Astronomy and Astrophysics – Astrophysics
Scientific paper
2006-10-31
Astrophys.Space Sci. 300 (2005) 395
Astronomy and Astrophysics
Astrophysics
24 pages, 8 figures
Scientific paper
10.1007/s10509-005-8792-2
This work derives the linearized equations of motion, the Lagrangian density, the Hamiltonian density, and the canonical angular momentum density for general perturbations [$\propto \exp(im\phi)$ with $m=0,\pm 1,..$] of a geometrically thin self-gravitating, homentropic fluid disk including the pressure. The theory is applied to ``eccentric,'' $m=\pm 1$ perturbations of a geometrically thin Keplerian disk. We find $m=1$ modes at low frequencies relative to the Keplerian frequency. Further, it shown that these modes can have negative energy and negative angular momentum. The radial propagation of these low frequency $m=1$ modes can transport angular momentum away from the inner region of a disk and thus increase the rate of mass accretion. Depending on the radial boundary conditions there can be discrete low-frequency, negative-energy, $m=1$ modes.
Lovelace Richard V. E.
Zhang Lianchang
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