Binary asteroid population 1. Angular momentum content
Binary asteroid population 1. Angular momentum content
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DOI：
10.1016/j.icarus.2007.02.023
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发表时间：
2007-09
期刊：
影响因子：
3.2
通讯作者：
P. Pravec;A. Harris
中科院分区：
文献类型：
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作者：
P. Pravec;A. Harris
我们编制了一个列表的估计参数的小行星从近地特洛伊轨道之间的二元系统。在本文中，我们描述了建设的名单，我们目前的研究结果的角动量含量在二元小行星。在近地小行星、穿越火星的小行星和主带小行星中，主直径小于或等于10公里的近距离双星系统是最多的。它们的总角动量非常接近，但一般不会超过，在重力状态下的单个物体的临界极限。这表明它们是由以临界速率旋转的母体（在大小范围内的小行星的重力旋转极限）通过某种裂变或质量脱落形成的。Yarkovsky-O 'Keefe-Radzievskii-Paddack（YORP）效应是上旋不稳定性的主要来源。在接近类地行星的过程中，引力相互作用不可能是双星形成的主要机制，但它可能会影响双星中NEA部分的性质。
We compiled a list of estimated parameters of binary systems among asteroids from near-Earth to trojan orbits. In this paper, we describe the construction of the list, and we present results of our study of angular momentum content in binary asteroids. The most abundant binary population is that of close binary systems among near-Earth, Mars-crossing, and main belt asteroids that have a primary diameter of about 10 km or smaller. They have a total angular momentum very close to, but not generally exceeding, the critical limit for a single body in a gravity regime. This suggests that they formed from parent bodies spinning at the critical rate (at the gravity spin limit for asteroids in the size range) by some sort of fission or mass shedding. The Yarkovsky–O'Keefe–Radzievskii–Paddack (YORP) effect is a candidate to be the dominant source of spin-up to instability. Gravitational interactions during close approaches to the terrestrial planets cannot be a primary mechanism of formation of the binaries, but it may affect properties of the NEA part of the binary population.