Chandrasekhar–Friedman–Schutz instability
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Chandrasekhar–Friedman–Schutz instability or shortly CFS instability refers to an instability that can occur in rapidly rotating
Roberts–Stewartson instability and CFS instability
Although it has been anticipated a long time (1883) ago by
The instability that arises only when there is a dissipation, but disappears in the absence of dissipation is referred to as the secular instability.[5] Both the Roberts–Stewartson instability and CFS instability are secular instability, although they do not both correspond to same modes in the following sense: In the absence of radiation reaction and viscosity, the Maclaurin spheroid (a model for rotating, self-gravitating body) becomes marginally or neutrally stable when its eccentricity reaches a critical value with two possible neutral modes, but it does not become unstable after this bifurcation. It is only in the presence of dissipation, Maclaurin spheroid becomes unstable when eccentricity exceeds its bifurcation value. The Roberts–Stewartson instability stems from one of the neutral mode, whereas the CFS instability stems from the other neutral mode.
References
- ^ Chandrasekhar, S. (1970). Solutions of two problems in the theory of gravitational radiation. Physical Review Letters, 24(11), 611.
- ^ Schutz, B. F., & Friedman, J. L. (1975). Gravitational radiation instability in rotating stars. The Astrophysical Journal, 199, L157-L159.
- ^ Friedman, J. L., & Schutz, B. F. (1978). Secular instability of rotating Newtonian stars. Astrophysical Journal, Part 1, vol. 222, May 15, 1978, p. 281-296., 222, 281-296.
- ^ Roberts, P. H., & Stewartson, K. (1963). On the Stability of a Maclaurin Spheroid of Small Viscosity. Astrophysical Journal, vol. 137, p. 777, 137, 777.
- ^ Chandrasekhar, S. (1987). Ellipsoidal figures of equilibrium. New York: Dover. Page 95.