Nonlinear wave dynamics in the dissipation range

Details Nonlinear wave dynamics in the dissipation range Nonlinear wave dynamics in the dissipation range

Feb 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003padeu..13..153v&link_type=abstract

In: Contributions to NATO Advanced Research Workshop Turbulence, Waves, and Instabilities in the Solar Plasma; Hungary, 16-20 Se

Astronomy and Astrophysics

Astronomy

Scientific paper

There is abundant observational evidence that the ions in the solar corona (in particular, O(+5) ) are heated anisotropicaly, predominantly across the background magnetic field. This heating is usually attributed to the dissipation of ion-cyclotron waves. We study an alternative possibility with the dissipation range in the solar corona formed by the kinetic Alfvén waves (KAWs) which are very short- wavelengths across the magnetic field. Instead of transport of MHD wave energy towards to the range of ion-cyclotron waves, we study transport into the dissipation range of KAWs. We show that the nonlinear excitation of short-wavelength (of the order 10 m) KAWs in the extended solar corona and solar wind can be provided by upward-propagating fast and Alfvén MHD waves launched from the coronal base by the convection or magnetic reconnection. KAWs are very efficient in the energy exchange with plasma particles, providing plasma heating and particles acceleration. In particular, these transversal wavelengths make KAWs accessible for the stochastic perpendicular heating of oxygen ions when the wave/background magnetic field ratio exceeds 0.005. Both the quasi-steady coronal heating and the transient heating events observed by Yohkoh and SOHO may be due to KAWs that are nonlinearly excited by MHD waves.

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