in good
agreement with helioseismic measurements.
