Structure and stability of rotating fluid disks around massive objects. I - Newtonian formulation

Details Structure and stability of rotating fluid disks around massive objects. I - Newtonian formulation Structure and stability of rotating fluid disks around massive objects. I - Newtonian formulation

Dec 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981japa....2..421c&link_type=abstract

Journal of Astrophysics and Astronomy, vol. 2, Dec. 1981, p. 421-437.

Statistics

Computation

7

Celestial Bodies, Computational Fluid Dynamics, Flow Stability, Newtonian Fluids, Rotating Disks, Rotating Fluids, Astrophysics, Equilibrium Flow, Flow Equations, Flow Velocity, Kepler Laws, Perturbation Theory, Velocity Distribution

Scientific paper

The structure and stability of a system of an uncharged fluid disk with nonzero pressure rotating about a massive object are examined in a Newtonian formulation neglecting disk self-gravitation. A class of steady-state solution to the equations governing the dynamics of a perfect fluid rotating around a central gravitating source is obtained, and the stability of the configuration to linear axisymmetric perturbations is analyzed for cases of different density and velocity distributions and disk radii. The critical adiabatic index for the onset of instability is found always to be less than 4/3, indicating the disk to be stable for all cases under axisymmetric perturbations. Ordinary perfect fluid disks with an adiabatic index of 5/3 are thus stable to radial perturbations of frequency equal to sq rt (MG/r-cubed), where M is the central mass.

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