Polarization Measurements of Solar Radio Transients Associated with Coronal Mass Ejections

The Solar Corona is a teneous medium of magnetized plasma with an inherent distribution of number density of electrons which decreases as one moves radially outward from the sun. Transient radio emissions from the corona are often-observed over a wide-range of radio frequencies from few Ghz down to a few kHz which correspond to coronal regions closer to the Sun into the interplanetary medium respectively. It is now understood that such activity is primarily governed by the magnetic field that shapes the plasma and hence study of polarization of the radio emission will help us understand the structure of the coronal plasma. In this presentation I will focus on the polarization observations of different radio transients at meter wavelengths associated with eruptive phenomena called Coronal Mass Ejections (CME) and the estimation of magnetic field at and near the CME.