论文标题
闪烁可以解释SGR 1935+2154的明亮无线电爆发的光谱结构
Scintillation can explain the spectral structure of the bright radio burst from SGR 1935+2154
论文作者
论文摘要
通过加拿大氢强度映射实验FRB协作（Chime/FRB）和瞬态天文学无线电发射2（Steare2）的调查，发现了与银河系相关的快速无线电爆发（FRB），这为完善的机会提供了完善的机会来完善FRB发射模型。铃声/FRB发现的爆发显示了两个具有不同光谱的组件。我们探索星际闪烁，作为这种光谱结构变化的起源。建模与磁铁相关的超新星残留物中的弱散射屏幕，我们发现需要$> 9.5 \的发射区域的超光静脉表观横向速度，以解释光谱变化。另外，这两个组件可能源自$> 8.3 \ times10^4 \，$ km的独立排放区域。这些情况可能是在“遥远”模型中引起的，其中发射起源于磁层的磁层（例如，通过超偏射主义辐射冲击而建立的同步体模式机制），但不是在磁层内的“近距离”模型中。如果对磁体的进一步观察结果确认闪烁是观察到的光谱结构变化的来源，则该散射模型会限制发射区域的位置。
The discovery of a fast radio burst (FRB) associated with a magnetar in the Milky Way by the Canadian Hydrogen Intensity Mapping Experiment FRB collaboration (CHIME/FRB) and the Survey for Transient Astronomical Radio Emission 2 (STARE2) has provided an unprecedented opportunity to refine FRB emission models. The burst discovered by CHIME/FRB shows two components with different spectra. We explore interstellar scintillation as the origin for this variation in spectral structure. Modeling a weak scattering screen in the supernova remnant associated with the magnetar, we find that a superluminal apparent transverse velocity of the emission region of $>9.5\,c$ is needed to explain the spectral variation. Alternatively, the two components could have originated from independent emission regions spaced by $>8.3\times10^4\,$km. These scenarios may arise in "far-away" models where the emission originates from well beyond the magnetosphere of the magnetar (for example through a synchrotron-maser mechanism set up by an ultra-relativistic radiative shock), but not in "close-in" models of emission from within the magnetosphere. If further radio observations of the magnetar confirm scintillation as the source for the observed variation in spectral structure, this scattering model thus constrains the location of the emission region.
