Peculiarities of Radio Pulsars with Long Periods

The analysis of parameters of radio pulsars with periods \(P > 5\) s has been carried out. It was found that there is no clear dependence of \(dP{\text{/}}dt\) on \(P\) on the \(\{ dP{\text{/}}dt,P\} \) diagram. The lack of dependence can be explained within the disk model. It is shown that the pulse width decreases with increasing period for the sample considered. It is the opposite of the dependence in the generally accepted pulsar model. It indicates that the distance from the surface of the neutron star to the radio emission generation region in the studied population depends on the period or that the magnetic field in the generation region has a non-dipolar structure. The possibility of explaining the longest intervals between successive pulses in pulsars J0901–4046 and J0250+5854 by the influence of drift waves at the periphery of the magnetosphere has been considered. Within the framework of the drift model, the calculated rotation periods in these pulsars turn out to be several times shorter than the observed intervals between successive pulses.