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Kelvin-Helmholtz instability in type-1 comet tails and associated phenomena

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Abstract

Selected problems of the solar wind — comet tail coupling that are currently accessible to quantitative analysis are reviewed. The model of a comet tail as a plasma cylinder separated by a tangential discontinuity surface from the solar wind is discussed in detail. This model is compatible with the well-known Alfvén mechanism of formation of the comet tail. The stability problem of the comet tail boundary (considered as a discontinuity surface) is solved. Under typical conditions a comet tail boundary can undergo the Kelvin-Helmholtz instability. With finite amplitude the stabilizing effect of the magnetic field increases, and waves become stabilized. This model supplies a detailed quantitative description of helical waves observed in type-1 comet tails. A more general model of the tail boundary as a transition layer with a continuous change of the plasma parameters within it is also considered.

This theory, in principle, enables us to solve one of the fundamental problems of cometary physics: the magnetic field of the comet tail can be derived from the observations of helical waves. This field turns out to be of the order of the interplanetary field. Various other considerations, discussed in this review, also support this conclusion.

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  1. Dept. of Geophysics and Planetary Sciences, Tel-Aviv University, Ramat-Aviv, Israel

    Alexander I. Ershkovich

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Ershkovich, A.I. Kelvin-Helmholtz instability in type-1 comet tails and associated phenomena. Space Sci Rev 25, 3–34 (1980). https://doi.org/10.1007/BF00200796

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  • DOI: https://doi.org/10.1007/BF00200796

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