# User:Tohline/Apps/RotatingWhiteDwarfs

(Difference between revisions)
 Revision as of 11:39, 5 July 2019 (view source)Tohline (Talk | contribs)← Older edit Current revision as of 13:33, 5 July 2019 (view source)Tohline (Talk | contribs) (→Binary White Dwarfs) Line 30: Line 30: =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=

# Rotationally Flattened White Dwarfs

## 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.