User:Tohline/Apps/RotatingWhiteDwarfs

Rotationally Flattened White Dwarfs

Example Equilibrium Configurations

Uniform Rotation

• R. A. James (1964), 140, 552

Structures have been determined for axially symmetric [uniformly] rotating gas masses, in the polytropic and white-dwarf cases … Physical parameters for the rotating configurations were obtained for values of n < 3, and for a range of white-dwarf configurations. The existence of forms of bifurcation of the axially symmetric series of equilibrium forms was also investigated. The white-dwarf series proved to lack such points of bifurcation, but they were found on the polytropic series for n < 0.808.

Differential Rotation

• J. P. Ostriker, P. Bodenheimer & D. Lynden-Bell (1966), Phys. Rev. Letters, 17, 816: Equilibrium Models of Differentially Rotating Zero-Temperature Stars

… work by Roxburgh (1965, Z. Astrophys., 62, 134), Anand (1965, Proc. Natl. Acad. Sci. U.S., 54, 23), and James (1964, ApJ, 140, 552) shows that the [Chandrasekhar (1931, ApJ, 74, 81)] mass limit <math>~M_3</math> is increased by only a few percent when uniform rotation is included in the models, … In this Letter we demonstrate that white-dwarf models with masses considerably greater than <math>~M_3</math> are possible if differential rotation is allowed … models are based on the physical assumption of an axially symmetric, completely degenerate, self-gravitating fluid, in which the effects of viscosity, magnetic fields, meridional circulation, and relativistic terms in the hydrodynamical equations have been neglected.

• J. -L. Tassoul & J. P. Ostriker (1968), ApJ, 154, 613: On the Oscillations and Stability of Rotating Stellar Models. I. Mathematical Techniques
• J. P. Ostriker & J. -L. Tassoul (1969), ApJ, 155, 987: On the Oscillations and Stability of Rotating Stellar Models. II. Rapidly Rotating White Dwarfs
• R. H. Durisen & J. N. Imamura (1981), ApJ, 243, 612

See Also

• Our discussion of Rotating Polytropes: Example Equilibria
• Fission Theory of Binary Star Formation

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