Subject headings: cooling flows–galaxies: Seyfert–X-rays: galaxies

摘要: We numerically simulate the structure of the X-ray heated winds believed to form the “mirrors” which reflect light from obscured Seyfert galaxy nuclei into our line of sight. The order of magnitude estimates made by Krolik & Begelman are largely confirmed. For a central luminosity of 10 “ergs sT" and an inner toroidal radius of 1 pc, the characteristic temperature in the wind is-1 x 10 K, and the flow speed is several hundred km s". When L/L, 5 008, most of the mass evaporated off the torus's inner edge is captured; when L/L, J08, a substantial wind is driven off, with a maximum mass-loss rate that scales roughly in proportion to the injection pressure. Even when L/L,> 0.08, if mass is injected more rapidly than the maximum rate, it is captured. Subsonic, or at most weakly supersonic, injection is necessary in order for most of the mass injected to be expelled.We present predictions of: the reflected fraction, the polarization of …