热性星际气体的仿射回收模型

presented for a hydrostatic isothermal hot gas distribution in a gravitational well of a giant elliptical galaxy immersed in a massive dark halo. The self-consistently determined gravitational potential of the system provides the optical surface brightness distribution of the galaxy, matching the de Vaucouleurs R^1/4-law, if the sound speed in the gas, stellar velocity dispersion, and velocity dispersion of dark matter are related so that optical and X-ray brightness profiles match each other. The thermal equilibrium of the gas is described in the framework of a one-zone model, which incorporates radiative cooling, stellar mass loss, supernova heating, and mass sink due to local condensational instability. The sequence of saddle-node and saddle-connection bifurcations provides a first-order phase transition, which separates the stable hot phase in the cooling medium for a reasonably high efficiency of condensation and precludes catastrophic cooling of the gas. The bifurcations occur naturally, due to the shape of the radiative cooling function, and this holds for a wide range of gas metallicities. The one-zone model implies a scaling relation for the equilibrium stellar and gas densities, which allows a hydrostatic, thermally stable distribution for the hot isothermal coronal gas. The resulting model for gas recycling reproduces the basic optical and X-ray properties of relatively isolated giant elliptical galaxies with hot haloes. Implications for cD galaxies in X-ray dominant clusters and groups are briefly discussed in the general context of galaxy formation and evolution.