高偏心率小行星因自旋造成的Gyr-timescale破坏和2006年HY51幸免的原因
Gyr-timescale destruction of high-eccentricity asteroids by spin and why 2006 HY51 has been spared
摘要：
小行星和其他小天体具有明显的扁长形状，在高度偏心轨道的近心通过期间施加的扰动三轴扭矩触发并维持混沌旋转状态。由于绕惯性主轴的自旋速率从上到下是不受限制的，因此它可能意外地达到对应于旋转破裂的阈值。由于运动方程的刚性，以前对这一过程的研究仅限于对$\sim 10^3$轨道的积分。我们在这里提出了一个快速的一维模拟方法来计算这个自旋率的演变$\sim 10^9$轨道。我们应用该方法的最偏心的太阳系小行星，2006年HY 51（与$e = 0.9684$），并发现，对于任何合理预期的形状参数，它永远不会被加速到解体的速度。然而，在更偏心轨道上的原始太阳系小行星可能已经从这种类型的旋转裂变中分裂出来。该方法也为研究极偏心三轴系外小行星（$e > 0.99$）的长期演化提供了一个很好的机会，这些小行星被认为是白矮星行星系中常见的
英文摘要：
Asteroids and other small celestial bodies have markedly prolate shapes, and the perturbative triaxial torques which are applied during pericenter passages in highly eccentric orbits trigger and sustain a state of chaotic rotation. Because the prograde spin rate around the principal axis of inertia is not bounded from above, it can accidentally reach the threshold value corresponding to rotational break-up. Previous investigations of this process were limited to integrations of $\sim 10^3$ orbits because of the stiff equation of motion. We present here a fast 1D simulation method to compute the evolution of this spin rate over $\sim 10^9$ orbits. We apply the method to the most eccentric solar system asteroid known, 2006 HY51 (with $e = 0.9684$), and find that for any reasonably expected shape parameters, it can never be accelerated to break-up speed. However, primordial solar system asteroids on more eccentric orbits may have already broken up from this type of rotational fission. The method also represents a promising opportunity to investigate the long-term evolution of extremely eccentric triaxial exo-asteroids ($e > 0.99$), which are thought to be common in white dwarf planetary systems
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