Be star omega CMa V light curve & polarimetry

Among all the proposed models explaining the physics of such disks, the Viscous Decretion Disk (VDD) paradigm matches best with the observations. In this work, we challenge the VDD model by applying it to the variety of data of the Be star {omega} CMa observed by different techniques.

We find that the VDD model explains the data well, qualitatively. However, we see some quantitative discrepancies that in turn are clues for better understanding the underlying physics of the Be disks. We investigate the possibilities of existing an undetected binary companion, and a radially variable viscous parameter, {alpha} to explain the mismatch between the data and the model.