The core component width in normal pulsars, with periods ($P$) $>$ 0.1seconds, measured at the half-power point at 1 GHz has a lower boundary line(LBL) which closely follows the $P^{-0.5}$ scaling relation. This result is offundamental importance for understanding the emission process and requiresextended studies over a wider frequency range. In this paper we have carriedout a detailed study of the profile component widths of 123 normal pulsarsobserved in the Meterwavelength Single-pulse Polarimetric Emission Survey at333 and 618 MHz. The components in the pulse profile were separated into coreand conal classes. We found that at both frequencies the core as well as theconal component widths versus period had a LBL which followed the $P^{-0.5}$relation with a similar lower boundary. The radio emission in normal pulsarshave been observationally shown to arise from a narrow range of heights arounda few hundred kilometers above the stellar surface. In the past the $P^{-0.5}$relation has been considered as evidence for emission arising from last opendipolar magnetic field lines. We show that the $P^{-0.5}$ dependence only holdsif the trailing and leading half-power points of the component are associatedwith the last open field line. In such a scenario we do not find any physicalmotivation which can explain the $P^{-0.5}$ dependence for both core and conalcomponents as evidence for dipolar geometry in normal pulsars. We believe theperiod dependence is a result of an yet unexplained physical phenomenon.
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机译：在1 GHz的半功率点处测量的正常脉冲星的核心分量宽度（周期（$ P $）$> $ 0.1秒）具有下边界线（LBL），该边界线紧随$ P ^ {-0.5} $比例关系。该结果对于理解排放过程具有根本的重要性，并且需要在更宽的频率范围内进行扩展研究。在本文中，我们对在333 MHz和618 MHz的米波长单脉冲极化发射测量中观测到的123个正常脉冲星的剖面分量宽度进行了详细研究。脉冲轮廓中的成分分为核心和圆锥类。我们发现，在两个频率下，磁芯以及圆锥形组件的宽度随周期的变化都有一个LBL，该LBL遵循$ P ^ {-0.5} $关系，并具有相似的下边界。观察到正常脉冲星的无线电发射是由恒星表面上方几百公里左右的狭窄高度范围引起的。在过去，$ P ^ {-0.5} $关系被认为是由最后的开放偶极磁场线引起的发射的证据。我们证明，只有当组件的尾随和前半功率点与最后一条空场线相关联时，$ P ^ {-0.5} $依赖性才成立。在这种情况下，我们找不到任何物理动力可以解释对核心和圆锥形分量的$ P ^ {-0.5} $依赖性，以此作为正常脉冲星偶极几何的证据。我们认为，周期依赖性是尚未解释的物理现象的结果。
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