旋转玻色星的不稳定性
Instability of rotating Bose stars
摘要：
轻玻色子（类轴子）暗物质可能形成玻色星--由自引力支撑的非相对论性玻色-爱因斯坦凝聚体。我们研究由角动量非零的凝聚粒子组成的旋转玻色星$l$。我们分析证明，这些对象是不稳定的任意$l \ne 0$，如果粒子的自相互作用是有吸引力的或可忽略不计的小。它们通过脱落粒子并将角动量传输到系统的外围而衰减，直到出现类似土星的配置：一个（或几个）自旋为零的玻色星和弥散粒子云围绕共同的中心轨道运行。在没有自相互作用的情况下，我们计算的配置文件和主导的不稳定模式的旋转恒星：数值在$1 \leq l\leq 15$和解析在$l\gg 1$。值得注意的是，它们的寿命总是与反向结合能相当;因此，这些物体不能被认为是长寿的。最后，我们用数值方法证明了在具有足够强的排斥自相互作用的模型中，具有$l=1$的玻色星是稳定的。
英文摘要：
Light bosonic (axion-like) dark matter may form Bose stars - clumps of nonrelativistic Bose-Einstein condensate supported by self-gravity. We study rotating Bose stars composed of condensed particles with nonzero angular momentum $l$. We analytically prove that these objects are unstable at arbitrary $l \ne 0$ if particle self-interactions are attractive or negligibly small. They decay by shedding off the particles and transporting the angular momentum to the periphery of the system until a Saturn-like configuration appears: one (or several) spin-zero Bose stars and clouds of diffuse particles orbit around the mutual center. In the case of no self-interactions we calculate the profiles and dominant instability modes of the rotating stars: numerically at $1 \leq l\leq 15$ and analytically at $l\gg 1$. Notably, their lifetimes are always comparable to the inverse binding energies; hence, these objects cannot be considered long-living. Finally, we numerically show that in models with sufficiently strong repulsive self-interactions the Bose star with $l=1$ is stable.
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