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Black holes were hypothesized as far back as the 1770s, but were not theoretically formalized until 1916, nor observationally identified until the 1970s. Since then, they have been recognized as a ubiquitous and important component of galaxy evolution and the baryon cycle. At the heart of AGN/quasars, they generate powerful outflows, which are believed to be radiatively driven. The nature of these outflows depends on the luminosity generated by the black hole accretion disks and the radiative efficiency of the accretion process. The luminosity is characterized by the Eddington ratio, the ratio of the bolometric luminosity to the Eddington luminosity, which is the value at which radiation pressure propels infalling gas outward. Quasars are observed to have a Schechter function distribution of Eddington ratios. Based on arguments of force multipliers, the case for radiative line-driven winds is advanced. A simplified picture in which outflows can be predicted on a plot of Eddington ratio versus black hole mass is discussed, as well as a black hole evolution H-R type of diagram based on “downsizing.”
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