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It is well established that the transverse MHD waves are ubiquitous in thesolar corona. One of the possible mechanisms for heating both open (e.g.coronal holes) and closed (e.g. coronal loops) magnetic field regions of thesolar corona is due to the MHD wave-driven turbulence. In this work, we havestudied the variation in the filling factor of overdense structures in thesolar corona due to the generation of the transverse MHD wave-driventurbulence. Using 3D MHD simulations, we estimate the density filling factor ofan open magnetic structure by calculating the fraction of the volume occupiedby the overdense plasma structures to the entire volume of the simulationdomain. Next, we perform forward modeling and generate synthetic spectra of FeXIII 10749 \AA\ and 10800 \AA\ density sensitive line pairs using FoMo. Usingthe synthetic images, we again estimate the filling factors. The estimatedfilling factors obtained from both methods are in reasonable agreement. Also,our results match fairly well with the observations of filling factors incoronal holes and loops. Our results show that the generation of turbulenceincreases the filling factor of the solar corona.

How transverse MHD wave-driven turbulence influences the density filling factor in the solar corona?