Abstract
The distribution of pulsars in the wide range of observed luminosities has been obtained. It is shown that the function of luminosity (FL) within 3×1026≤L≤2×1030 erg s−1 conforms to the power law dN/dL−c1L−γ, where γ=1.76±0.06. ForL≤3×1026 erg s−1, FL changes its inclination and may be approximated as\({{dN} \mathord{\left/ {\vphantom {{dN} {dL \sim }}} \right. \kern-\nulldelimiterspace} {dL \sim }}L^{ - \gamma _1 } \), where γ1 = 0.7±0.2. On the basis of statistical selection, including all pulsars withL>3×1028 erg s−1, the distribution of pulsars has been investigated as a function of the distance to the centreR and galactic planeZ.
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