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This study aims to investigate the ambiguous source and the underlyingphysical processes of the solar type III radio bursts that occurred on April 3,2019, through the utilization of multiwavelength observations from the LOFARradio telescope and the PSP space mission, as well as incorporating resultsfrom a PFSS and MHD models. The primary goal is to identify the spatial andtemporal characteristics of the radio sources, as well as the plasma conditionsalong their trajectory. Data preprocessing techniques are applied to combinehigh- and low-frequency observations from LOFAR and PSP between 2.6 kHz and 80MHz. We then extract information on the frequency drift and speed of theaccelerated electron beams from the dynamic spectra. Additionally, we use LOFARinterferometric observations to image the sources of the radio emission atmultiple frequencies and determine their locations and kinematics in thecorona. Lastly, we analyze the plasma parameters and magnetic field along thetrajectories of the radio sources using PFSS and MHD model results. We presentseveral notable findings related to type III radio bursts. Firstly, through ourautomated implementation, we were able to effectively identify and characterize9 type III radio bursts in the LOFAR-PSP combined dynamic spectrum and 16 typeIII bursts in the LOFAR dynamic spectrum. Secondly, our imaging observationsshow that the electrons responsible for these bursts originate from the samesource and within a short time frame of fewer than 30 minutes. Finally, ouranalysis provides informative insights into the physical conditions along thepath of the electron beams. For instance, we found that the plasma densityobtained from the MAS model is significantly lower than the expectedtheoretical density.

Coronal Diagnostics of Solar Type-III Radio Bursts Using LOFAR and PSP Observations