Speaker
Description
Coronal Mass Ejections (CMEs) are the primary drivers of space weather phenomena.
Once a CME reaches Earth the severity of the geomagnetic response is dependent on CME properties such as speed, dynamic pressure, and the specific magnetic configuration of the CME. CMEs can be modelled with a bright front, dark cavity and core. This core is associated with a flux rope in CME models.
We present a case study of the formation and subsequent expansion of a flux rope prior to its eruption. This flux rope was observed in extreme-ultraviolet (EUV) on the 28th February 2024.
In addition to being observable in EUV images, the formation and evolution of the rope appeared to be associated with radio emissions that indicate that the energisation of electrons was taking place. The emission mechanism for the radio has been determined to be fundamental plasma emission and this emission mechanism allows for electron density to be calculated; we found that the electrons generating the radio emission range in density from 0.3e9-2.4e9 cm^-3.
It was also found that the EUV expansion pattern matched the expansion pattern the radio emission, supporting the interpretation what the EUV emission and the radio emission are both originating in the same structure.
This study shows that the value of using complementary EUV and radio data to probe the timescales over which a pre-eruptive structure forms, and how the radio emissions can be used to probe important flux properties such as plasma density.
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