Other
Scientific paper
Dec 1986
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986p%26ss...34.1223u&link_type=abstract
Planetary and Space Science (ISSN 0032-0633), vol. 34, Dec. 1986, p. 1223-1227.
Other
12
Kelvin-Helmholtz Instability, Magnetospheric Instability, Plasma Layers, Space Plasmas, Critical Velocity, Energy Spectra, Flow Velocity
Scientific paper
The hydromagnetic Kelvin-Helmholtz (K-H) instability problem is studied analytically for a three-layered system, by arriving at the marginal instability condition. As the magnetic field directions are taken to vary in the three regions, both the angle and finite thickness effects are seen on the instability criterion. When the relative flow speed of the plasmas on the two sides of the interfaces separating the inner and the surrounding layers is U less than U(c), where U(c) is the critical speed, the system is stable both for symmetric and asymmetric perturbations. However, unlike the case of the interface bounded by two semiinfinite media, U(c) is no longer the minimum critical speed above which the system will be unstable for all wavenumbers; another critical speed U-asterisk greater than U(c) is introduced due to the finiteness of the system. When U is in the range between U(c) and U-asterisk the instability can set in either through the symmetric or asymmetric mode, depending on the ratio of the plasma parameters and angle between the magnetic field directions across the boundaries. The instability arises for a finite range of wavenumbers, thus giving rise to the upper and lower cut-off frequencies for the spectra of hydromagnetic surface waves generated by the K-H instability mechanism. When U greater than U-asterisk, both the modes are unstable for short wavelengths. The results are finally used to explain some observational features of the dependence of hydromagnetic energy spectra in the magnetosphere on the interplanetary parameters.
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