  We present a model which relates the Broad Emission Line Regions of AGN to
the accretion mechanism. Based on the Keplerian assumption for the high
velocity clouds of the gas responsible for the production of the Broad Emission
Lines, we identify that gas with an outflowing disk/coronal wind forms a
stabilized Shakura-Sunyaev accretion disk. We show that in the framework of
this picture the observed range of H-beta FWHM from Broad Line to Narrow Line
type 1 AGN, is well reproduced as a function of the accretion rate.
