The secular instability of axisymmetric collisionless star clusters

Details The secular instability of axisymmetric collisionless star clusters The secular instability of axisymmetric collisionless star clusters

Oct 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apj...380..511k&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 380, Oct. 20, 1991, p. 511-514.

Statistics

Computation

14

Computational Astrophysics, Gravitational Waves, Secular Variations, Star Clusters, Distribution Functions, Perturbation Theory

Scientific paper

This paper uses recently developed Hamiltonian techniques to investigate the stability of an axisymmetric, collisionless equilibrium, characterized by a distribution function f0(E, Jz, m) depending on both the particle energy E and azimuthal angular momentum Jz, as well as the particle mass m. The conserved total energy epsilon associated with a phase-preserving linear perturbation (delta) f is constructed, and it is shown that, generically, epsilon is not positive definite. It follows that, in the same sense as is true for rotating axisymmetric perfect fluid stars, 'generic' rotating axisymmetric equilibria f0(E, Jz, m) are unstable or at least marginally unstable in the presence of dissipation.

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