Kinetic Alfvén Waves Excited by Oblique Magnetohydrodynamic Alfvén Waves in Coronal Holes

Details Kinetic Alfvén Waves Excited by Oblique Magnetohydrodynamic Alfvén Waves in Coronal Holes Kinetic Alfvén Waves Excited by Oblique Magnetohydrodynamic Alfvén Waves in Coronal Holes

Jul 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011apj...735..114z&link_type=abstract

The Astrophysical Journal, Volume 735, Issue 2, article id. 114 (2011).

Astronomy and Astrophysics

Astronomy

Instabilities, Plasmas, Sun: Corona, Waves

Scientific paper

Kinetic Alfvén waves (KAWs) are small-scale dispersive AWs that can play an important role in particle heating and acceleration of space and solar plasmas. An excitation mechanism for KAWs created by the coupling between large-scale oblique AWs and small-scale KAWs is presented in this paper. Taking into account both the collisional and Landau damping dissipations, the results show that the net growth rate of the excited KAWs increases with their perpendicular wavenumber k bottom and reaches maximum at λ e k bottom ~ 0.3, where λ e is the electron inertial length. However, for KAWs with shorter perpendicular wavelengths, the net growth rate decreases rapidly due to dissipative effects. The evaluation of the threshold amplitude of the AW implies that for KAWs with λ e k bottom < 0.3, the relative threshold amplitude is well below 10%, which is easy to satisfy. In particular, when applying this mechanism to the case of a solar coronal hole containing a dense plume structure, our results show that KAWs with λ e k bottom < 0.3 can be not only efficiently excited in the interplume region but also strongly dissipated in the dense plume due to the Landau damping.

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