  Violation of the axial synnetry of a magnetic field essentially modifies the
physics of the plasma outflow in the magnetosphere of rotating objects. In
comparison to the axisymmetric outflow, two new affects appear: more efficient
magnetocentrifugal acceleration of the plasma along particular field lines and
generation of MHD waves. Here, we use an ideal MHD approximation to study the
dynamics of a cold wind in the nonaxisymmetric magnetosphere. We obtain a
self-consistent analytical solution of the problem of cold plasma outflow from
a slowly rotating star with a slightly nonaxisymmetric magnetic field using
perturbation theory. In the axisymmetric (monopole-like) magnetic field, the
first term in the expansion of the terminating energy of the plasama in powers
of $\Omega$ is proportional to $\Omega^4$, where $\Omega$ is the angular
velocity of the central source. Violation of the axial symmetry of the magnetic
field crucially changes this dependence. The first correction to the energy of
the plasma becomes proportional to $\Omega$. Efficient magnetocentrifugal
acceleration occurs along the field lines curved initially in the direction of
the rotation. I argue that all necessary conditions for the efficient
magnetocentrifugal acceleration of the plasma exist in the radio pulsar
megnetosphere. We calculated the first correction of the rotational losses due
to the generation of the MHD waves and analysed the plasma acceleration by
these waves.
