Abstract
A uniform statistical description of the sample of pulsars including the millisecond and binary pulsars is obtained by considering them to originate from the main-sequence population of both single and binary stars. Assuming that a substantial fraction of pulsars have a binary origin, the observed gap in the field strength and spin period distribution of pulsars is shown to arise from a corresponding gap in the mass distribution of the secondary star (after the first-stage mass transfer) in binary systems. Magnetic field decay time-scales ≃ 10 8 yr are shown to be consistent with the above analysis
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