Spin evolution of Be/X-ray pulsars observed in Small Magellanic Cloud is discussed. If these neutron stars accrete material from a keplerian disk or quasi-spherical flow, their magnetic field should be either above the quantum critical level or below 0.01TG. I discuss a possibility to model these pulsars within the magnetic-levitation accretion scenario. The magnetic field of the neutron stars in this case turns out to be close to its conventional value.

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