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

TL;DR

This study uses 3D MHD simulations and synthetic spectral modeling to investigate how transverse MHD wave-driven turbulence affects the density filling factor in the solar corona, providing insights into coronal heating mechanisms.

Contribution

It introduces a combined simulation and forward modeling approach to quantify the impact of MHD turbulence on coronal density structures, aligning with observational data.

Findings

Turbulence increases the density filling factor in the solar corona.

Simulated filling factors agree with observational measurements.

Generated synthetic spectra match observed line ratios.

Abstract

It is well established that the 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 due to the MHD wave-driven turbulence. In this work, we have studied the variation in the filling factor of overdense structures in the solar corona due to the generation of the transverse MHD wave-driven turbulence. Using 3D MHD simulations, we estimate the density filling factor of an open magnetic structure by calculating the fraction of the volume occupied by the overdense plasma structures to the entire volume of the simulation domain. Next, we perform forward modeling and generate synthetic spectra of Fe XIII 10749 \AA\ and 10800 \AA\ density sensitive line pairs using FoMo. Using the synthetic images, we again estimate the filling factors. The estimated filling factors obtained from both methods are in reasonable agreement. Also, our results match fairly well with the observations of filling factors in coronal holes and loops. Our results show that the generation of turbulence increases the filling factor of the solar corona.