  We present magnetohydrodynamic simulations of a resistive accretion disk
continuously launching transmagnetosonic, collimated jets. We time-evolve the
full set of magnetohydrodynamic equations, but neglect radiative losses in the
energetics (radiatively inefficient). Our calculations demonstrate that a jet
is self-consistently produced by the interaction of an accretion disk with an
open, initially bent large-scale magnetic field. A constant fraction of heated
disk material is launched in the inner equipartition disk regions, leading to
the formation of a hot corona and a bright collimated, super-fastmagnetosonic
jet. We illustrate the complete dynamics of the ``hot'' near steady-state
outflow (where thermal pressure $\simeq$ magnetic pressure) by showing force
balance, energy budget and current circuits. The evolution to this near
stationary state is analyzed in terms of the temporal variation of energy
fluxes controlling the energetics of the accretion disk. We find that unlike
advection-dominated accretion flow, the energy released by accretion is mainly
sent into the jet rather than transformed into disk enthalpy. These magnetized,
radiatively inefficient accretion-ejection structures can account for
under-luminous thin disks supporting bright fast collimated jets as seen in
many systems displaying jets (for instance M87).
