  Using a simple description of feedback from black hole (BH) growth, we
develop an analytic model for the fueling of Seyferts (low-luminosity AGN) and
their relation to their host galaxies, Eddington ratio distributions, and
cosmological evolution. We derive a solution for evolution of accretion rates
in a feedback-driven blast wave, applicable to large-scale outflows from bright
quasars in galaxy mergers, low-luminosity AGN, and BHs in supernova remnants.
Under the assumption that cold gas stochastically accretes onto a central SMBH
at a rate set by the dynamics of that gas, our solution determines the Seyfert
light curve evolution. We use this to predict the Seyfert luminosity function
(LF), duty cycles, lifetimes, and distribution of host morphologies, Eddington
ratios, and obscuration as a function of AGN luminosity and mass, and find
agreement with observations at z=0. We consider the breakdown of contributions
from this and stellar wind accretion and merger-driven activity. We make
specific predictions for the weak evolution of the Seyfert LF with redshift (LF
of non-merger driven activity), and for changes in both the slope and scatter
of the M_BH-sigma relation at low-M_BH. Quiescent fueling dominates over a wide
luminosity range (-14 > M_B > -22) at z=0, where most BH growth occurs around
M_BH~10^7 M_sun, in S0 and Sa/b galaxies. However, quasar activity from
gas-rich mergers evolves more rapidly with redshift, and by z=1 quiescent
fueling is important only at luminosities an order of magnitude or more below
the LF break. Although non-merger driven fueling is important for BH growth and
the M_BH-sigma relation at low M_BH, it does not significantly contribute to
the total BH mass density or cosmological backgrounds.
