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Monitoring of pulse period variations in accreting binary pulsars is animportant tool to study the interaction between the magnetosphere of theneutron star and the accretion disk. While the X-ray flux of the brightestX-ray pulsars have been successfully monitored over many years (e.g. withRXTE/ASM, CGRO/BATSE, Swift/BAT), the possibility to monitor their pulse timingproperties continuously has so far been very limited. In our work we useSwift/BAT observations to study one of the most enigmatic X-ray pulsars,Hercules X-1. For the first time, a quasi-continuous monitoring of the pulseperiod and the pulse period derivative of Her X-1, is achieved over a long time(> 4 yrs). We argue that together with the long-term decrease of the orbitalperiod in Her X-1 the measured pulse period behaviour requires the presence ofmass ejection from the inner parts of the accretion disk along the openmagnetic field lines. The mass ejection episodes probably take place duringstrong spin-down episodes which are associated with the low X-ray luminosity.

Monitoring of pulse period in Her X-1 with Swift/BAT: evidence of mass ejection