Editing Apps/RotatingWhiteDwarfs (section)

==Example Equilibrium Configurations==
===Uniform Rotation===

* [https://ui.adsabs.harvard.edu/abs/1964ApJ...140..552J/abstract R. A. James (1964)], 140, 552
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<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>
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===Differential Rotation===

* [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''
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<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>
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* [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