transient X-ray pulsar systems: EXO 2030+375 [@Wil02], A0535+26 [@Bil97], 2S 1845-024 [@Fin99], GRO J1744-28 [@Bil97], GRO J1750-27 [@Sco97], XTE J1543-568 [@InZ01], SAX J2103.5+4545 [@Bay02], 2S 1416-62 [@Ina04]. In the last source the correlation between spin-up rate and X-ray flux was found for both main outbursts and the following mini outbursts [@Ina04]. However, the correlation between torque and flux, which was observed in BATSE experiment for some Be X-ray pulsars [@Fin96a; @Fin96b], does not confirm the pulsar spin-up rate $\dot{\nu}$ dependence on accretion rate $\dot{M}$, such as $\dot{\nu} \sim \dot{M}^{6/7}$, which was predicted by accretion torque theory. It is still unclear if this disagreement can be explained by bolometric or beaming corrections [@Bil97]. The BATSE instrument does not measure bolometric flux, but only pulsed flux in definite bands, while the large changes in beaming fraction imply the changing pulse profiles. Thus, it seems clear that new data on transient pulsars dynamics implying the flux, pulse profile and rotation period measurements on the long-term database including different luminosity regimes are quite useful for further progress on these phenomenon understanding. Below we will discuss the results of the search and study of periodic processes in hard X-rays from some transient pulsars during the 