User:Tohline/Apps/RotatingWhiteDwarfs - Revision history

Tohline: /* Binary White Dwarfs */

2019-07-05T19:33:00Z

Binary White Dwarfs

← Older revision		Revision as of 19:33, 5 July 2019
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	=Binary White Dwarfs=		=Binary White Dwarfs=
	* [https://ui.adsabs.harvard.edu/abs/1986ApJ...308..161H/abstract I. Hachisu, Y. Eriguchi & K. Nomoto (~~1986~~)], ApJ, 308, 161: ''Fate of Merging Double 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=

Tohline at 17:39, 5 July 2019

2019-07-05T17:39:03Z

← Older revision		Revision as of 17:39, 5 July 2019
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	* [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/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 (1986)], ApJ, 308, 161: ''Fate of Merging Double White Dwarfs''

	=See Also=		=See Also=

Tohline: /* Differential Rotation */

2019-06-24T23:50:59Z

Differential Rotation

← Older revision		Revision as of 23:50, 24 June 2019
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	* [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/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/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

Tohline: /* Differential Rotation */

2019-06-24T22:22:20Z

Differential Rotation

← Older revision		Revision as of 22:22, 24 June 2019
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	<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>		<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>
	</td></tr></table>		</td></tr></table>
	* [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/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

Tohline: /* Differential Rotation */

2019-06-16T22:56:57Z

Differential Rotation

← Older revision		Revision as of 22:56, 16 June 2019
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	<td align="center" width="5%"> </td><td align="left">		<td align="center" width="5%"> </td><td align="left">
	<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>
	</td></tr></table>		</td></tr></table>
	* [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/1969ApJ...155..987O/abstract J. P. Ostriker & J. -L. Tassoul (1969)], ApJ, 155, 987

Tohline: /* Example Equilibrium Configurations */

2019-06-16T22:46:05Z

Example Equilibrium Configurations

← Older revision		Revision as of 22:46, 16 June 2019
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	* [https://ui.adsabs.harvard.edu/abs/1966PhRvL..17..816O/abstract J. P. Ostriker, P. Bodenheimer & D. Lynden-Bell (1966)], Phys. Rev. Letters, 17, 816: ''Equilibrium Models of Differentially Rotating Zero-Temperature Stars''		* [https://ui.adsabs.harvard.edu/abs/1966PhRvL..17..816O/abstract J. P. Ostriker, P. Bodenheimer & D. Lynden-Bell (1966)], Phys. Rev. Letters, 17, 816: ''Equilibrium Models of Differentially Rotating Zero-Temperature Stars''
			<table border="0" align="center" width="100%" cellpadding="1"><tr>
			<td align="center" width="5%"> </td><td align="left">
			<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>
			</td></tr></table>
	* [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/1969ApJ...155..987O/abstract J. P. Ostriker & J. -L. Tassoul (1969)], ApJ, 155, 987
	* [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

Tohline: /* Differential Rotation */

2019-06-16T22:33:10Z

Differential Rotation

← Older revision		Revision as of 22:33, 16 June 2019
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	===Differential Rotation===		===Differential Rotation===

			* [https://ui.adsabs.harvard.edu/abs/1966PhRvL..17..816O/abstract J. P. Ostriker, P. Bodenheimer & D. Lynden-Bell (1966)], Phys. Rev. Letters, 17, 816: ''Equilibrium Models of Differentially Rotating Zero-Temperature Stars''
	* [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/1969ApJ...155..987O/abstract J. P. Ostriker & J. -L. Tassoul (1969)], ApJ, 155, 987
	* [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

Tohline: /* Uniform Rotation */

2019-06-16T21:39:53Z

Uniform Rotation

← Older revision		Revision as of 21:39, 16 June 2019
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	===Uniform Rotation===		===Uniform Rotation===

			* [https://ui.adsabs.harvard.edu/abs/1964ApJ...140..552J/abstract R. A. James (1964)], 140, 552
			<table border="0" align="center" width="100%" cellpadding="1"><tr>
			<td align="center" width="5%"> </td><td align="left">
			<font color="green">Structures have been determined for axially symmetric</font> [uniformly] <font color="green">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.</font>
			</td></tr></table>

	===Differential Rotation===		===Differential Rotation===

Tohline: /* See Also */

2019-06-16T21:24:43Z

Tohline: /* See Also */

2019-06-15T22:10:52Z

← Older revision		Revision as of 21:24, 16 June 2019
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	=See Also=		=See Also=
	* Our discussion of [[User:Tohline/Apps/RotatingPolytropes\|Rotating Polytropes: Example Equilibria]]		* Our discussion of [[User:Tohline/Apps/RotatingPolytropes\|Rotating Polytropes: Example Equilibria]]
			* [[User:Tohline/ThreeDimensionalConfigurations/BinaryFission\|Fission Theory of Binary Star Formation]]


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← Older revision		Revision as of 22:10, 15 June 2019
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	=See Also=		=See Also=
			* Our discussion of [[User:Tohline/Apps/RotatingPolytropes\|Rotating Polytropes: Example Equilibria]]


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