Abstract

We have analyzed the results of our observations of the millisecond pulsar B0329+54 (J0332+5434), which exhibits quasi-periodic variations in the barycentric times of arrival (TOAs) of pulses on long time scales. We have tested the hypothesis about the existence of a planet with a mass close to the mass of the terrestrial planets and an orbital period of 27.8 yr around this pulsar that was proposed previously to explain the variations in its TOAs. We show that this hypothesis is not confirmed when considering the series of TOA residuals over the entire available time interval of observations 1968–2022 and that the TOA variations for this pulsar apparently have a different physical cause.

中文翻译：

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检验关于围绕脉冲星 B0329+54 (J0332+5434) 运行的行星是否存在的假设

摘要

我们分析了毫秒脉冲星 B0329+54（J0332+5434）的观测结果，该脉冲星在长时间尺度上表现出脉冲重心到达时间（TOA）的准周期变化。我们已经测试了关于是否存在一颗质量接近类地行星质量且围绕该脉冲星轨道周期为 27.8 年的行星的假设，该假设是之前提出的，用于解释其 TOA 的变化。我们表明，当考虑 1968-2022 年整个可用观测时间间隔内的 TOA 残差系列时，这一假设并未得到证实，并且该脉冲星的 TOA 变化显然有不同的物理原因。