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.

http://arxiv.org/icons/sfx.gif

Comments are closed, but trackbacks and pingbacks are open.