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A general relativistic model for the formation and acceleration of lowmass-loaded jets from systems containing accreting black holes is presented.The model is based on previous numerical results and theoretical studies in theNewtonian regime, but modified to include the effects of space-time curvaturein the vicinity of the event horizon of a spinning black hole. It is arguedthat the boundary layer between the Keplerian accretion disk and the eventhorizon is best suited for the formation and acceleration of theaccretion-powered jets in active galactic nuclei and micro-quasars.  The model is based on matching the solutions of three different regions: i- aweakly magnetized Keplerian accretion disk in the outer part, where thetransport of angular momentum is mediated through the magentorotationalinstability, ii- a strongly magnetized, advection-dominated and turbulent-freeboundary layer (BL) between the outer cold accretion disk and the eventhorizon, where the plasma rotates sub-Keplerian and iii- a transition zone (TZ)between the BL and the overlying corona, where the electrons and protons arethermally uncoupled, highly dissipative and rotate super-Keplerian.  Our model predicts the known correlation between the Lorentz-factor and thespin parameter of the BH. It also shows that the effective surface of the BL,through which the baryons flow into the TZ, shrinks with increasing the spinparameter, implying therefore that low mass-loaded jets most likely originatefrom around Kerr black holes.  When applying our model to the jet in the elliptical galaxy M87, we find aspin parameter in the range 0.99 - 0.998, a transition radius of about 30gravitational radii and a fraction of 0.05 - 0.1 of the mass accretion rategoes into the TZ, where the plasma speeds up its outward-oriented motion toreach a Lorentz factor of 2.5 - 5.0 at the transition radius.

Launching proton-dominated jets from accreting Kerr black holes: the case of M87