On the peculiarities in the rotational frequency evolution of isolated neutron stars

Conference paper


The measurements of pulsar frequency second derivatives have shown that they are 102−106 times larger than expected for standard pulsar spin-down law, and are even negative for about half of pulsars. We explain these paradoxical results on the basis of the statistical analysis of the rotational parameters ν, \(\dot{\nu}\) and \(\ddot{\nu}\) of the subset of 295 pulsars taken mostly from the ATNF database. We have found a strong correlation between \(\ddot{\nu}\) and \(\dot{\nu}\) for both \(\ddot{\nu}>0\) and \(\ddot{\nu}<0\) , as well as between ν and \(\dot{\nu}\) . We interpret these dependencies as evolutionary ones due to \(\dot{\nu}\) being nearly proportional to the pulsars’ age. The derived statistical relations as well as “anomalous” values of \(\ddot{\nu}\) are well described by assuming the long-time variations of the spin-down rate. The pulsar frequency evolution, therefore, consists of secular change of ν ev(t), \(\dot{\nu}_{\mathrm{ev}}(t)\) and \(\ddot{\nu}_{\mathrm{ev}}(t)\) according to the power law with n≈5, the irregularities, observed within a timespan as a timing noise, and the variations on the timescale larger than that—several decades.


Methods: data analysis Methods: statistical Pulsars: general 


97.60.Jd 97.60.Gb 97.10.Kc 98.62.Ve 


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Copyright information

© Springer 2007

Authors and Affiliations

  1. 1.SAI MSUMoscowRussia

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