During the last 60s years, systematic observations (in situ) of plasma parameters and magnetic field in the solar wind near the Earth has been performed. The data obtained combined with the ones obtained from Solar observations has help us to understand that the origin of the most important magnetic storms are related with transient solar phenomena. Magnetic storms are associated with an intense and long duration of the southward component of interplanetary magnetic field that facilitate the energetic coupling solar wind-Earth magnetosphere by magnetic reconnection. In this contest, radio emission can occur associated with magnetic structures traveling in the interplanetary medium ejected from the Sun. In this work we will use computer simulation to understand the physical process of radio emission generated by potentially geoeffective phenomena. Some radio emissions generated by this kind of phenomena are characterized by a main frequency, near of local plasma frequency and harmonics of this one. Recent theories suggest that this kind of waves can be generated by multiples electron beams that are injected into interplanetary medium during solar eruptive events. Particle simulation (PIC-code) will be used to study wave-particle and wave-wave interaction. In particular we focus on spatio-temporal evolution of electromagnetic waves generated by Langmuir wave packages resulting from the interaction of multiples electron beams with solar wind plasma associated with type II and III solar radio bursts.
News published in Agência FAPESP Newsletter about the scholarship: