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At the site of their origin, solar meterwave radio bursts contain pristineinformation about the local coronal magnetic field and plasma parameters. Onits way through the turbulent corona, this radiation gets substantiallymodified due to the propagation effects. Effectively disentangling theintrinsic variations in emission from propagation effects has remained achallenge. We demonstrate a way to achieve this, using snapshot spectroscopicimaging study of weak type III bursts using data from the Murchison WidefieldArray (MWA). We use this study to present the first observational evidence forsecond-scale Quasi-Periodic Oscillations (QPOs) in burst source sizes andorientation with simultaneous QPOs in intensity. The observed oscillations insource sizes are so fast and so large that, they would require two orders ofmagnitude larger Alfven speed than the typical 0.5 Mm/s, if interpreted withina MHD framework. These observations imply the presence of a quasi-periodicregulation mechanism operating at the particle injection site, modulating thegeometry of energetic electron beams that generate type III bursts. Inaddition, we introduce a method to characterize plasma turbulence in midcoronal ranges, using such frequent weak bursts. We also detect evidence for asystematic drift in the location of the burst sources superposed on the randomjitter induced by scattering. We interpret this as the motion of the open fluxtube within which the energetic electron beams travel.

Evidence for Super-Alfvenic oscillations in sources of Solar type III radio bursts