妊神星碰撞族的产生
The Creation of Haumea's Collisional Family
摘要：
最近，在柯伊伯带发现了第一个碰撞族。这个家庭的母体，Haumea，是柯伊伯带中最大的物体之一，由两颗卫星环绕。有人提出妊神星家族是由巨大撞击产生的分散碎片形成的。然而，这个提出的妊神星家族的起源与观测到的家族成员之间的速度分散（\sim 140 m/s）相矛盾，后者明显小于妊神星表面的逃逸速度（\sim 900 m/s）。在本文中，我们提出了一个不同的形成方案妊神星的碰撞家庭。在我们的场景中，家庭成员在围绕妊神星的轨道上被弹出。因此，这种情况下，自然会产生一个较低的速度分散之间的家庭成员比预期的直接喷射从妊神星的表面。在我们的场景中，妊神星的巨大撞击形成了一个单一的卫星，它潮汐式地向外演化，直到它遭受毁灭性的碰撞，从而创造了这个家族。我们表明，这种形成的情况下产生的速度分散\sim 190米/秒的家庭成员之间的观测结果是一致的。妊神星在今天的柯伊伯带发生初始大碰撞的概率小于10^{-3}。然而，在我们的设想中，妊神星的巨大撞击可能发生在柯伊伯带激发和家族成员弹射之前。这样做的好处是可以保持动力学的一致性，并解释妊神星最初的巨大撞击，这是几个数量级更有可能发生在原始的动力学冷柯伊伯带相比，动力学激发柯伊伯带今天。删节
英文摘要：
Recently, the first collisional family was discovered in the Kuiper belt. The parent body of this family, Haumea, is one of the largest objects in the Kuiper belt and is orbited by two satellites. It has been proposed that the Haumea family was created from dispersed fragments that resulted from a giant impact. This proposed origin of the Haumea family is however in conflict with the observed velocity dispersion between the family members (\sim 140 m/s) which is significantly less than the escape velocity from Haumea's surface (\sim 900 m/s). In this paper we propose a different formation scenario for Haumea's collisional family. In our scenario the family members are ejected while in orbit around Haumea. This scenario, therefore, gives naturally rise to a lower velocity dispersion among the family members than expected from direct ejection from Haumea's surface. In our scenario Haumea's giant impact forms a single moon that tidally evolves outward until it suffers a destructive collision from which the family is created. We show that this formation scenario yields a velocity dispersion of \sim 190m/s among the family members which is in good agreement with the observations. The probability for Haumea's initial giant impact in todays Kuiper belt is less than 10^{-3}. In our scenario, however, Haumea's giant impact can occur before the excitation of the Kuiper belt and the ejection of the family members afterwards. This has the advantage that one can preserve the dynamical coherence of the family and explain Haumea's original giant impact, which is several orders of magnitude more likely to have occurred in the primordial dynamically cold Kuiper belt compared to the dynamically excited Kuiper belt today. Abridged
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
