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Stability of plasma cylinder with current in a helical plasma flow

Published online by Cambridge University Press:  19 March 2018

Anatoly S. Leonovich ,
Daniil A. Kozlov  and
Qiugang Zong
Anatoly S. Leonovich*
Affiliation:
Institute of Solar-Terrestrial Physics SB RAS, p. o. box 291, Irkutsk, 664033, Russia
Daniil A. Kozlov
Affiliation:
Institute of Solar-Terrestrial Physics SB RAS, p. o. box 291, Irkutsk, 664033, Russia
Qiugang Zong
Affiliation:
Institute of Space Physics and Applied Technology, Peking University, Beijing, China
*
†Email address for correspondence: leon@iszf.irk.ru
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Abstract

Stability of a plasma cylinder with a current wrapped by a helical plasma flow is studied. Unstable surface modes of magnetohydrodynamic (MHD) oscillations develop at the boundary of the cylinder enwrapped by the plasma flow. Unstable eigenmodes can also develop for which the plasma cylinder is a waveguide. The growth rate of the surface modes is much higher than that for the eigenmodes. It is shown that the asymmetric MHD modes in the plasma cylinder are stable if the velocity of the plasma flow is below a certain threshold. Such a plasma flow velocity threshold is absent for the symmetric modes. They are unstable in any arbitrarily slow plasma flows. For all surface modes there is an upper threshold for the flow velocity above which they are stable. The helicity index of the flow around the plasma cylinder significantly affects both the Mach number dependence of the surface wave growth rate and the velocity threshold values. The higher the index, the lower the upper threshold of the velocity jump above which the surface waves become stable. Calculations have been carried out for the growth rates of unstable oscillations in an equilibrium plasma cylinder with current serving as a model of the low-latitude boundary layer (LLBL) of the Earth’s magnetic tail. A tangential discontinuity model is used to simulate the geomagnetic tail boundary. It is shown that the magnetopause in the geotail LLBL is unstable to a surface wave (having the highest growth rate) in low- and medium-speed solar wind flows, but becomes stable to this wave in high-speed flows. However, it can remain weakly unstable to the radiative modes of MHD oscillations.

Keywords

plasma instabilitiesplasma wavesspace plasma physics
Type
Research Article
Information
Journal of Plasma Physics , Volume 84 , Issue 2 , April 2018 , 905840203
Copyright
© Cambridge University Press 2018 

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