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During solar flares a large amount of electrons with energies greater than 20keV is generated with a production rate of typically $10^{36}$ s$^{-1}$. A partof them is able to propagate along open magnetic field lines through the coronainto interplanetary space. During their travel they emit radio radiation whichis observed as type III radio bursts in the frequency range from 100 MHz downto 10 kHz by the WAVES radio spectrometer aboard the spacecraft WIND, forinstance. From the drift rates of these bursts in dynamic radio spectra theradial propagation velocity $V_r$ of the type III burst exciting electrons isderived by employing a newly developed density model of the heliosphere.Calculations show that the radio radiation is emitted by electrons withdifferent $V_r$ and therefore by different electrons of the initially producedelectron distribution.

Propagation of energetic electrons from the corona into interplanetary space and type III radio emission