Comprehensive Analysis of a Type III Radio Storm Using Multi-Spacecraft Observations

Solar flares are often accompanied by intense radio emissions, particularly notable in the form of fast-drifting type III bursts. These bursts are generated by suprathermal electron beams that are accelerated at solar flare reconnection sites. These electron beams travel outward along open magnetic field lines, passing through the corona and interplanetary medium. Type III Radio Storms, characterized by nearly continuous type III radio burst activity, can persist for hours or days. This study reports on a significant type III storm observed between 2023-09-20 and 2023-09-27, observed simultaneously by STEREO-A and Parker Solar Probe. During this interval, the spacecraft were longitudinally separated by 5 to 45 degrees, providing a unique opportunity to examine both radial and longitudinal variations in type III storms. Additionally, the Solar Orbiter's position on the opposite side of the Sun, complemented by SDO data, enabled nearly 360-degree solar coverage in EUV during this event. This extensive coverage allowed for the correlation of individual radio bursts with EUV images, offering a comprehensive view of the full Sun. Our findings contribute to the understanding of solar flare dynamics and electron beam propagation in solar eruptions.