On X-ray emission of radio pulsars
Abstract
The analysis of distributions of some parameters of radio pulsars emitting X-ray radiation was carried out. The majority of such pulsars has short spin periods with the average value < P > = 133 msec. The distribution of period derivatives reveals a bimodality, dividing millisecond (< log dPdt> = -19.69) and normal (< log dPdt> = -13.29) pulsars. Magnetic fields at the surface of the neutron star are characterized by the bimodal distribution as well. The mean values of <log Bs> are 8.48 and 12.41 for millisecond pulsars and normal ones, respectively. The distribution of magnetic fields near the light cylinder, it does not show the noticeable bimodality. The median value of log Blc = 4.43 is almost three orders higher comparing with this quantity (<log Blc> = 1.75) for radio pulsars without registered X-ray emission. Losses of rotational energy (<log dEdt> = 35.24) are also three orders higher than corresponding values for normal pulsars. There is the strong correlation between X-ray luminosities and losses of rotational energies. The dependence of the X-ray luminosity on the magnetic field at the light cylinder has been detected. It shows that the generation of the non-thermal X-ray emission takes place at the periphery of the magnetosphere and is caused by the synchrotron mechanism. We detected the positive correlations between luminosities in radio, X-ray and gamma -ray ranges. Such correlations give the possibility to carry out a purposeful search for pulsars in one of these ranges if they radiate in other one.
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