Abstract
We present the results of an analysis of the rotation regularities of pulsars from the current observations and retrospective data on the timing of pulsars at Pushchino Observatory, obtained since 1978 to 2017. Parametric approximation of numerical series of Times of Arrival (ToAs) the convergence polynomial series defined the combinations of numerical values, unique for each pulsar, identical in any reference system for coinciding epochs, irrespective of duration of observations that corresponds to the coherence of periodic radiation of pulsars. The braking index at all observed pulsars is n =−(0.9 ± 0.2) that corresponds monotony of slowing down of rotation (>0). The polynomial power series of the intervals calculated in observed parameters of rotation represent an analytical time scale on which variations of observed intervals, uncorrelated with rotation, are counted, as at pulsars B1919+21 and B0809+74, or the unpredictable variations of intervals defining the movement of a pulsar in the supernova remnants, as at PSR B0531+21 or at PSR B1822-09 which spontaneous movement also doesn’t exclude its belonging to the supernova remnants.
Highlights
The most significant results in studying the physical properties of pulsars are connected with periodic regularity of a radio emission of the rotating magnetized neutron star
The polynomial power series of the intervals calculated in observed parameters of rotation represent an analytical time scale on which variations of observed intervals, uncorrelated with rotation, are counted, as at pulsars B1919+21 and B0809+74, or the unpredictable variations of intervals defining the movement of a pulsar in the supernova remnants, as at PSR B0531+21 or at PSR B1822-09 which spontaneous movement doesn’t exclude its belonging to the supernova remnants
The consistency of the rotation parameters does not depend on the choice of the initial epoch; in any case, the initial period value corresponding to the chosen sample of the initial epoch, taking into account the derivatives of the period (6), is determined by approximating the intervals PTobs
Summary
The most significant results in studying the physical properties of pulsars are connected with periodic regularity of a radio emission of the rotating magnetized neutron star. In addition to a local time standard and the Solar-System ephemerides pulsar timing requires knowledge of the pulsar’s pulse period and spin-down, its astrometric position and proper motion, its distance, parallax (where detectable) dispersion measure in the interstellar medium and (on the binary system) any orbital parameters All of these parameters are included in a timing model, which can be used to predict the phase of the pulsar’s periodic signal at any point in time. Unpredictable, abnormally high variations of residuals are interpreted as sudden failures of the period of rotation (glitches) In this consideration, especially significant is a reliable extraction of physical characteristics of rotation of pulsars, including the second derivative, on directly observed data of, in view of basic restrictions of reliability of statistical estimates on residuals. The comprehensive fitting should be enough only those parameters whose exact values can be derived directly from observation
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