  A self-similar solution for the 3D axi-symmetric radiative MHD equations,
which revisits the formation and acceleration of accretion-powered jets in AGNs
and microquasars, is presented. The model relies primarily on electromagnetic
extraction of rotational energy from the disk plasma and forming a
geometrically thin super-Keplerian layer between the disk and the overlying
corona. The outflowing plasma in this layer is dissipative, two-temperature,
virial-hot, advective and electron-proton dominated. The innermost part of the
disk in this model is turbulent-free, sub-Keplerian rotating and
advective-dominated. This part ceases to radiate as a standard disk, and most
of the accretion energy is converted into magnetic and kinetic energies that go
into powering the jet. The corresponding luminosities of these
turbulent-truncated disks are discussed.
