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Abstract <p>This paper presents ephemerides derived from observations of giant radio pulses emitted by pulsar B0531<InlineEquation ID="IEq3"> <EquationSource Format="TEX">\(+\)</EquationSource> <!--BPhysMGU2570165Kurdubov-m3--> </InlineEquation>21 (Crab Pulsar). Observations began in mid-2023 using the RT-13 telescopes of the Quasar VLBI network in the S, X, and Ka bands, facilitated by a VLBI registration system and enhanced custom software for data processing. We developed an improved algorithm for estimating the dispersion measure (DM) and refined our method for determining pulse arrival times (TOAs) at the reference epoch. The newly established monitoring service has generated weekly ephemerides spanning more than 1.5 years. Our TOA measurements differ from those of the Jodrell Bank Observatory by approximately 63 <InlineEquation ID="IEq4"> <EquationSource Format="TEX">\(\mu\)</EquationSource> <!--BPhysMGU2570165Kurdubov-m4--> </InlineEquation>s RMS, while the derived pulsar periods exhibit an RMS deviation of about 2.5 ps, highlighting the high precision of our technique.</p>

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Ephemeris of Pulsar B0531\(\boldsymbol{+}\)21 from Radio Giant Pulses Observations

  • 期刊论文

  • 发表日期：

    2025年12月1日

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  • S. L. Kurdubov,
  • D. A. Marshalov,
  • I. A. Bezrukov,
  • I. S. Gayazov,
  • A. A. Dyakov,
  • A. V. Ipatov,
  • D. V. Ivanov,
  • A. E. Melnikov,
  • A. G. Mikhaylov,
  • V. G. Olifirov,
  • I. A. Rakhimov,
  • R. M. Urunova

摘要

Abstract

This paper presents ephemerides derived from observations of giant radio pulses emitted by pulsar B0531 \(+\) 21 (Crab Pulsar). Observations began in mid-2023 using the RT-13 telescopes of the Quasar VLBI network in the S, X, and Ka bands, facilitated by a VLBI registration system and enhanced custom software for data processing. We developed an improved algorithm for estimating the dispersion measure (DM) and refined our method for determining pulse arrival times (TOAs) at the reference epoch. The newly established monitoring service has generated weekly ephemerides spanning more than 1.5 years. Our TOA measurements differ from those of the Jodrell Bank Observatory by approximately 63 \(\mu\) s RMS, while the derived pulsar periods exhibit an RMS deviation of about 2.5 ps, highlighting the high precision of our technique.