On the possibility of determining the coronal magnetic field from solar type III radio burst observations

A simple method of estimating the coronal magnetic field is suggested. It i s based on the observational fact that the duration of the highly polarized part in type III bursts can be different, varying from a small fraction of the burst length to its total duration. We suggest that this difference is determined by the relation between the size of the region where only the o rdinary wave can propagate and the size of the region where the burst is ge nerated at a fixed frequency. The magnetic field is estimated at several te ns of gauss in regions emitting highly polarized type III bursts at frequen cies over 200 MHz. Density and magnetic field scales are estimated.