TeV Emission from the Galactic Center Black Hole Plerion

The HESS collaboration recently reported highly significant detection of TeVgamma-rays coincident with Sgr A*. In the context of other Galactic Center (GC)observations, this points to the following scenario: In the extremeadvection-dominated accretion flow (ADAF) regime of the GC black hole (BH),synchrotron radio/sub-mm emission of 100 MeV electrons emanates from aninefficiently radiating turbulent magnetized corona within 20 Schwarzschildradii of the GCBH. These electrons are accelerated through second-order Fermiprocesses by MHD turbulence. Closer to the innermost stable orbit of the ADAF,instabilities and shocks within the flow inject power-law electrons throughfirst-order Fermi acceleration to make synchrotron X-ray flares observed withChandra, XMM, and INTEGRAL. A subrelativistic MHD wind subtending a 1sr conewith 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 windtermination shock, at > 10^{16.5} cm from the GCBH, and Compton-scatter theADAF and the far infra-red (FIR) dust radiation to TeV energies. Thesynchrotron radiation of these electrons forms the quiescent X-ray sourceresolved by Chandra. The radio counterpart of this TeV/X-ray plerion, formedwhen the injected electrons cool on timescales 10^4 yrs, could explain theorigin of nonthermal radio emission in the pc-scale bar of the radio nebula SgrA West.Comment: 6 pages, 2 figures; accepted for publication in ApJ Letters, minor revison