Drift-pair bursts are an unusual type of solar low-frequency radio emission, which appear in the dynamic spectra as two parallel drifting bright stripes separated in time. Recent imaging spectroscopy observations allowed for the quantitative characterization of the drifting pairs in terms of source size, position, and evolution. Here, the drift-pair parameters are qualitatively analyzed and compared with the newly-developed Monte Carlo ray-tracing technique simulating radio-wave propagation in the inhomogeneous anisotropic turbulent solar corona. The results suggest that the drift-pair bursts can be formed due to a combination of the refraction and scattering processes, with the trailing component being the result of turbulent reflection (turbulent radio echo). The formation of drift-pair bursts requires an anisotropic scattering with the level of plasma density fluctuations comparable to that in type III bursts, but with a stronger anisotropy at the inner turbulence scale. The anisotropic radio-wave scattering model can quantitatively reproduce the key properties of drift-pair bursts: the apparent source size and its increase with time at a given frequency, the parallel motion of the source centroid positions, and the delay between the burst components. The trailing component is found to be virtually co-spatial and following the main component. The simulations suggest that the drift-pair bursts are likely to be observed closer to the disk center and below 100 MHz due to the effects of free-free absorption and scattering. The exciter of drift-pairs is consistent with propagating packets of whistlers, allowing for a fascinating way to diagnose the plasma turbulence and the radio emission mechanism.

中文翻译：

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湍流日冕中的无线电回波和太阳漂移对无线电爆发的模拟

漂移对爆发是一种不寻常的太阳低频射电发射，它在动态光谱中表现为两个平行漂移的明亮条纹，在时间上分开。最近的成像光谱观察允许在源大小、位置和演化方面对漂移对进行定量表征。在这里，对漂移对参数进行了定性分析，并与新开发的蒙特卡罗射线追踪技术进行了比较，该技术模拟了非均匀各向异性湍流日冕中的无线电波传播。结果表明，由于折射和散射过程的组合，可以形成漂移对突发，尾随分量是湍流反射（湍流无线电回波）的结果。漂移对爆发的形成需要各向异性散射，其等离子体密度波动水平与 III 型爆发相当，但在内部湍流尺度上具有更强的各向异性。各向异性无线电波散射模型可以定量再现漂移对突发的关键特性：视源大小及其在给定频率下随时间的增加、源质心位置的平行运动以及突发分量之间的延迟。发现尾随分量实际上是共空间的并跟随主分量。模拟表明，由于自由吸收和散射的影响，漂移对爆发很可能在更靠近磁盘中心和低于 100 MHz 的地方观察到。漂移对的激励器与传播的哨声数据包一致，