A study has been made of the behaviour in time of the positions, flux density and polarization for the radio emissions at frequencies of 237 and 408 MI-Iz (from Trieste observations), taking into account also the published results at 169 and 160-200 MHz (from Nangay and Utrecht) connected with the solar flare which occurred on JanuarY 14, 1971, at llh21 m UT.
The flare and the subsequent emissions may have been excited by a fall of coronal matter along the lines of force of the magnetic field in the relevant active region, exciting radio emissions of two different types: a type II-like emission and a type III group apparently located at different positions.
This discrepancy can be easily explained if we assume that the type III group was due to second harmonic emission in backward direction, strongly refracted by the coronal plasma.
The observed spike emission was due to a source high in the corona, excited by the type II-like perturbation which originated in the flare region, and this fact clearly points out the relationship between all the observed peculiar emissions from type IV sources, as has already been stated by this author.