TeV Emission from the Black-Hole Plerion at the Galactic Center

Details TeV Emission from the Black-Hole Plerion at the Galactic Center TeV Emission from the Black-Hole Plerion at the Galactic Center

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aas...205.3201d&link_type=abstract

American Astronomical Society Meeting 205, #32.01; Bulletin of the American Astronomical Society, Vol. 36, p.1398

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Scientific paper

The HESS collaboration recently reported the detection of TeV γ -ray emission 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 R S (Schwarzschild radii) of the GCBH. Electrons are accelerated in this ADAF 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 an ˜ 1 sr cone with power ≳ 1037 erg s-1 is driven by the ADAF from the vicinity of the GCBH. Electrons accelerated at the wind termination shock at ≳ 1016.5 cm from the GCBH Compton-scatter ADAF and FIR dust emission to TeV energies. The synchrotron radiation of these electrons produces the quiescent X-ray plerionic source resolved by Chandra. The radio counterpart of the TeV/X-ray plerion, formed when the injected electrons cool on timescales of ≳ 104 yrs, could explain the origin of the nonthermal radio emission in the two-sided bar of the radio nebula Sgr A West.

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