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arXiv 2202.09602astro-ph.HE
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重复快速射电暴源附近磁化非均匀环境的时间散射、去极化和持续射电发射

Temporal Scattering, Depolarization, and Persistent Radio Emission from Magnetized Inhomogeneous Environments Near Repeating Fast Radio Burst Sources

Yuan-Pei Yang, Wenbin Lu, Yi Feng, Bing Zhang, Di Li

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11 pages, 1 figures, accepted for publication in ApJL
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摘要：

某些重复快速射电暴（FRB）源具有复杂的极化行为，包括频率相关的去极化、旋转测度（RM）的变化以及极化分量的振荡谱结构。最近，Feng等人（2022）报道，有源中继器表现出明显的频率依赖性去极化以及RM散射（$σ_{\rm RM}$）和时间散射时间（$τ_{\rm s}$）（$σ_{\rm RM}\proptoτ_{\rm s}^{1.0\pm0.2}$）之间的强相关性，这两者都可以通过磁化非均匀等离子体屏的多径传播来很好地描述。这一观察结果强烈表明，时间散射和RM散射起源于同一区域。此外，Feng等人（2022）的一个特别值得注意的发现是，具有紧凑持续射电源（PRS）的FRB往往具有极端的$σ_{\rm RM}$。在这项工作中，我们专注于时间散射，RM散射去极化，和PRS贡献的磁化等离子体环境接近一个重复FRB源之间的关系的一些理论预测。RM散射的行为意味着磁化等离子体环境与超新星遗迹或脉冲星风星云一致，并且预测的$σ_{\rm RM}$ - $τ_{\rm s}$关系在不同的天体物理情景下为$σ_{\rm RM}\proptoτ_{\rm s}^{(0.54-0.83)}$。我们进一步对不依赖于特定天体物理场景的PRS进行了一般性讨论。我们表明，特定的亮度的PRS应该有一个正相关的RM等离子体屏幕的贡献。这与FRB 121102和FRB 190520 B的观测结果一致。

英文摘要：

Some repeating fast radio burst (FRB) sources exhibit complex polarization behaviors, including frequency-dependent depolarization, variation of rotation measure (RM), and oscillating spectral structures of polarized components. Very recently, Feng et al. (2022) reported that active repeaters exhibit conspicuous frequency-dependent depolarization and a strong correlation between RM scatter ($σ_{\rm RM}$) and the temporal scattering time ($τ_{\rm s}$), $σ_{\rm RM}\proptoτ_{\rm s}^{1.0\pm0.2}$, both of which can be well described by multi-path propagation through a magnetized inhomogeneous plasma screen. This observation strongly suggests that the temporal scattering and RM scatter originate from the same region. Besides, a particular finding of note in Feng et al. (2022) is that the FRBs with compact persistent radio sources (PRS) tend to have extreme $σ_{\rm RM}$. In this work, we focus on some theoretical predictions on the relations among temporal scattering, depolarization by RM scatter, and PRS contributed by the magnetized plasma environment close to a repeating FRB source. The behaviors of the RM scatter imply that the magnetized plasma environment is consistent with a supernova remnant or a pulsar wind nebula, and the predicted $σ_{\rm RM}$-$τ_{\rm s}$ relation is $σ_{\rm RM}\proptoτ_{\rm s}^{(0.54-0.83)}$ for different astrophysical scenarios. We further make a general discussion on PRS that does not depend on specific astrophysical scenarios. We show that the specific luminosity of a PRS should have a positive correlation with the RM contributed by the plasma screen. This is consistent with the observations of FRB 121102 and FRB 190520B.

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