Nonlinear Evolution of Kinetic Alfvén Waves and Filament Formation

Details Nonlinear Evolution of Kinetic Alfvén Waves and Filament Formation Nonlinear Evolution of Kinetic Alfvén Waves and Filament Formation

Jul 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005soph..229..287m&link_type=abstract

Solar Physics, Volume 229, Issue 2, pp.287-304

Physics

2

Scientific paper

The transfer of wave energy to plasma energy is a very crucial issue in coronal holes and helmet streamer regions. Mixed mode Alfvén waves, also known as kinetic Alfvén wave (KAW) can play an important role in the energization of the plasma particles because of their potential ability to heat and accelerate the plasma particles via Landau damping. This paper presents an investigation of the growth of a Gaussian perturbation on a non-uniform kinetic Alfvén wave having Gaussian wave front. The effect of the nonlinear coupling between the main KAW and the perturbation has been studied. The dynamical equations for the field of the main KAW and the perturbation have been established and their semi-analytical solution has been obtained in the low (β≪ m e/ m i≪ 1) and the high (β≫ m e/ m i≪ 1) β cases. The critical field of the main KAW and the perturbation has been evaluated. Nonlinear evolution of the main KAW and the perturbation into the filamentary structures and its dependence on various parameters of the solar wind and the solar corona have been investigated in detail. These filamentary structures can act as a source for the particle acceleration by wave particle interaction because the KAWs are mixed modes and Landau damping is possible. Especially, in the solar corona, the low β and the high β cases could correspond to the coronal holes and the helmet streamer. The presence of the primary and the secondary filaments of the perturbation may change the spectrum of the Alfvénic turbulence in the solar wind.

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