Weak compressible magnetohydrodynamic turbulence in the solar corona

Preprint

21 November 2005

preprint
Published by arXiv in arXiv

https://doi.org/10.48550/arXiv.astro-ph/0511586

Abstract

This Letter presents a calculation of the power spectra of weakly turbulent Alfven waves and fast magnetosonic waves ("fast waves") in low-beta plasmas. It is shown that three-wave interactions transfer energy to high-frequency fast waves and, to a lesser extent, high-frequency Alfven waves. MHD turbulence is thus a promising mechanism for producing the high-frequency waves needed to explain the anisotropic heating of minor ions in the solar corona.

Keywords

COMPRESSIBLE MAGNETOHYDRODYNAMIC
MAGNETOHYDRODYNAMIC TURBULENCE
WEAK COMPRESSIBLE
SOLAR CORONA
ALFVEN WAVES
FAST WAVES
TURBULENCE
MHD

All Related Versions

Version 1, 2005-11-21, ArXiv
Published version: Physical Review Letters, 95 (26), 265004.

This publication has 0 references indexed in Scilit: