  We present comprehensive models for the Herbig Ae stars MWC275 and AB Aur
that aim to explain their spectral energy distribution (from UV to millimeter)
and long baseline interferometry (from near-infrared to millimeter)
simultaneously. Data from the literature, combined with new mid-infrared (MIR)
interferometry from the Keck Segment Tilting Experiment, are modeled using an
axisymmetric Monte Carlo radiative transfer code. Models in which most of the
near-infrared (NIR) emission arises from a dust rim fail to fit the NIR
spectral energy distribution (SED) and sub-milli-arcsecond NIR CHARA
interferometry. Following recent work, we include an additional gas emission
component with similar size scale to the dust rim, inside the sublimation
radius, to fit the NIR SED and long-baseline NIR interferometry on MWC275 and
AB Aur. In the absence of shielding of star light by gas, we show that the
gas-dust transition region in these YSOs will have to contain highly refractory
dust, sublimating at ~1850K. Despite having nearly identical structure in the
thermal NIR, the outer disks of MWC275 and AB Aur differ substantially. In
contrast to the AB Aur disk, MWC275 lacks small grains in the disk atmosphere
capable of producing significant 10-20micron emission beyond ~7AU, forcing the
outer regions into the "shadow" of the inner disk
