A viscous magnetohydrodynamic Kelvin Helmholtz instability in the interface of two fluid layer Part II An application to the atmosphere of the Sun

TL;DR

This paper investigates how parameters like wave number, shear velocity, magnetic field, and temperature influence the growth rate of magnetized Kelvin-Helmholtz instability at the solar atmosphere interface, using a viscous magnetohydrodynamic model.

Contribution

It applies a viscous MHD model to analyze the effects of multiple parameters on KHI growth in the solar atmosphere, extending previous theoretical work.

Findings

KHI occurs under various parameter conditions in the solar atmosphere.

Magnetic field and shear velocity significantly affect instability growth.

Parameter values relevant to the solar atmosphere were identified.

Abstract

The main aim of this submission is to investigate the effects of some parameters like wave number, shear velocity, magnetic field and temperature for the growth rate of the magnetized Kelvin-Helmholtz instability (KHI) with incessant profiles through interface of two viscous fluid layer occurred in the solar atmosphere using the model of Hoshoudy, Cavus and Mahdy (2019). In this examination, the presence of KHI is identified for the various cases of wave number, magnetic field, shear velocity and temperature in the solar atmosphere. The sensible values of these parameters were acquired.