Speaker
Description
Coronal mass ejections (CMEs) are often accompanied by a variety of solar radio emissions, among which moving type IV bursts are particularly interesting. These complex radio bursts are thought to be produced by energetic electrons trapped within expanding CME magnetic structures. Previous studies indicate that both gyrosynchrotron and plasma emission processes may contribute. Investigations of moving type IV bursts can provide valuable insight into the physical properties of CME magnetic structures and the energetic particles they contain.
On 28 March 2025, an X1.1 flare was observed by GOES and was followed by a fast CME with a projected speed of approximately 1986 km s⁻¹. The eruption was associated with the interaction between a rising flux rope and a filament. During this event, a variety of radio emissions were detected by ORFEES and the Nançay Radioheliograph (NRH), including a particularly complex moving type IV burst. Using NRH imaging, we find that the radio emission originated from multiple locations within the interacting flux rope–filament system. The event was also observed by HXI/ASO-S and possibly by STIX aboard the Solar Orbiter. By combining radio, extreme-ultraviolet (EUV), and hard X-ray (HXR) observations, we investigate the origin of the different type IV radio sources and explore the emission mechanisms responsible for their generation.