  We perform GR-MHD simulations of outflow launching from thin accretion disks.
As in the non-relativistic case, resistivity is essential for the mass loading
of the disk wind. We implemented resistivity in the ideal GR-MHD code HARM3D,
extending previous works (Qian et al. 2017, 2018) for larger physical grids,
higher spatial resolution, and longer simulation time. We consider an initially
thin, resistive disk orbiting the black hole, threaded by a large-scale
magnetic flux. As the system evolves, outflows are launched from the black hole
magnetosphere and the disk surface. We mainly focus on disk outflows,
investigating their MHD structure and energy output in comparison with the
Poynting-dominated black hole jet. The disk wind encloses two components -- a
fast component dominated by the toroidal magnetic field and a slower component
dominated by the poloidal field. The disk wind transitions from sub to
super-Alfv\'enic speed, reaching velocities $\simeq 0.1c$. We provide parameter
studies varying spin parameter and resistivity level, and measure the
respective mass and energy fluxes. A higher spin strengthens the
$B_{\phi}$-dominated disk wind along the inner jet. We disentangle a critical
resistivity level that leads to a maximum matter and energy output for both,
resulting from the interplay between re-connection and diffusion, which in
combination govern the magnetic flux and the mass loading. For counter-rotating
black holes the outflow structure shows a magnetic field reversal. We estimate
the opacity of the inner-most accretion stream and the outflow structure around
it. This stream may be critically opaque for a lensed signal, while the axial
jet funnel remains optically thin.
