Wave energy dissipation by phase mixing in magnetic coronal plasmas

Free access article

Issue		A&A Volume 440, Number 1, September II 2005


Page(s)		357 - 366
Section		The Sun
DOI		http://dx.doi.org/10.1051/0004-6361:20052985

A&A 440, 357-366 (2005)
DOI: 10.1051/0004-6361:20052985

Wave energy dissipation by phase mixing in magnetic coronal plasmas

I. J. D. Craig and G. Fruit

University of Waikato, New Zealand
e-mail: fruit@waikato.ac.nz

(Received 4 March 2005 / Accepted 2 May 2005 )

Abstract
Wave energy dissipation by viscous and resistive damping in magnetic coronal plasmas is examined. We begin by pointing out that since the dimensionless viscous damping coefficient $\nu$ is generally much greater than the dimensionless resistivity $\eta$ , viscous dissipation can be expected to be the dominant mechanism in many coronal applications. A detailed analysis is presented for the case of perpendicular polarized shear wave disturbances which propagate in a horizontally stratified magnetic channel. We show that when the equilibrium field contains a neutral line (specifically, $\vec{B} = B_0 y \vec{\widehat{x}}\,$ ) the development of small length scales by phase mixing $\ell\simeq(\eta+\nu)^{1/3}$ leads to efficient wave energy losses: in particular, the bulk of the energy losses take place over the time interval $(\eta+\nu)^{-1/3}$ . However, the later stages of the decay depends critically on whether viscosity or resistivity provides the dominant damping mechanism. When resistivity is sufficiently small the decay rate weakens at later times due to the emergence of a self-similar mode which allows a separation of the global kinetic and magnetic energies ( $\nu\gg\eta$ ). If the resistivity is large enough but still not dominant, self-similar behaviour can give way to monotonic exponential damping on the visco-resistive length scale $\ell\simeq(\eta\nu)^{1/6}$ . In either case, provided only that $\nu > \eta$ , energy equipartition eventually breaks down and the remnants of the initial wave energy wind up mainly in the magnetic field.

Key words: Sun: corona -- magnetohydrodynamics (MHD) -- waves

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