Jeans Instability of Tidal Tails and Molecular Filaments

Details Jeans Instability of Tidal Tails and Molecular Filaments Jeans Instability of Tidal Tails and Molecular Filaments

May 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010dda....41.0508q&link_type=abstract

American Astronomical Society, DDA meeting #41, #5.08; Bulletin of the American Astronomical Society, Vol. 41, p.930

Astronomy and Astrophysics

Astronomy

Scientific paper

Tidal tails composed of stars should be unstable to the Jeans instability and this can cause them to look like beads on a string. The Jeans wavelength and tail diameter determine the wavelength and growth rate of the fastest growing unstable mode. Consequently the distance along the tail to the first clump and spacing between clumps can be used to estimate the mass density in the tail and its longitudinal velocity dispersion. Clumps in the tidal tails of the globular cluster Palomar 5 could be due to Jeans instability. We find that their spacing is consistent with the fastest growing mode if the velocity dispersion in the tail is similar to that in the cluster itself.

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