发表机构
Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences（波兰科学院尼古拉·哥白尼天文学中心）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本文提出基于非相干叠加的二维偏振模型，仅用单一本征模式即可解释射电脉冲星中的正交偏振轨道、模式分离及S型摆动，表明RVM参数反映辐射区几何而非偶极磁场。
AI 中文摘要
射电脉冲星信号中观测到的两个正交偏振模式长期以来被归因于强磁化等离子体中波振荡的本征模式。然而，最近的研究表明，对于产生非相干叠加偏振信号的扩展辐射区域，这些模式很容易出现。本文提出了一个基于射电信号非相干叠加的二维偏振模型。该模型涉及单一本征模式（例如O模），但导致了两个正交偏振轨道的出现，并自然地产生了平均轮廓中偏振模式分离的三重形式（中心模式两侧被另一模式包围），以及先前从波束映射推断出的模式在纬度上的位移。在锥形辐射区域的情况下，模拟的偏振倾向于模仿旋转矢量模型（RVM）的一般偏振特性。然而，其原因是辐射区域的对称性——而非偶极磁场方位角的通常投影。因此，得出的RVM参数揭示了辐射区域的几何形状，而非偶极磁场的几何形状。这些结果有力地支持了非双折射模式效应在射电脉冲星轮廓中的重要作用。可能不需要两个本征模式来解释两个正交偏振轨道的观测现象。
英文摘要
Two orthogonal polarization modes observed in radio pulsar signals have long been attributed to proper modes of wave oscillation in strongly magnetized plasma. Yet it has been shown recently that they show up readily for extended emission regions that produce incoherently-superposed polarization signal. In this paper we present a two-dimensional polarization model based on incoherent superposition of radio signals. The model involves a single proper mode, say the O mode, but leads to the appearance of two orthogonal polarization tracks and naturally produces the triple form of polarization mode segregation in averaged profiles (central mode flanked on boths sides by another mode), as well as the displacement of modes in latitude, previously inferred from beam mapping. In the case of conal emission regions, the modelled polarization tends to mimic general polarization properties of the rotating vector model (RVM). However, the reason for this is the symmetry of the emission region - not the usual projection of dipolar magnetic azimuths. Thus the emerging RVM parameters reveal geometry of the emission region, not of the dipolar magnetic field. The results strongly support the vital role of nonbirefringent modal effects in radio pulsar profiles. Two proper modes may not be needed to explain observations of two orthogonal polarization tracks.
Comments6 pages, 5 figures, submitted to AandA on 9 Jul 2026
