论文标题
Gyr-Timesscale通过自旋破坏高分子小行星，以及为什么幸免于2006 HY51
Gyr-timescale destruction of high-eccentricity asteroids by spin and why 2006 HY51 has been spared
论文作者
论文摘要
小行星和其他小天体的形状明显明显，在高度偏心轨道触发的周围通道期间施加了扰动的三轴扭矩，并维持混乱的旋转状态。由于惯性主轴周围的旋转速率不是从上方界定的，因此它可以意外地达到与旋转分解相对应的阈值。由于动作的僵硬方程，对此过程的先前研究仅限于$ \ sim 10^3 $轨道的整合。我们在这里提出了一种快速的1D仿真方法，以计算$ \ sim 10^9 $ orbits的旋转速率的演变。我们将该方法应用于最古怪的太阳系小行星已知的2006 HY51（$ e = 0.9684 $），并发现对于任何合理的期望形状参数，它永远无法加速以分解速度。但是，在更多偏心轨道上的原始太阳系小行星可能已经从这种旋转裂变中分解了。该方法还代表了研究极其古怪的三轴exo-asteroids（$ e> 0.99 $）的长期演变的有前途的机会，这在白矮人行星系统中被认为很常见
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
