Abstract
A hot, two-temperature accretion disk can be a strong ..gamma..-ray and relativistic particle source. This occurs when the accretion rate is high enough: M/M> or approx. =3 x 10/sup -9/..cap alpha.. yr/sup -1/ for a canonical Kerr black hole: due to the high ion temperature in the inner disk. We present detailed photon and particle spectra for specific disk models. The predicted ..gamma..-ray flux is as high as 10% of the bolometric luminosity in sub-Eddington models. Most of the ..gamma..-radiation is continuous, due to the ..pi../sup 0/ decay, emitted around 100 MeV but degraded to a few MeV in optically thick models. Spectral lines, due to position annihilation or to excited nuclei, provide only a small amount of the primary ..gamma..-ray luminosity. The energy flux in approx.35 MeV pairs is comparable to the ..gamma..-ray luminosity; Penrose effects provide a smaller number of approx.1 GeV pairs.
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