  The HESS collaboration recently reported highly significant detection of TeV
gamma-rays coincident with Sgr A*. In the context of other Galactic Center (GC)
observations, this points to the following scenario: In the extreme
advection-dominated accretion flow (ADAF) regime of the GC black hole (BH),
synchrotron radio/sub-mm emission of 100 MeV electrons emanates from an
inefficiently radiating turbulent magnetized corona within 20 Schwarzschild
radii of the GCBH. These electrons are accelerated through second-order Fermi
processes by MHD turbulence. Closer to the innermost stable orbit of the ADAF,
instabilities and shocks within the flow inject power-law electrons through
first-order Fermi acceleration to make synchrotron X-ray flares observed with
Chandra, XMM, and INTEGRAL. A subrelativistic MHD wind subtending a 1sr cone
with power > 10^{37} erg/s is driven by the ADAF from the vicinity of the GCBH.
As in pulsar powered plerions, electrons are accelerated at the wind
termination shock, at > 10^{16.5} cm from the GCBH, and Compton-scatter the
ADAF and the far infra-red (FIR) dust radiation to TeV energies. The
synchrotron radiation of these electrons forms the quiescent X-ray source
resolved by Chandra. The radio counterpart of this TeV/X-ray plerion, formed
when the injected electrons cool on timescales 10^4 yrs, could explain the
origin of nonthermal radio emission in the pc-scale bar of the radio nebula Sgr
A West.
