Kelvin-Helmholtz instability in an Alfven resonant layer of a solar coronal loop

Details Kelvin-Helmholtz instability in an Alfven resonant layer of a solar coronal loop Kelvin-Helmholtz instability in an Alfven resonant layer of a solar coronal loop

Jul 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991soph..134..111u&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 134, July 1991, p. 111-121. Research supported by NASA and NSF.

Physics

8

Coronal Loops, Kelvin-Helmholtz Instability, Magnetohydrodynamic Waves, Solar Corona, Boundary Value Problems, Resonant Frequencies

Scientific paper

A Kelvin-Helmholtz instability has been identified numerically on an azimuthally symmetric Alfven resonant layer in an axially bounded, straight cylindrical coronal loop. The set of equations is solved numerically as an initial value problem. The linear growth rate of this instability is shown to be approximately proportional to the Alfven driving amplitude and inversely proportional to the width of the Alfven resonant layer. It is also shown that the linear growth rate increases linearly with m - 1 up to a certain m, reaches its maximum value for the mode whose half wavelength is comparable to the Alfven resonant layer width, and decreases at higher azimuthal mode number.

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