长周期射电脉冲星的特殊性

IF 1.1 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS
I. F. Malov
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引用次数: 0

摘要

对周期为(P > 5\ )秒的射电脉冲星的参数进行了分析。结果发现,在\(\{ dP\text{/}dt,P\} \)图上,\(dP{text{/}dt\)对\(P\)没有明显的依赖关系。这种缺乏依赖性的现象可以用圆盘模型来解释。研究表明,在所考虑的样本中,脉冲宽度随着周期的增加而减小。这与普遍接受的脉冲星模型的依赖性正好相反。这表明在所研究的群体中,从中子星表面到射电发射生成区的距离取决于周期,或者生成区的磁场具有非两极结构。考虑了通过磁层外围漂移波的影响来解释脉冲星 J0901-4046 和 J0250+5854 中连续脉冲之间最长间隔的可能性。在漂移模型的框架内,计算出的这些脉冲星的旋转周期比观测到的连续脉冲之间的间隔短几倍。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
Peculiarities of Radio Pulsars with Long Periods

The analysis of parameters of radio pulsars with periods \(P > 5\) s has been carried out. It was found that there is no clear dependence of \(dP{\text{/}}dt\) on \(P\) on the \(\{ dP{\text{/}}dt,P\} \) diagram. The lack of dependence can be explained within the disk model. It is shown that the pulse width decreases with increasing period for the sample considered. It is the opposite of the dependence in the generally accepted pulsar model. It indicates that the distance from the surface of the neutron star to the radio emission generation region in the studied population depends on the period or that the magnetic field in the generation region has a non-dipolar structure. The possibility of explaining the longest intervals between successive pulses in pulsars J0901–4046 and J0250+5854 by the influence of drift waves at the periphery of the magnetosphere has been considered. Within the framework of the drift model, the calculated rotation periods in these pulsars turn out to be several times shorter than the observed intervals between successive pulses.

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来源期刊
Astronomy Reports
Astronomy Reports 地学天文-天文与天体物理
CiteScore
1.40
自引率
20.00%
发文量
57
审稿时长
6-12 weeks
期刊介绍: Astronomy Reports is an international peer reviewed journal that publishes original papers on astronomical topics, including theoretical and observational astrophysics, physics of the Sun, planetary astrophysics, radio astronomy, stellar astronomy, celestial mechanics, and astronomy methods and instrumentation.
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