Abstract
We interpret observations of wave-like phenomena in cometary ion tails in terms of the interaction of the tails with the solar wind through Kelvin-Helmholtz helical instabilities. The calculations are applied to three comets, Comet Kohoutek (1973f), Comet Arend Roland (1957 III) and Comet Morehouse (1908c). Whilst some disagreement is found with earlier work, it is nevertheless shown that, assuming typical parameters, the growth rate of the K-H helical mode should be significant for wavelengths approximately equal to the tail radius.
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