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The spatial distribution and birth-rate of pulsars

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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−c 1 L −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.

The obtained laws of the radial andZ-distribution of pulsars and galactic supernova remnants and also the radial distribution of types I and II supernovae in the models Sb and Sc support the hypothesis of their origin from the objects of the flat subsystem of Population I. Since there are some arguments in favour of a possible connection between supernovae I and the objects of the intermediate component of the Galaxy, one cannot exclude the possibility of supernovae explosions at the end of the evolution of stars with masses of 1.5–2M ⊙. It is also shown that pulsars and supernovae are evidently objects that are connected genetically, and, within the limits of statistical error, they have a similar birth-rate.

The empirical law of the evolution of a pulsar's luminosity as a function of its true age has been obtained, according to whichL=c 2 t −β, wherec 2=(3.69±3.4)×1035, β=1.32±0.11.

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Authors and Affiliations

  1. Shemakha Astrophysical Observatory, The Scientific Centre ‘Kaspy’, Shemakha, Azerbaijan SSR, U.S.S.R.

    O. H. Guseinov & F. K. Kasumov

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  1. O. H. Guseinov
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  2. F. K. Kasumov
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Guseinov, O.H., Kasumov, F.K. The spatial distribution and birth-rate of pulsars. Astrophys Space Sci 59, 285–300 (1978). https://doi.org/10.1007/BF01023920

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