A rotating star may be modeled as a continuous system of particles attracted to each other by gravity and with a given total mass and prescribed angular velocity. Mathematically this leads to the Euler–Poisson system. A white dwarf star is modeled by a very particular, and rather delicate, equation of state for the pressure as a function of the density. We prove an existence theorem for rapidly rotating white dwarfs that depend continuously on the speed of rotation. The key tool is global continuation theory, combined with a delicate limiting process. The solutions form a connected set ##IMG## [http://ej.iop.org/images/0951-7715/33/9/4783/nonab8d13ieqn1.gif] {$\mathcal{K}$} in an appropriate function space. As the speed of rotation increases, we prove that either the supports of white dwarfs in ##IMG## [http://ej.iop.org/images/0951-7715/33/9/4783/nonab8d13ieqn2.gif] {$\mathcal{K}$} become unbounded or their densities become unbounded....

中文翻译：

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快速旋转的白矮星

可以将旋转的恒星建模为由重力吸引并具有给定的总质量和规定的角速度的连续粒子系统。从数学上讲，这导致了欧拉-泊松系统。白矮星由压力的一个非常特殊且相当微妙的状态方程模拟，该状态方程是密度的函数。我们证明了快速旋转的白矮星的存在性定理，它连续地取决于旋转速度。关键工具是全局延续理论，并结合了精细的限制过程。解决方案在适当的情况下形成一个连接集## IMG ## [http://ej.iop.org/images/0951-7715/33/9/4783/nonab8d13ieqn1.gif] {$ \ mathcal {K} $}功能空间。随着旋转速度的提高，我们证明了## IMG ## [http://ej.iop.com中的白矮星的支持。