  We present a model for the radio emission from radio-quiet quasar nuclei. We
show that a thermal origin for the high brightness temperature, flat spectrum
point sources (known as radio ``cores'') is possible provided the emitting
region is hot and optically-thin. We hence demonstrate that optically-thin
bremsstrahlung from a slow, dense disk wind can make a significant contribution
to the observed levels of radio core emission. This is a much more satisfactory
explanation, particularly for sources where there is no evidence of a jet, than
a sequence of self-absorbed synchrotron components which collectively conspire
to give a flat spectrum. Furthermore, such core phenomena are already observed
directly via milli-arcsecond radio imaging of the Galactic microquasar SS433
and the active galaxy NGC1068. We contend that radio-emitting disk winds must
be operating at some level in radio-loud quasars and radio galaxies as well
(although in these cases, observations of the radio cores are frequently
contaminated/dominated by synchrotron emission from jet knots). This
interpretation of radio core emission mandates mass accretion rates that are
substantially higher than Eddington. Moreover, acknowledgment of this mass-loss
mechanism as an AGN feedback process has important implications for the input
of energy and hot gas into the inter-galactic medium (IGM) since it is
considerably less directional than that from jets.
