Difference between revisions of "User:Tohline/Apps/RotatingWhiteDwarfs"
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<font color="green">… 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</font> [Chandrasekhar (1931, ApJ, 74, 81)] <font color="green">mass limit <math>~M_3</math> is increased by only a few percent when uniform rotation is included in the models, …</font> | <font color="green">… 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</font> [Chandrasekhar (1931, ApJ, 74, 81)] <font color="green">mass limit <math>~M_3</math> is increased by only a few percent when uniform rotation is included in the models, …</font> | ||
<font color="green">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.</font> | |||
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* [https://ui.adsabs.harvard.edu/abs/1969ApJ...155..987O/abstract J. P. Ostriker & J. -L. Tassoul (1969)], ApJ, 155, 987 | * [https://ui.adsabs.harvard.edu/abs/1968ApJ...154..613T/abstract J. -L. Tassoul & J. P. Ostriker (1968)], ApJ, 154, 613: ''On the Oscillations and Stability of Rotating Stellar Models. I. Mathematical Techniques'' | ||
* [https://ui.adsabs.harvard.edu/abs/1969ApJ...155..987O/abstract J. P. Ostriker & J. -L. Tassoul (1969)], ApJ, 155, 987: ''On the Oscillations and Stability of Rotating Stellar Models. II. Rapidly Rotating White Dwarfs'' | |||
* [https://ui.adsabs.harvard.edu/abs/1975ApJ...195..483D/abstract R. H. Durisen (1975)], ApJ, 195, 483: ''Viscous effects in rapidly rotating stars with application to white-dwarf models. III. Further numerical results'' | |||
* [https://ui.adsabs.harvard.edu/abs/1975ApJ...199..179D/abstract R. H. Durisen (1975)], ApJ, 199, 179: ''Upper mass limits for stable rotating white dwarfs'' | |||
* [https://ui.adsabs.harvard.edu/abs/1981ApJ...243..612D/abstract R. H. Durisen & J. N. Imamura (1981)], ApJ, 243, 612 | * [https://ui.adsabs.harvard.edu/abs/1981ApJ...243..612D/abstract R. H. Durisen & J. N. Imamura (1981)], ApJ, 243, 612 | ||
=Binary White Dwarfs= | |||
* [https://ui.adsabs.harvard.edu/abs/1986ApJ...308..161H/abstract I. Hachisu, Y. Eriguchi & K. Nomoto (1986a)], ApJ, 308, 161: ''Fate of Merging Double White Dwarfs'' | |||
* [https://ui.adsabs.harvard.edu/abs/1986ApJ...311..214H/abstract I. Hachisu, Y. Eriguchi & K. Nomoto (1986b)], ApJ, 311, 214: ''Fate of Merging Double White Dwarfs. II — Numerical Method'' | |||
* [https://ui.adsabs.harvard.edu/abs/2009ApJS..184..248E/abstract W. Even & J. E. Tohline (2009)], ApJSuppl., 184, 248: ''Constructing Synchronously Rotating Double White Dwarf Binaries'' | |||
=See Also= | =See Also= | ||
Latest revision as of 19:33, 5 July 2019
Rotationally Flattened White Dwarfs
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Example Equilibrium Configurations
Uniform Rotation
- R. A. James (1964), 140, 552
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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
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… 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 (1975), ApJ, 195, 483: Viscous effects in rapidly rotating stars with application to white-dwarf models. III. Further numerical results
- R. H. Durisen (1975), ApJ, 199, 179: Upper mass limits for stable rotating white dwarfs
- R. H. Durisen & J. N. Imamura (1981), ApJ, 243, 612
Binary White Dwarfs
- I. Hachisu, Y. Eriguchi & K. Nomoto (1986a), ApJ, 308, 161: Fate of Merging Double White Dwarfs
- I. Hachisu, Y. Eriguchi & K. Nomoto (1986b), ApJ, 311, 214: Fate of Merging Double White Dwarfs. II — Numerical Method
- W. Even & J. E. Tohline (2009), ApJSuppl., 184, 248: Constructing Synchronously Rotating Double White Dwarf Binaries
See Also
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