Difference between revisions of "User:Tohline/Apps/RotatingWhiteDwarfs"

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===Uniform Rotation===
===Uniform Rotation===


* [https://ui.adsabs.harvard.edu/abs/1964ApJ...140..552J/abstract R. A. James (1964)], 140, 552
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<td align="center" width="5%">&nbsp;</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 &hellip; 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===


* [https://ui.adsabs.harvard.edu/abs/1969ApJ...155..987O/abstract J. P. Ostriker &amp; J. -L. Tassoul (1969)], ApJ, 155, 987
* [https://ui.adsabs.harvard.edu/abs/1966PhRvL..17..816O/abstract J. P. Ostriker, P. Bodenheimer &amp; 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%">&nbsp;</td><td align="left">
<font color="green">&hellip; 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, &hellip;</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 &hellip; 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>
* [https://ui.adsabs.harvard.edu/abs/1968ApJ...154..613T/abstract J. -L. Tassoul &amp; 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 &amp; 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 &amp; J. N. Imamura (1981)], ApJ, 243, 612
* [https://ui.adsabs.harvard.edu/abs/1981ApJ...243..612D/abstract R. H. Durisen &amp; J. N. Imamura (1981)], ApJ, 243, 612
=Binary White Dwarfs=
* [https://ui.adsabs.harvard.edu/abs/1986ApJ...308..161H/abstract I. Hachisu, Y. Eriguchi &amp; 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 &amp; K. Nomoto (1986b)], ApJ, 311, 214:  ''Fate of Merging Double White Dwarfs. II &#8212; Numerical Method''
* [https://ui.adsabs.harvard.edu/abs/2009ApJS..184..248E/abstract W. Even &amp; J. E. Tohline (2009)], ApJSuppl., 184, 248:  ''Constructing Synchronously Rotating Double White Dwarf Binaries''


=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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Latest revision as of 19:33, 5 July 2019

Rotationally Flattened White Dwarfs

Whitworth's (1981) Isothermal Free-Energy Surface
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Example Equilibrium Configurations

Uniform Rotation

 

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

 

… 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.

Binary White Dwarfs

See Also


Whitworth's (1981) Isothermal Free-Energy Surface

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