EDP Sciences
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Volume 428, Number 3, December IV 2004
Page(s) 943 - 951
Section Stellar structure and evolution
DOI http://dx.doi.org/10.1051/0004-6361:20034399

A&A 428, 943-951 (2004)
DOI: 10.1051/0004-6361:20034399

On the pulse-width statistics in radio pulsars

M. Kolonko1, 2, J. Gil3 and K. Maciesiak3

1  Institute of Nuclear Physics, Radzikowskiego 152, 31-342 Kraków, Poland
2  Institute of Astronomy, Jagiellonian University, Orla 171, 30-244 Kraków, Poland
3  Institute of Astronomy, University of Zielona Góra, Lubuska 2, 65-265 Zielona Góra, Poland
    e-mail: jag@astro.ia.uz.zgora.pl

(Received 25 September 2003 / Accepted 28 July 2004)

We perform Monte Carlo simulations of pulsar periods, pulse-widths and magnetic inclination angles. Using the available observational data sets we study possible parent distribution functions by means of the Kolmogorov-Smirnov significance tests. We also use an additional condition that the numbers of generated interpulses, whether from both magnetic poles or from a single pole, are at the observed levels. We derived a model distribution function of magnetic inclination angles which has a local maximum near $\alpha=25^\circ$ and another weaker one near $\alpha=90^\circ$. The gamma function is a plausible distribution function describing pulsar periods. The average beaming fraction describing the fraction of observable radio pulsars is about 0.12.

Key words: stars: pulsars: general -- stars: neutron -- stars: rotation

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