  The aim of this article is to study how the differential rotation of
solar-like stars is influenced by rotation rate and mass in presence of
magnetic fields generated by a convective dynamo. We use the ASH code to model
the convective dynamo of solar-like stars at various rotation rates and masses,
hence different effective Rossby numbers. We obtained models with either
prograde (solar-like) or retrograde (anti-solar-like) differential rotation.
The trends of differential rotation versus stellar rotation rate obtained for
simulations including the effect of the magnetic field are weaker compared with
hydro simulations ($\Delta \Omega \propto (\Omega/\Omega_{\odot})^{0.44}$ in
the MHD case and $\Delta \Omega \propto (\Omega/\Omega_{\odot})^{0.89}$ in the
hydro case), hence showing a better agreement with the observations. Analysis
of angular momentum transport revealed that the simulations with retrograde and
prograde differential rotation have opposite distribution of the viscous,
turbulent Reynolds stresses and meridional circulation contributions. The
thermal wind balance is achieved in the prograde cases. However, in retrograde
cases Reynolds stresses are dominant for high latitudes and near the top of the
convective layer. Baroclinic effects are stronger for faster rotating models.
