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The mechanism that can be responsible for the bimodal luminosity distributionof super-Eddington X-ray pulsars in binary systems is pointed out. Thetransition from the high to low state of these objects is explained byaccretion flow spherization due to the radiation pressure at certain (high)accretion rates. The transition between the states can be associated with agradual change in the accretion rate. The complex behavior of the recentlydiscovered ultraluminous X-ray pulsars M 82 X-2, NGC 5907 ULX-1, and NGC 7793P13 is explained by the proposed mechanism. The proposed model also naturallyexplains the measured spinup of the neutron star in these pulsars, which isslower than the expected one by several times.

The origin of the bimodal luminosity distribution of ultraluminous X-ray pulsars