| Abstract : | It is well established that transverse MHD waves are ubiquitous in the solar corona. One of the possible mechanisms for heating both open (e.g., coronal holes) and closed (e.g., coronal loops) magnetic field regions of the solar corona is MHD wave-driven turbulence. Using very high-resolution 3D MHD simulations and forward modelling, we study the density filling factor of an open magnetic structure in the solar corona. In this talk, I will present a novel scenario where the filling factor of overdense structures in the solar corona varies due to the generation of transverse MHD wave-driven turbulence. Further, I will show a comparison of the theoretical estimates with the observations. Finally, I will discuss its implication on the energy flux carried by the MHD waves and the overall coronal heating budget. |
