<p>Solar radio bursts of Type III are believed to result from a sequence of physical processes ultimately leading to electromagnetic wave emissions near the electron plasma frequency &#969;<sub>p</sub> and its harmonic 2&#969;<sub>p</sub>. The radiation bursts are due to energetic electron beams accelerated during solar &#64258;ares. When propagating in the solar corona and the interplanetary wind, these &#64258;uxes excite Langmuir and upper-hybrid wave turbulence, which can be further transformed into electromagnetic radiation near the frequencies &#969;<sub>p</sub> and 2&#969;<sub>p</sub>.</p><p>It is believed that, in a homogeneous plasma, Langmuir turbulence evolves due to three-wave interaction processes, such as the fusion of Langmuir waves L with sound waves S leading to the formation of electromagnetic waves T<sub>&#969;p</sub> at &#969;<sub>p</sub> or the decay of L-waves into S-waves and T<sub>&#969;</sub><sub>p</sub>-waves. On the other hand, the electromagnetic waves radiated at 2&#969;<sub>p</sub> should arise from the coalescence L + L&#8217; --> T<sub>2&#969;</sub><sub>p</sub> of Langmuir waves L generated by the beam with Langmuir waves L&#8217; coming from the electrostatic decay L --> L&#8217; +&#160; S.</p><p>Large-scale 2D3V Particle-In-Cell simulations have been performed with the fully kinetic code Smilei [Derouillat et al., 2018], using parameters typical of Type III solar radio busts. The excitation of upper-hybrid wave turbulence by energetic electron beams propagating in magnetized plasmas leads ultimately to electromagnetic emissions near the fundamental and the harmonic plasma frequencies.</p><p><em>Derouillat et al. , Comput. Phys. Commun., 222, 351, <strong>2017</strong>.</em></p>