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Drift-pair bursts are an unusual type of solar low-frequency radio emission,which appear in the dynamic spectra as two parallel drifting bright stripesseparated in time. Recent imaging spectroscopy observations allowed for thequantitative characterization of the drifting pairs in terms of source size,position, and evolution. Here, the drift-pair parameters are qualitativelyanalyzed and compared with the newly-developed Monte Carlo ray-tracingtechnique simulating radio-wave propagation in the inhomogeneous anisotropicturbulent solar corona. The results suggest that the drift-pair bursts can beformed due to a combination of the refraction and scattering processes, withthe trailing component being the result of turbulent reflection (turbulentradio echo). The formation of drift-pair bursts requires an anisotropicscattering with the level of plasma density fluctuations comparable to that intype III bursts, but with a stronger anisotropy at the inner turbulence scale.The anisotropic radio-wave scattering model can quantitatively reproduce thekey properties of drift-pair bursts: the apparent source size and its increasewith time at a given frequency, the parallel motion of the source centroidpositions, and the delay between the burst components. The trailing componentis found to be virtually co-spatial and following the main component. Thesimulations suggest that the drift-pair bursts are likely to be observed closerto the disk center and below 100 MHz due to the effects of free-free absorptionand scattering. The exciter of drift-pairs is consistent with propagatingpackets of whistlers, allowing for a fascinating way to diagnose the plasmaturbulence and the radio emission mechanism.

Radio Echo in the Turbulent Corona and Simulations of Solar Drift-Pair Radio Bursts