  BD+53 2790, an O9.5Vp star, is the optical counterpart to the HMXRB 4U
2206+54. This system was classified initially as a BeX, but observational
evidence soon stressed the need to revise this classification. The permanent
asymmetry in the H-alpha line profiles (in contrast with the cyclic variations
shown by Be stars), the variations in the profile of this line in time scales
of hours (while time scales from weeks to months are expected in Be stars), and
the lack of correlation between IR observables and H-alpha line parameters,
strongly suggest that, while BD+53 2790 contains a circunstellar disc, it is
not like the one present in Be stars. Furthermore, there is evidence of
overabundance of He in BD+53 2790. Together with the presence of an anomalous
wind, found through UV spectroscopy, the possibility to link this star with the
group of He rich stars is open. We will discuss the work done with IUE data
from BD+53 2790 and the unexpected finding of a slow and dense wind, very rare
for an O9.5V star.
