  We present an axisymmetric numerical model of a dynamo active accretion disc.
If the dynamo-generated magnetic field in the disc is sufficiently strong
(close to equipartition with thermal energy), a fast magneto-centrifugally
driven outflow develops within a conical shell near the rotation axis, together
with a slower pressure driven outflow from the outer parts of the disc as well
as around the axis. Our results show that a dynamo active accretion disc can
contribute to driving an outflow even without any external magnetic field. The
fast outflow in the conical shell is confined by the azimuthal field which is
produced by the dynamo in the disc and advected to the disc corona. This part
of the outflow has high angular momentum and is cooler and less dense than its
surroundings. The conical shell's half-opening angle is typically about 30
degrees near the disc and decreases slightly with height. The slow outflow is
hotter and denser.
