  We have observed 14 Herbig Ae/Be sources with the long-baseline near-IR
Palomar Testbed Interferometer, All except two sources are resolved at 2.2 um,
with angular sizes generally <5 mas. We determine the size scales and
orientations of the 2.2 um emission using various models: uniform disks,
Gaussians, uniform rings, flat accretion disks with inner holes, and flared
disks with puffed-up inner rims; 7 objects display significantly inclined
morphologies, generally compatible with the outer disk geometries inferred from
millimeter interferometric observations, implying that HAEBE disks are not
significantly warped. Using the derived inner disk sizes and inclinations, we
compute the spectral energy distributions for two simple physical disk models,
and compare these with observed SEDs compiled from the literature and new
near-IR photometry. While geometrically flat accretion disk models are
consistent with the data for the earliest spectral types in our sample (MWC
297, V1685 Cyg, and MWC 1080), the later-type sources are explained better
through models incorporating puffed-up inner disk walls; this may indicate
different accretion mechanisms for early and late-type Herbig Ae/Be stars.
