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The observed emission lines of Be stars originate from a circumstellarKeplerian disk that are generally well explained by the Viscous Decretion Diskmodel. In an earlier work we performed the modeling of the full light curve ofthe bright Be star $\omega$ CMa (Ghoreyshi et al. 2018) with the 1-Dtime-dependent hydrodynamics code SINGLEBE and the Monte Carloradiative-transfer code HDUST.  We used the V -band light curve that probes the inner disk through four diskformation and dissipation cycles. This new study compares predictions of thesame set of model parameters with time-resolved photometry from the near UVthrough the mid-infrared, comprehensive series of optical spectra, and opticalbroad-band polarimetry, that overall represent a larger volume of the disk.Qualitatively, the models reproduce the trends in the observed data due to thegrowth and decay of the disk. However, quantitative differences exist, e.g., anoverprediction of the flux increasing with wavelength, too slow decreases inBalmer emission-line strength that are too slow during disk dissipation, andthe discrepancy between the range of polarimetric data and the model. We findthat a larger value of the viscosity parameter alone, or a truncated disk by acompanion star, reduces these discrepancies by increasing the dissipation ratein the outer regions of the disk.

A Multi-observing-technique Study of the Dynamical Evolution of the Viscous Disk around the Be Star $\omega$ CMa