  Using a geometry consisting of a hot central Comptonizing plasma surrounded
by a thin accretion disk, we model the optical through hard X-ray spectral
energy distributions of the type 1 Seyfert galaxies NGC 3516 and NGC 7469. As
in the model proposed by Poutanen, Krolik, & Ryde for the X-ray binary Cygnus
X-1 and later applied to Seyfert galaxies by Zdziarski, Lubi\'nski, & Smith,
feedback between the radiation reprocessed by the disk and the thermal
Comptonization emission from the hot central plasma plays a pivotal role in
determining the X-ray spectrum, and as we show, the optical and ultraviolet
spectra as well. Seemingly uncorrelated optical/UV and X-ray light curves,
similar to those which have been observed from these objects can be explained
by variations in the size, shape, and temperature of the Comptonizing plasma.
Furthermore, by positing a disk mass accretion rate which satisfies a condition
for global energy balance between the thermal Comptonization luminosity and the
power available from accretion, one can predict the spectral properties of the
hard X-ray continuum above $\sim 50$ keV in type 1 Seyfert galaxies.
Forthcoming measurements of the hard X-ray continuum by more sensitive hard
X-ray and soft $\gamma$-ray telescopes, in conjunction with simultaneous
optical, UV, and soft X-ray monitoring, will allow the mass accretion rates to
be directly constrained for these sources in the context of this model.
