Rapid rotation is a fundamental characteristic of classical Be stars and a crucial property
allowing for the formation of their circumstellar disks. Past evolution in a mass and angular …

Context. Empirical evidence for the involvement of nonradial pulsations (NRPs) in the mass
loss from Be stars ranges from (i) a singular case (μ Cen) of repetitive mass ejections …

We use the three-dimensional Monte Carlo radiative transfer code hdust to model Be stars
where the disc is tilted from the equatorial plane of the star. We compute 128 models across …

TESS photometry is analyzed for 430 classical Be stars observed in the first year of the
mission. The often complex and diverse variability of each object in this sample is classified …

γ Cas stars are a∼ 1% minority among classical Be stars with hard (≥ 5− 10 keV), but only
moderately strong continuous thermal X-ray flux, and mostly very early-B spectral type. The …

We use a three-dimensional smoothed particle hydrodynamics code to simulate growth and
dissipation of Be star discs in systems where the binary orbit is misaligned with respect to …

With hydrodynamic simulations, we show that a coplanar disc around one component of a
binary can be unstable to global tilting when the disc orbits in a retrograde direction relative …

The bright and understudied classical Be star HD 6226 has exhibited multiple outbursts in
the last several years during which the star grew a viscous decretion disc. We analyse 659 …

We use a time-dependent hydrodynamic code and a non-LTE Monte Carlo code to model
disk dissipation for the Be star 66 Ophiuchi. We compiled 63 years of observations from …

Classical B emission (Be) stars are fast rotating, near-main-sequence B-type stars. The
rotation and the presence of circumstellar discs profoundly modify the observables of active …