  We present a brief description of a model for the broad emission line region
(BELR) in quasars, which is supported by analysis of CIV and other emission
lines in the spectra of high-z SDSS quasars. Specifically we consider a
two-component BELR with a disk and wind where the relative strength of each
component is a function of luminosity. The implications of such a model for our
understanding of quasar outflows and estimates of their black hole masses and
accretion rates are discussed.
