||Corona, the outermost layer of the Sun, is believed to permeate from a heliocentric distance of 1.01R⊙ to more than 1 AU. Being highly tenuous plasma medium, it harbors large scale structures, as
multi-frequency observations reveal. One of the most common signatures of any flicker on the Sun is known as solar type III radio bursts. These bursts are an important diagnostic tool to understand the
acceleration of non-thermal electron beams along the coronal magnetic field lines. Using the interferometric and beam formed capabilities of LOw Frequency ARray (LOFAR), we analyzed a group of type
III radio bursts observed between 80-20 MHz, on 30 March 2018. Taking advantage of the high spectral, temporal and spatial resolution of LOFAR, we were able to distinguish five different trajectories of
propagation of the electron beams in the type III group. Using full Stokes observations(frequency and time resolution of 12 kHz and 10 ms, respectively) by the simultaneous beam formed LOFAR
observations, we estimated the coronal magnetic field along these five electron beam trajectories. This was done by calculating the degree of circular polarization of the harmonic plasma emission from
the type III bursts. The results obtained here is in close agreement with the previously reported work in the same height ranges.