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We investigate the differences between an outflow in a highly-resistiveaccretion disk corona, and the results with smaller or vanishing resistivity.For the first time, we determine conditions at the base of a two-dimensionalradially self-similar outflow in the regime of very large resistivity. Weperformed simulations using the {\sc pluto} magnetohydrodynamics code, andfound three modes of solutions. The first mode, with small resistivity, issimilar to the ideal-MHD solutions. In the second mode, with largerresistivity, the geometry of the magnetic field changes, with a "bulge" abovethe super-fast critical surface. At even larger resistivities, the third modeof solutions sets in, in which the magnetic field is no longer collimated, butis pressed towards the disk. This third mode is also the final one: it does notchange with further increase of resistivity. These modes describe topologicalchange in a magnetic field above the accretion disk because of the uniform,constant Ohmic resistivity.

Large resistivity in numerical simulations of radially self-similar outflows