Constraining the Physical Parameters of Coronal Mass Ejections at Large Coronal Heights using Low Radio Frequency Gyrosynchrotron Emission

Coronal Mass Ejection (CMEs) are large scale explosive eruptions of magnetised plasma from the Sun into the Heliosphere. Measuring the physical parameters of CMEs is crucial for understanding their physics and for assessing their geo-effectiveness. Radio observations offer the most direct means for estimating these plasma parameters when gyrosynchrotron (GS) emission is detected from the CME. However, since the first detection by Bastian et al. in 2001, only a handful of studies have successfully detected GS emission from CME plasma.This is usually attributed to the challenges involved in obtaining the high contrast imaging required for observing this faint emission in the vicinity of active solar emissions.