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Be stars are main sequence fast-rotating stars that display a circumstellar emission. This emission is regarded as originated from a disk, formed by episodic mass-loss from the star. I will present the current modeling efforts and recent achievements of the BeACoN group at the IAG/USP (Brazil), which aims at understanding the rich Be phenomenology and the physical processes driving It. Based on the VDD (Viscous Decretion Disk) model and radiative transfer simulations, I will report (i) the observational campaign of the Be star Achernar over a full active phase, that started in 2013 and ended in 2016; (ii) the measurement of the Be disks viscosity from a sample in the Magellanic clouds and (iii) some predicted and observed binarity effects in these systems. |
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