  The spectral shape of IR emission from Herbig Ae/Be stars has been invoked as
evidence for accretion disks around high-mass protostars. Instead, we present
here models based on spherical envelopes with $r^{-1.5}$ dust density profile
that successfully explain the observed spectral shapes. The spectral energy
distributions (SEDs) of eight primary candidates for protostellar disks are
fitted in detail for all wavelengths available, from visual to far IR. The only
envelope property adjusted in individual sources is the overall visual optical
depth, and it ranges from 0.3 to 3. In each case, our models properly reproduce
the data for both IR excess, visual extinction and reddening. The success of
our models shows that accretion disks cannot make a significant contribution to
the radiation observed in these pre-main sequence stars.
