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(Binary White Dwarfs)
 
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=Binary White Dwarfs=
=Binary White Dwarfs=
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* [https://ui.adsabs.harvard.edu/abs/1986ApJ...308..161H/abstract I. Hachisu, Y. Eriguchi &amp; K. Nomoto (1986)], ApJ, 308, 161:  ''Fate of Merging Double White Dwarfs''
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* [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''
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* [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''
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* [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=

Current revision as of 13:33, 5 July 2019

Contents

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 ~M_3 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 ~M_3 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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