双星小行星的角动量：对它们可能起源的启示
Angular Momemtum of Binary Asteroids: Implication for their possible origin
摘要：
在这项工作中，我们描述了对广泛观测的主带和特洛伊双星的物理和轨道特征的深入研究，主要来自LAOSA（大型小行星自适应光学调查，Marchis等人，2006 c）数据库，以及分叉对象的选择。计算和讨论了每个系统的无自旋量，如比角动量和主自旋速率。他们认为，这些小行星系统可能是旋转裂变或质量脱落的结果，可能受到外部扭矩的母体。由一个大的主星（Rp > 100 km）和一个小得多的副星（Rs < 20 km）组成的分离双星最显著的特征之一是它们的总角动量都是0.27。这个值非常接近旋转流体的麦克劳林-雅可比分叉（0.308）。另外，由相似大小的组件组成的接触双星和潮汐锁定双小行星的角动量大于0.48。它们成功地与旋转流体质量的裂变平衡序列进行了比较。总之，我们发现，总角动量是一个有用的代理，以评估这种系统的内部结构。
英文摘要：
We describe in this work a thorough study of the physical and orbital characteristics of extensively observed main-belt and Trojan binaries, mainly taken from the LAOSA (Large Adaptive Optics Survey of Asteroids, Marchis et al., 2006c) database, along with a selection of bifurcated objects. Dimensionless quantities, such as the specific angular momentum and the primary spin rate, are computed and discussed for each system. They suggest that these asteroidal systems might be the outcome of rotational fission or mass shedding of a parent body presumably subjected to an external torque. One of the most striking features of separated binaries composed of a large primary (Rp > 100 km) with a much smaller secondary (Rs < 20 km) is that they all have total angular momentum of 0.27. This value is quite close to the Maclaurin-Jacobi bifurcation (0.308) of a spinning fluid body. Alternatively, contact binaries and tidally locked double asteroids, made of components of similar size, have an angular momentum larger than 0.48. They compare successfully with the fission equilibrium sequence of a rotating fluid mass. In conclusion, we find that total angular momentum is a useful proxy to assess internal structure of such systems.
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