CONICET | Buscador de Institutos y Recursos Humanos

Because of its proximity, our Sun provides a unique opportunity to perform high resolution observations of its outer layers through-out the whole electromagnetic spectrum. We can also theoretically model most of the fascinating physical phenomena taking place on theSun, as well as their impact on the solar system.Many of these phenomena can be properly studied within the framework of magnetohydrodynamics. More specifically, we assume afully ionized hydrogen plasma and adopt the more comprehensive two-fluid magnetohydrodynamic approximation. For problems suchas the solar wind or magnetic loops in the solar corona, which are shaped by a relatively strong mean magnetic field, the reduced mag-netohydrodynamic approximation is often used.We will review the basic features of both two-fluid and one-fluid magnetohydrodynamics, and focus on two particular applications:the turbulent heating of coronal active regions and the dynamics of the solar wind.