  We present an improved calculation of the vertical structure and ultraviolet
spectrum of a dissipative accretion disk in an AGN. We calculate model spectra
in which the viscous stress is proportional to the total pressure, the gas
pressure only and the geometric mean of the radiation and gas pressures (cf.
Laor & Netzer 1989: LN89). As a result of a more complete treatment of
absorptive opacity, we find greater overall spectral curvature than did LN89,
as well as larger amplitudes in both the Lyman and HeII photoionization edges.
The local black body approximation is not a good description of the near UV
spectrum. With relativistic corrections (appropriate to non-rotating black
holes) included, we find that the near UV spectrum hardens with increasing
m-dot / m_8 (m-dot is the accretion rate in Eddington units, m_8 the black hole
mass in units of 10^8 M_Sun). The near UV spectrum is consistent with
observations if m-dot/ m_8 \sim 10^{-3}, but disks this cold would have large,
and unobserved, absorption features at the Lyman edge. The edge amplitude is
reduced when m-dot/m_8 is larger, but then the near-UV slope is too hard to
match observations. We conclude that models in which conventional disks orbit
non-rotating black holes do not adequately explain UV continuum production in
AGN.
