Hektor -木星特洛伊人中的一个特殊的D型家族
Hektor - an exceptional D-type family among Jovian Trojans
摘要：
在这项工作中，我们分析木星特洛伊木马在合适的共振元素的空间，我们确定集群的可能碰撞起源的两个独立的方法：层次聚类和所谓的“随机盒”。与我们以前的工作（Brodegan和Rozehnal 2011）相比，我们研究了两倍大的样本。除了Eurybates、Ennomos和$1996\,\rm RJ$族外，我们还发现了另外三个星团-即围绕小行星的（20961）~Arkesilaos、$L_4$天平动带中的（624）~Hektor和$L_5$中的（247341）~ $2001\,\rm UV_{209}$。这些家系符合我们严格的标准，即高统计学显著性、高同质性和比背景更陡的大小-频率分布。为了理解它们的性质，我们用Boulder代码（Morbidelli et al. 2009）模拟了它们的长期碰撞演化，并用修改后的SWIFT积分器（Levison and Duncan，1994）模拟了它们的动力学演化。在我们的进化模型的框架内，我们能够将Hektor家族的年龄限制在1至4 Gyr，或者不太可能，0.1至2.5 Gyr，这取决于最初的影响几何形状。由于（624）Hektor本身似乎是一个带有卫星的双叶形天体（Marchis等人，2014年），即一个例外的天体，我们讨论了它与D型家族的关联，并证明了月球和家族可以在一次撞击事件中产生。我们用光滑粒子流体动力学（SPH，Benz和Asphaug，1994）模拟了撞击坑事件。这也是第一例与D型母体相关的族。
英文摘要：
In this work, we analyze Jovian Trojans in the space of suitable resonant elements and we identify clusters of possible collisional origin by two independent methods: the hierarchical clustering and a so-called "randombox". Compared to our previous work (Brož and Rozehnal 2011), we study a twice larger sample. Apart from Eurybates, Ennomos and $1996\,\rm RJ$ families, we have found three more clusters --- namely families around asteroids (20961)~Arkesilaos, (624)~Hektor in the $L_4$ libration zone and (247341)~$2001\,\rm UV_{209}$ in $L_5$. The families fulfill our stringent criteria, i.e. a high statistical significance, an albedo homogeneity and a steeper size-frequency distribution than that of background. In order to understand their nature, we simulate their long term collisional evolution with the Boulder code (Morbidelli et al. 2009) and dynamical evolution using a modified SWIFT integrator (Levison and Duncan, 1994). Within the framework of our evolutionary model, we were able to constrain the the age of the Hektor family to be either 1 to 4 Gyr or, less likely, 0.1 to 2.5 Gyr, depending on initial impact geometry. Since (624) Hektor itself seems to be a bilobed--shape body with a satellite (Marchis et al. 2014), i.e. an exceptional object, we address its association with the D--type family and we demonstrate that the moon and family could be created during a single impact event. We simulated the cratering event using a Smoothed Particle Hydrodynamics (SPH, Benz and Asphaug, 1994). This is also the first case of a family associated with a D--type parent body.
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