AI 中文总结
本研究提出结合脉冲星闪烁与偏振数据相位检索的方法，探测到PSR B0834+06处AU尺度的磁场反转，为约束宇宙射线传输及脉冲星计时阵列噪声模型提供新途径。
AI 中文摘要
星际介质中的AU尺度结构已在天体物理学多个领域受到关注，从星际介质微观物理学到脉冲星计时阵列以及宇宙射线（CR）传播均涉及此类结构。磁场反转处形成的电流片尤其受关注，因为它们可将主导的GeV宇宙射线群体偏转大角度。脉冲星闪烁是探测等离子体密度的出色探针，能分辨这些结构，但无法分辨其磁场构型。常规法拉第旋转量（RM）在AU尺度上的灵敏度仅勉强达标，还会受电离层系统误差影响。我们提出一种方法，通过对偏振数据应用相位检索，分离双折射诱导的偏振——这是磁场反转的特征。脉冲星闪烁还能分辨约1 AU分离的射线路径，实现差分RM测量，在保留AU尺度磁场信号的同时抑制电离层共模。我们利用PSR B0834+06的存档观测数据演示该方法，相位检索将1毫秒散射特征分解为多普勒-延迟空间中的两个分支。根据波纹电流片解释，这些分支对应采样AU尺度电流片两侧的射线路径。我们在10 MHz带宽内测得分支间RM差为(-9.3±3.2)×10⁻³ rad m⁻²，显著性达2.9σ，该信号与平行磁场平均差|Δ⟨B∥⟩|≃4.4±2.1 μG的磁场反转一致，足以维持长寿命电流片。仅用6个独立子带，我们将此作为概念验证而非确定性探测。若该方法可扩展，其全面实施将能约束宇宙射线传输，并为脉冲星计时阵列中传播诱导噪声的模型提供信息。
英文摘要
AU-scale structures in the interstellar medium have become relevant across several areas of astrophysics, from ISM microphysics to pulsar timing arrays and cosmic-ray (CR) propagation. Current sheets formed at magnetic-field reversals have drawn particular attention because they can deflect the dominant GeV CR population through large angles. Pulsar scintillation, an outstanding probe of plasma density, resolves these structures---but not their magnetic configuration. Conventional Faraday rotation measures (RM) are only marginally sensitive at AU scales and are further compromised by ionospheric systematics. We propose a method that isolates birefringence-induced polarization---the signature of magnetic reversal---by applying phase retrieval to polarized data. Pulsar scintillation further resolves ray paths separated by $\sim 1\,\rm{AU}$, enabling differential RM measurements that suppress the ionospheric common mode while preserving the AU-scale magnetic signal. We demonstrate the method on an archival observation of PSR B0834+06. Phase retrieval resolves the 1-ms scattering feature into two branches in Doppler-delay space. Under the corrugated current-sheet interpretation, these branches correspond to ray paths sampling opposite sides of an AU-scale current sheet. We measure a branch-to-branch RM difference of $(-9.3\pm3.2)\times 10^{-3}\text{ rad m}^{-2}$ at 2.9$σ$ across a 10-MHz band. The signal is consistent with a field reversal of $|Δ\langle B_\parallel \rangle| \simeq4.4\pm2.1\,μ\rm G$, sufficient to sustain a long-lived sheet. With only six independent subbands, we present this as a proof of concept rather than a definitive detection. If it proves scalable, its full implementation could constrain cosmic-ray transport and inform models of propagation-induced noise in pulsar timing arrays.
