Viscosity effects on waves in partially and fully ionized plasma in magnetic field

Abstract

Viscosity is discussed in multicomponent partially and fully ionized plasma, and its effects on two very different waves (Alfven and Langmuir) in solar atmosphere. A full set of viscosity coefficients is presented which includes coefficients for electrons, protons and hydrogen atoms. These are applied to layers with mostly magnetized protons in solar chromosphere where the Alfven wave could in principle be expected. The viscosity coefficients are calculated and presented graphically for the altitudes between 700 and 2200 km, and required corresponding cross sections for various types of collisions are given in terms of altitude. It is shown that in chromosphere the viscosity plays no role for the Alfven wave, which is only strongly affected by ion friction with neutrals. In corona, assuming the magnetic field of a few Gauss, the Alfven wave is more affected by ion viscosity than by ion-electron friction only for wavelengths shorter that 1-30 km, dependent on parameters and assuming the perturbed magnetic field of one percent of its equilibrium value. For the Langmuir wave the viscosity-friction interplay in chromosphere is shown to be dependent on altitude and on wavelengths. In corona the viscosity is the main dissipative mechanism acting on the Langmuir mode.

5 figures

References in corpus (2)

• Energy flux of Alfven waves in weakly ionized plasma
• Kinetic instability of drift-Alfven waves in solar corona and stochastic heating

Cited by in corpus (4)

• Multifluid modeling of magnetosonic wave propagation in the solar chromosphere -- effects of impact ionization and radiative recombination
• The non-ideal finite Larmor radius effect in the solar atmosphere
• The Effect of Anisotropic Viscosity on the Nonlinear Kink Instability
• Fast giant flares in discs around supermassive black holes