Electromagnetic wave radiation in turbulent magnetized and inhomogeneous plasmas : theory and simulations

In a weakly magnetized and randomly inhomogeneous solar wind plasma where upper-hybrid wave turbulence is generated, electromagnetic radiation at plasma frequency is modeled theoretically and numerically. Owing to three independent approaches which lead to the same results (Particle-In-Cell simulations, theoretical and numerical modeling, as well as analytical calculations performed in the framework of weak turbulence theory extended to randomly inhomogeneous plasmas), electromagnetic emissions in the O-, X- and Z-modes, as well as their corresponding radiation rates, are calculated as a function of the ratio of the cyclotron to the plasma frequency ω_c/ω_p and the average level of random density fluctuations ΔN. These emissions are due to electrostatic waves transformations and mode conversion on random density fluctuations. In this view, the condition for appearance or absence of some modes, are discussed for the case of type III solar radio bursts.