Abstract
QSOs in galactic nuclei can be modeled using a massive black hole, a nuclear starburst stellar cluster, an accretion disc and an interstellar medium. The symbiosis of the starburst and black hole self‐consistently explains the production of the bolometric luminosity and the lines. The ISM contains both inflow, which fuels the black hole and accretion disc, and a wind. This system leads naturally to a two component broad emission line region (BELR). High ionization lines (the HIL) are emitted by wind gas which has cooled after shocking against supernovae in the starburst cluster (Perry & Dyson7). the HIL velocity reflects a combination of the wind speed and the Keplerian velocity of the supernovae which is hypersonic with respect to the second speed (cs≊400 km s−1) in the Compton heated wind. Low ionization lines (LIL) are emitted from the accretion disc surface: the disc rotational velocity produces their line widths (Collin‐Souffrin, Dyson, McDowell & Perry1).
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