  We study the connections between the sun's convection zone and the evolution
of the solar wind and corona. We let the magnetic fields generated by a 2.5D
axisymmetric kinematic dynamo code (STELEM) evolve in a 2.5D axisymmetric
coronal isothermal MHD code (DIP). The computations cover an 11 year activity
cycle. The solar wind's asymptotic velocity varies in latitude and in time in
good agreement with the available observations. The magnetic polarity reversal
happens at different paces at different coronal heights. Overall sun's mass
loss rate, momentum flux and magnetic braking torque vary considerably
throughout the cycle. This cyclic modulation is determined by the latitudinal
distribution of the sources of open flux and solar wind and the geometry of the
Alfv\'en surface. Wind sources and braking torque application zones also vary
accordingly.

Solar and Stellar Astrophysics