脉冲星轮廓的拓扑结构（ToPP）。I. 图论方法及EPN分类
Topology of Pulsar Profiles (ToPP). I. Graph theory method and classification of the EPN
AI总结：
本文提出首个基于图拓扑的无监督方法ToPP，按轮廓形状相似性对脉冲星分类，应用于EPN数据库揭示连续演化轨迹，并可系统归入Rankin经验方案，为平方公里阵列时代的大规模脉冲星普查提供关键工具。
摘要：
射电脉冲星的一些最重要信息来源于其平均脉冲轮廓。许多早期脉冲星研究必然仅基于少数几个这样的轮廓。在这些研究中，离散的轮廓分量通过人工解释与单颗恒星的辐射机制模型联系起来。对于整个脉冲星群体而言，轮廓形态必然反映射电辐射区的几何结构和整体演化。然而，问题在于这一群体正变得过于庞大，难以对所有源逐一进行深入研究。此外，将大量脉冲星的轮廓联系起来也迅速变得繁琐。在本文中，我们提出了ToPP，这是首个利用图拓扑结构、根据轮廓形状相似性对脉冲星进行无监督分类的方法。我们将ToPP应用于公开可用的欧洲脉冲星网络（European Pulsar Network）轮廓数据库，首次提供了代表90颗独立脉冲星的多频轮廓的有组织可视化概览。我们发现离散的演化轨迹，从所有频率上的简单单分量轮廓，到具有频率演化的更复杂轮廓的多样混合。轮廓演化是连续的，一直延伸到毫秒脉冲星，并不落入截然分明的类别。我们将这些轮廓解释为脉冲星核/锥辐射类型、自旋减慢能量学以及视线相对于磁轴撞击角的混合结果。我们展示了ToPP如何能够系统地将源分类到Rankin经验轮廓方案中。ToPP构成了关键的无监督方法之一，对于探索即将到来的脉冲星普查数据（例如平方公里阵列（Square Kilometer Array）所预期的数据）将是必不可少的。
英文摘要：
Some of the most important information on a radio pulsar is derived from its average pulse profile. Many early pulsar studies were necessarily based on only few such profiles. There, discrete profile components were linked to emission mechanism models for individual stars through human interpretation. For the population as a whole, profiles morphology must reflect the geometry and overall evolution of the radio emitting regions. The problem, however, is that this population is becoming too large for intensive studies of all sources individually. Moreover, connecting profiles from a large collection of pulsars rapidly becomes cumbersome. In this article, we present ToPP, the first-ever unsupervised method to sort pulsars by profile-shape similarity, using graph topology. We apply ToPP to the publicly available European Pulsar Network profile database, providing the first organised visual overview of multi-frequency profiles representing 90 individual pulsars. We find discrete evolutionary tracks, varying from simple, single component profiles at all frequencies, towards diverse mixtures of more complex profiles with frequency evolution. The profile evolution is continuous, extending out to millisecond pulsars, and does not fall in sharp classes. We interpret the profiles as a mixture of pulsar core/cone emission type, spin-down energetics, and the line-of-sight impact angle towards the magnetic axis. We show how ToPP can systematically classify sources into the Rankin empirical profile scheme. ToPP forms one of the key unsupervised methods that will be essential to explore upcoming pulsar census data such as expected by the Square Kilometer Array.
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