Physics – Fluid Dynamics
Scientific paper
May 1975
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975apj...197..745s&link_type=abstract
Astrophysical Journal, vol. 197, May 1, 1975, pt. 1, p. 745-765.
Physics
Fluid Dynamics
50
Astronomical Models, Fluid Dynamics, Relativity, Rotary Stability, Stellar Rotation, Ideal Fluids, Relativistic Effects, Stellar Structure, Thermal Conductivity, Viscosity
Scientific paper
The stability of axisymmetric, differential rotation in nonmagnetic stars of uniform chemical composition is studied in the context of general relativity theory. Criteria are found for stability against local, linear, axisymmetric perturbations in conducting, viscous stars and in perfect fluid models. When stated in the proper language, the relativistic stability conditions have the same forms as the nonrelativistic conditions. When thermal conduction is much more efficient than viscosity, a star must be barotropic (the level surfaces of the pressure and the total density of mass energy must coincide) and the gradient of the geometrical angular momentum (L) must never point toward the interior of the quasicylindrical level surfaces of L. When viscosity dominates thermal conductivity by a large margin, a star must be barotropic. When conduction and viscosity have comparable efficiencies or are absent, the criteria are slightly more complex. Applications of the stability conditions to models of specific astrophysical objects are discussed.
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