On Kelvin-Helmholtz and parametric instabilities driven by coronal waves

TL;DR

This paper investigates how Kelvin-Helmholtz and parametric instabilities, driven by coronal MHD waves, contribute to energy extraction and turbulence in the solar corona, revealing conditions favoring each instability.

Contribution

It derives a Mathieu equation to analyze the stability of oscillatory shear flows and identifies a parametric instability that enhances energy transfer in coronal flux tubes.

Findings

Both instabilities can grow in coronal conditions.

Parametric instability produces smaller scale disturbances.

Time-scale for instabilities is approximately 100 seconds.

Abstract

The Kelvin-Helmholtz instability has been proposed as a mechanism to extract energy from magnetohydrodynamic (MHD) kink waves in flux tubes, and to drive dissipation of this wave energy through turbulence. It is therefore a potentially important process in heating the solar corona. However, it is unclear how the instability is influenced by the oscillatory shear flow associated with an MHD wave. We investigate the linear stability of a discontinuous oscillatory shear flow in the presence of a horizontal magnetic field within a Cartesian framework that captures the essential features of MHD oscillations in flux tubes. We derive a Mathieu equation for the Lagrangian displacement of the interface and analyse its properties, identifying two different instabilities: a Kelvin-Helmholtz instability and a parametric instability involving resonance between the oscillatory shear flow and two surface Alfv\'{e}n waves. The latter occurs when the system is Kelvin-Helmholtz stable, thus favouring modes that vary along the flux tube, and as a consequence provides an important and additional mechanism to extract energy. When applied to flows with the characteristic properties of kink waves in the solar corona, both instabilities can grow, with the parametric instability capable of generating smaller scale disturbances along the magnetic field than possible via the Kelvin-Helmholtz instability. The characteristic time-scale for these instabilities is $\sim 100$ s, for wavelengths of $200$ km. The parametric instability is more likely to occur for smaller density contrasts and larger velocity shears, making its development more likely on coronal loops than on prominence threads.