  I present a theoretical and numerical (Monte Carlo) N-particle analysis of
Penrose scattering processes in the ergosphere of a supermassive Kerr black
hole. These GR model calculations reveal that the observed high energies and
luminosities of quasars and other active galactic nuclei, the collimated jets
about the polar axis, and the asymmetrical jets (which can be enhanced by
relativistic Doppler beaming effects) all are inherent properties of rotating
black holes. The Penrose scattered escaping relativistic particles exhibit
tightly wound coil-like cone distributions (highly collimated vortical jet
distributions) about the polar axis, with helical polar angles of escape
varying from 0.5-30 deg for the highest energy particles. The gravitomagnetic
field exerts a force acting on the momentum vectors of the incident and
scattered particles, causing asymmetrical particle jet emission above and below
the equatorial plane. When the accretion disk is assumed to be an ADAF,
energies as high as 54 GeV can be attained by these Penrose processes alone;
and when relativistic beaming is included, energies in the TeV range can be
achieved, agreeing with observations of some BL Lac objects. This
energy-momentum extraction model can be applied to any size black hole. When
this model is applied specifically to quasars 3C 279, 3C 273, Seyfert 1 galaxy
MCG--60-30-15, and galactic black hole source Cygnus X-1, their observed high
energy luminosity spectra in general can be explained. The consistency of these
Penrose model calculations with observations suggests that the external
magnetic field of the accretion disk plays a negligible role in the extraction
of energy-momentum from a rotating black hole, close to the event horizon,
where gravitational forces appear to be dominant.
