  Stellar winds are an integral part of the underlying dynamo, the motor of
stellar activity. The wind controls the star's angular momentum loss, which
depends on the magnetic field geometry which varies significantly in time and
latitude. Here we study basic properties of a self-consistent model that
includes simple representations of both the global stellar dynamo in a
spherical shell and the exterior in which the wind accelerates and becomes
supersonic. We numerically solve an axisymmetric mean-field model for the
induction, momentum, and continuity equations using an isothermal equation of
state. The model allows for the simultaneous generation of a mean magnetic
field and the development of a Parker wind. The resulting flow is transonic at
the critical point, which we arrange to be between the inner and outer radii of
the model. The boundary conditions are assumed to be such that the magnetic
field is antisymmetric about the equator, i.e., dipolar. At the solar rotation
rate, the dynamo is oscillatory and of $\alpha^2$ type. In most of the domain,
the magnetic field corresponds to that of a split monopole. The magnetic energy
flux is largest between the stellar surface and the critical point. The angular
momentum flux is highly variable in time and can reach negative values,
especially at midlatitudes. At rapid rotation of up to 50 times the solar
value, most of the magnetic field is lost along the axis within the inner
tangential cylinder of the model. The model reveals unexpected features that
are not generally anticipated from models that are designed to reproduce the
solar wind: highly variable angular momentum fluxes even from just an
$\alpha^2$ dynamo in the star. A major caveat of our isothermal models with a
magnetic field produced by a dynamo is the difficulty to reach small enough
plasma betas without the dynamo itself becoming unrealistically strong inside
the star.
