三轴恒星系统中径向轨道不稳定性的对应
A Counterpart to the Radial Orbit Instability in Triaxial Stellar Systems
摘要：
三轴质量模型的自洽解是高度非唯一的。一般来说，这些解中的一些可能是动态不稳定的，使得它们不适合作为稳态星系的描述。在这里，我们证明了第一次在三轴星系模型的不稳定性类似的径向轨道不稳定性的球形模型的存在。当主要是径向运动的盒子轨道的数量足够大时，不稳定性就会显现出来。N体模拟验证了演化既不是由于混沌轨道，也不是由于模型偏离自洽，而是由于集体模式。不稳定性将三轴模型转换成更长的，但仍然是三轴的，配置。当径向轨道的质量贡献减少时，得到稳定的三轴模型。我们的结果的形状的暗物质晕的影响进行了讨论。
英文摘要：
Self-consistent solutions for triaxial mass models are highly non-unique. In general, some of these solutions might be dynamically unstable, making them inappropriate as descriptions of steady-state galaxies. Here we demonstrate for the first time the existence in triaxial galaxy models of an instability similar to the radial-orbit instability of spherical models. The instability manifests itself when the number of box orbits, with predominantly radially motions, is sufficiently large. N-body simulations verify that the evolution is due neither to chaotic orbits nor to departures of the model from self-consistency, but rather to a collective mode. The instability transforms the triaxial model into a more prolate, but still triaxial, configuration. Stable triaxial models are obtained when the mass contribution of radial orbits is reduced. The implications of our results for the shapes of dark-matter halos are discussed.
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