AI 中文总结
该研究提出脉冲星与快速射电暴（FRBs）可能存在线性偏振度与偏振角时间导数反相关的共同特征，通过脉冲星样本发现相关证据，其识别或助力理解FRBs起源并约束中子星参数。
AI 中文摘要
脉冲星和快速射电暴（FRBs）的偏振角（PA）是诊断其辐射区域磁场的有效工具，对理解它们的辐射机制和起源至关重要。在旋转中子星偏振辐射的通用几何框架内，我们提出线性偏振度$\text{\textbackslash Pi}_\text{L}$与偏振角时间导数$d\text{PA}/dt$之间可能存在反相关，这是脉冲星和FRBs的共同特征。退极化源于辐射区域可观测部分内不同偏振方向辐射的非相干叠加，仅当偏振角摆动足够陡峭时才可探测到。我们利用射电脉冲星样本检验该猜想，在部分脉冲星中发现了预期反相关的可能证据。由于观测数据有限，该关系是否适用于FRBs仍不确定。识别这一特征不仅能为FRBs的旋转磁层起源提供见解，还能为产生这些神秘暴的中子星的自转周期和几何参数施加约束。
英文摘要
The polarization angle (PA) of pulsars and fast radio bursts (FRBs) provides a useful diagnostic of the magnetic fields in their emission regions and is therefore crucial for understanding their radiation and origins. Within a general geometric framework for polarized emission from a rotating neutron star, we suggest a possible anti-correlation between the degree of linear polarization $Π_\text{L}$ and $d\text{PA}/dt$, the time derivative of the PA, as a common feature of pulsars and FRBs. The depolarization arises from the incoherent superposition of radiation with different polarization directions within the observable part of the emission region, and is detectable only when the PA swing is steep enough. We test this conjecture using a sample of radio pulsars and find possible evidence for the expected anti-correlation in a subset of pulsars. Whether this relation holds in FRBs remains uncertain due to limited observational data. Identification of this feature would not only provide insights into the rotating magnetospheric origin of FRBs, but also place constraints on the spin periods and geometric parameters of the neutron stars that power these mysterious bursts.
Comments11 pages, 9 figures, accepted by MNRAS
