How transverse MHD wave-driven turbulence influences the density filling factor in the solar corona?. (arXiv:2110.06844v1 [astro-ph.SR])

<a href="http://arxiv.org/find/astro-ph/1/au:+Sen_S/0/1/0/all/0/1">Samrat Sen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pant_V/0/1/0/all/0/1">Vaibhav Pant</a>

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.

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.

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