1 outbursts) with typical times about days often begin soon after periastron. The typical X-ray luminosity of type 1 outbursts in BeX systems is about $10^{36}$ erg/s [@Bla04]. Besides the series of periodically occurring outbursts, the so-called giant outbursts with higher luminosity (type 2 outbursts) were observed. The type 1 outbursts are associated with the direct wind accretion of the Be circumstellar disk, while the type 2 outbursts can be described by the disk-fed accretion after the bound material has collapsed into a standard but temporary accretion disc [@Ste86; @Rag98]. The outburst peaks occur at phase 0-0.5, depending on the wind characteristics and orbital eccentricity. The bright giant outbursts have high spin-up rates, longer duration, and often have peak at an orbital phase delayed relative to the mean normal outburst X-ray maximum (e.g. 4U0115+63 [@Whi89], 3A0535+26, [@Bil97]).

Extensive data on periodicity in hard X-rays from many transient pulsars were obtained during the BATSE experiment onboard the Compton orbital observatory (CGRO) [@Bil97]. As the result of BATSE CGRO experiment no association had been observed between giant and normal outbursts. It was found that many of the giant outbursts are in the middle, or followed by, series of normal outbursts. Sometimes type 