Titlebook: Cooling Flows in Clusters and Galaxies; A. C. Fabian Book 1988 Kluwer Academic Publishers 1988 cosmic ray.cosmology.observatory.quasar.rel

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Properties of Clusters of Galaxies,hich the cooling flow environment, which appears to be ubiquitous in the early-type galactic systems which form the hosts for strong radio sources, may affect the origin and structure of the radio emitting regions.

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卧虎藏龙

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Book 1988usters, and in elliptical galaxies, is so high that radiative cooling is a significant energy loss. The cooling time of the gas decreases rapidly towards the centre of the cluster or galaxy and is less than a Hubble time within the innermost few hundred kiloparsecs. This results in a cooling flow in

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Dynamics of Cosmic Rays in Cooling Flows,s interaction by means of steady models with spherical symmetry. It was found that the cosmic ray pressure may become comparable to the gas pressure in the halo region around a central galaxy with a cooling flow. Rayleigh Taylor instabilities might develop there and set the scale for inhomogeneities leading to filaments or star formation regions.

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