  The observed emission lines of Be stars originate from a circumstellar
Keplerian disk that are generally well explained by the Viscous Decretion Disk
model. In an earlier work we performed the modeling of the full light curve of
the bright Be star $\omega$ CMa (Ghoreyshi et al. 2018) with the 1-D
time-dependent hydrodynamics code SINGLEBE and the Monte Carlo
radiative-transfer code HDUST.
  We used the V -band light curve that probes the inner disk through four disk
formation and dissipation cycles. This new study compares predictions of the
same set of model parameters with time-resolved photometry from the near UV
through the mid-infrared, comprehensive series of optical spectra, and optical
broad-band polarimetry, that overall represent a larger volume of the disk.
Qualitatively, the models reproduce the trends in the observed data due to the
growth and decay of the disk. However, quantitative differences exist, e.g., an
overprediction of the flux increasing with wavelength, too slow decreases in
Balmer emission-line strength that are too slow during disk dissipation, and
the discrepancy between the range of polarimetric data and the model. We find
that a larger value of the viscosity parameter alone, or a truncated disk by a
companion star, reduces these discrepancies by increasing the dissipation rate
in the outer regions of the disk.
