  We investigate the differences between an outflow in a highly-resistive
accretion disk corona, and the results with smaller or vanishing resistivity.
For the first time, we determine conditions at the base of a two-dimensional
radially self-similar outflow in the regime of very large resistivity. We
performed simulations using the {\sc pluto} magnetohydrodynamics code, and
found three modes of solutions. The first mode, with small resistivity, is
similar to the ideal-MHD solutions. In the second mode, with larger
resistivity, the geometry of the magnetic field changes, with a "bulge" above
the super-fast critical surface. At even larger resistivities, the third mode
of solutions sets in, in which the magnetic field is no longer collimated, but
is pressed towards the disk. This third mode is also the final one: it does not
change with further increase of resistivity. These modes describe topological
change in a magnetic field above the accretion disk because of the uniform,
constant Ohmic resistivity.
