  Stationary and axisymmetric solutions of relativistic rotating stars with
strong mixed poloidal and toroidal magnetic fields are obtained numerically.
Because of the mixed components of the magnetic field, the underlying
stationary and axisymmetric spacetimes are no longer circular. These
configurations are computed from the full set of the Einstein-Maxwell
equations, Maxwell's equations and from first integrals and integrability
conditions of the magnetohydrodynamic equilibrium equations. After a brief
introduction of the formulation of the problem, we present the first results
for highly deformed magnetized rotating compact stars.
