标题： 一种与机制无关的方法，在南北对称框架下建模脉冲星的伽马射线相图 显示英文标题

标题： A mechanism-independent methodology for modeling γ-ray phaseograms of pulsars in the framework of north-south symmetry

摘要： Fermi-LAT观测显示，蟹状星云、Geminga、蜻蜓和Vela脉冲星的每个GeV相位折叠光曲线（也称为相位图）都包含两个脉冲（P1和P2）以及它们之间的“桥”。 在Vela脉冲星的桥相位处明显有一个“凸起”，也可以被视为第三个脉冲（P3）。 不同的是，蟹状星云、Geminga和蜻蜓的桥相对更像“谷底”。 尽管存在这种明显的差异，但有趣的是，可以研究它们的桥发射是否仍然属于与Vela相同的总体图景。 假设南北对称性，我们预期第四组分（Bridge2/P4）也应存在。 然而，这种假设的Bridge2/P4在蟹状星云、Geminga、蜻蜓和Vela脉冲星的$\gamma$射线相位图中并未直观地被识别出来。 暗示未发现Bridge2/P4的原因也很引人入胜。 我们的典型玩具模型不依赖于辐射区域或辐射机制的假设。 相反，它假设了南北对称的几何结构，并且每半球有一个圆形对称的波束，同时考虑了多普勒效应（最具创新性的元素）、时间延迟和能量相关的波束形状。 报告了我们拟合结果与风模型的初步兼容性。 值得注意的是，对于蟹状星云脉冲星，我们发现我们的模型预测与IXPE在X射线偏振方面的结果之间存在初步的定性相关性。 发现Geminga脉冲星较软的$\gamma$射线脉动覆盖其整个相位。 在系统评估的推动下，我们概述了我们玩具模型的一些潜在改进。 显示英文摘要

摘要： Fermi-LAT observations revealed that each GeV phase-folded light-curve (aka. phaseogram) of the Crab, Geminga, Dragonfly and Vela pulsars consists of two pulses (P1 & P2) and a "Bridge" between them. There is clearly a "bump" at the Bridge phase of Vela's pulse profiles, that could also be regarded as the third pulse (P3). Differently, the Crab's, Geminga's & Dragonfly's Bridges relatively resemble a "valley floor". Despite such an apparent difference, it is interesting to investigate whether their Bridge emissions are still within the same general picture as Vela's. Assuming the north-south symmetry, we would expect the fourth component (Bridge2/P4) to exist as well. However, such a hypothetical Bridge2/P4 is not intuitively identified on $\gamma$-ray phaseograms of the Crab, Geminga, Dragonfly and Vela pulsars. It is also intriguing to hint at the rationale for the non-discovery of Bridge2/P4. Our prototypical toy model is free of assumptions on emission regions or radiation mechanisms. Instead, it assumes a north-south symmetric geometry and one circularly symmetric beam per hemisphere, while taking into account Doppler shifts (the most innovative element), time delays and energy-dependent beam shapes. Tentative compatibility of our fitting results with wind models is reported. Notably, for the Crab pulsar, we found a preliminary qualitative correlation between our model predictions and the IXPE results on X-ray polarisation. The softer $\gamma$-ray pulsation of the Geminga pulsar is found to span over its full phase. Prompted by systematic evaluations, we outline some potential improvements for our toy model.