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Tidal tails composed of stars should be unstable to the Jeans instability andthis can cause them to look like beads on a string. The Jeans wavelength andtail diameter determine the wavelength and growth rate of the fastest growingunstable mode. Consequently the distance along the tail to the first clump andspacing between clumps can be used to estimate the mass density in the tail andits longitudinal velocity dispersion. Clumps in the tidal tails of the globularcluster Palomar 5 could be due to Jeans instability. We find that their spacingis consistent with the fastest growing mode if the velocity dispersion in thetail is similar to that in the cluster itself. While all tidal tails shouldexhibit gravitational instability, we find that clusters or galaxies with lowconcentration parameters are most likely to exhibit short wavelength rapidlygrowing Jeans modes in their tidal tails.

Jeans Instability of Palomar 5's Tidal Tail