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