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Abstract <p>We have performed timing of several of known second-period pulsars with poorly known coordinates and parameters of their own rotation. Data from the archive of round-the-clock monitoring observations with the third (uncontrolled) radiation pattern of the Large Phased Array telescope (LPA) of the Pushchino Radio Astronomy Observatory of the Lebedev Physical Institute (PRAO LPI) at a frequency of 111 MHz were used, which have an unsatisfactory time link of local quartz time standards to the reference scale (UTC). To compensate for the errors caused by this, we applied an algorithm previously developed by us, which uses an intermediate reference scale of pulsar time to calculate corrections at the Time of arrival (TOA) of pulsar pulses measured by local clocks and to switch to UTC. Based on the results of the analysis of a 10-year series of observations, we were able to significantly refine the rotational and astrometric parameters of 12 pulsars. The proper rotation frequencies ν and their first derivatives <InlineEquation ID="IEq1"> <EquationSource Format="TEX">\(\dot {\nu }\)</EquationSource> <!--AstEng2570230Andrianov-m1--> </InlineEquation> were determined with an accuracy of 10<sup>–10</sup> Hz and 10<sup>–19</sup> s<sup>–2</sup>, respectively, which is 5–6 orders of magnitude higher than the accuracy given in the catalog. The coordinates are determined with an accuracy better than a few tens of arcseconds.</p>

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The Pushchino Multibeams Pulsar Search. VII. The Results of the Timing of 12 Slow Pulsars

  • 期刊论文

  • 发表日期：

    2025年11月1日

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  • S. A. Andrianov,
  • V. A. Potapov,
  • S. A. Tyul’bashev

摘要

Abstract

We have performed timing of several of known second-period pulsars with poorly known coordinates and parameters of their own rotation. Data from the archive of round-the-clock monitoring observations with the third (uncontrolled) radiation pattern of the Large Phased Array telescope (LPA) of the Pushchino Radio Astronomy Observatory of the Lebedev Physical Institute (PRAO LPI) at a frequency of 111 MHz were used, which have an unsatisfactory time link of local quartz time standards to the reference scale (UTC). To compensate for the errors caused by this, we applied an algorithm previously developed by us, which uses an intermediate reference scale of pulsar time to calculate corrections at the Time of arrival (TOA) of pulsar pulses measured by local clocks and to switch to UTC. Based on the results of the analysis of a 10-year series of observations, we were able to significantly refine the rotational and astrometric parameters of 12 pulsars. The proper rotation frequencies ν and their first derivatives \(\dot {\nu }\) were determined with an accuracy of 10–10 Hz and 10–19 s–2, respectively, which is 5–6 orders of magnitude higher than the accuracy given in the catalog. The coordinates are determined with an accuracy better than a few tens of arcseconds.