Abstract
The authors report new Hα spectral observations on the V/R Be and shell star HD 184279. The observations cover part of a cycle that is probably reaching the steady-state of an activity period that started around 1971. The physical mechanism that can explain the observations, suggests that electron scattering is responsible for the very large emission wings observed. A small and very variable shell is present around the star, probably in form of an elongated disk that develops and grows during part of the cycle. A picture with an eccentric disk with semi-axis of 2 and 15 stellar radius seems to be adequate for this star. This envelope has a total mass of 10-9 stellar masses.
