  Twisted magnetic fields are frequently seen to emerge above the visible
surface of the Sun. This emergence is usually associated with the rise of
buoyant magnetic flux structures. Here we ask how magnetic fields from a
turbulent large-scale dynamo appear above the surface if there is no magnetic
buoyancy. The computational domain is split into two parts. In the lower part,
which we refer to as the turbulence zone, the flow is driven by an assumed
helical forcing function leading to dynamo action. Above this region, which we
refer to as the exterior, a nearly force-free magnetic field is computed at
each time step using the stress-and-relax method. Twisted arcade-like field
structures are found to emerge in the exterior above the turbulence zone.
Strong current sheets tend to form above the neutral line, where the vertical
field component vanishes. Time series of the magnetic field structure show
recurrent plasmoid ejections. The degree to which the exterior field is force
free is estimated as the ratio of the dot product of current density and
magnetic field strength to their respective rms values. This ratio reaches
values of up to 95% in the exterior. A weak outward flow is driven by the
residual Lorentz force.
