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Calculations of angles between magnetic moments and rotation axes have been carried out for radio pulsars located at different distances from the "death line." We have shown that these angles decrease from 36° to 10° when pulsars move to the "death line". Such values correspond to kinematic ages from 1 to 10 millions of years. We also argue that radio luminosities of pulsars decrease for these ages. This means that radio pulsars fade out when their age increases. [ABSTRACT FROM AUTHOR]

Distribution of angles β between magnetic moments and rotation axes for radio pulsars with periods in the interval 0.1 s < P < 2 s has been obtained. This distribution is rather wide with a mean value of 23°. For the bulk of pulsars, the inclination of axes is characterized by moderate values of angles β. About 60 per cent of pulsars considered have angles in the interval from 20° to 45°. The useful correlation between kinematic t kin and characteristic ages τ has been detected. The relationship between t kin and τ can be used to make a conversion of catalogue values of τ to more real pulsar ages t kin. It will be important in further pulsar investigations. It is shown that inclination angles for pulsars with 0.1 s < P < 2 s decrease with their ages. This decrease is the best described by the power law. Values of angles β have been calculated for pulsars, which are at the moment in SNRs. These angles are not changed markedly during 105 yr. Their decrease begins much later. [ABSTRACT FROM AUTHOR]

Angles between the rotation axis and the magnetic moment are calculated in two groups of radio pulsars with different periods ( s and s). Two methods have been used. The first method is based on the observed pulse widths and provides the minimum values of angle . The distributions of these angles differ significantly for these groups of objects. The second method uses polarization data to calculate more accurate values . There is a trend for bimodality in the distribution of values for pulsars with s. The closeness of the mean values ( for long-period pulsars and for sources with shorter periods) does not allow us to explain the previously discovered difference in the behavior of these two groups in the diagram by a decrease in the role of magnetic dipole radiation due to a decrease in . Our analysis showed that the observed difference can be explained by the different dependence of the pulsar wind and magnetic dipole braking on the period of the pulsar. The deceleration of pulsars with s is mainly caused by the pulsar wind. [ABSTRACT FROM AUTHOR]