The surfaces of many white dwarfs are polluted by metals, implying a recent accretion event. The tidal disruption of planetesimals is a viable source of white dwarf pollution and offers a unique window into the composition of exoplanet systems. The question of how planetary material enters the tidal disruption radius of the white dwarf is currently unresolved. Using a series of N-body simulations, we explore the response of the surrounding planetesimal debris disk as the white dwarf receives a natal kick caused by anisotropic mass loss on the asymptotic giant branch. We find that the kick can form an apse-aligned, eccentric debris disk in the range 30–240 au, which corresponds to the orbits of Neptune, the Kuiper Belt, and the scattered disk in our solar system. In addition, many planetesimals beyond 240 au flip to counterrotating orbits. Assuming an isotropic distribution of kicks, we predict that approximately 80% of white dwarf debris disks should exhibit significant apsidal alignment and a fraction of counterrotating orbits. The eccentric disk is able to efficiently and continuously torque planetesimals onto radial, star-grazing orbits. We show that the kick causes both an initial burst in tidal disruption events as well as an extended period of 100 Myr where tidal disruption rates are consistent with observed mass accretion rates on polluted white dwarfs.

中文翻译：

---

白矮星本命踢后偏心碎片盘对小行星的潮汐破坏

许多白矮星的表面都被金属污染，这意味着最近发生了吸积事件。星子的潮汐破坏是白矮星污染的一个可行来源，并为了解系外行星系统的组成提供了一个独特的窗口。行星物质如何进入白矮星潮汐扰动半径的问题目前尚未解决。使用一系列氮在体模拟中，我们探索了当白矮星受到渐近巨星分支上各向异性质量损失引起的出生踢时，周围星子碎片盘的反应。我们发现，踢动可以在 30-240 天文单位范围内形成后殿对齐的偏心碎片盘，这对应于海王星、柯伊伯带和太阳系中的散射盘的轨道。此外，许多超过 240 个天文单位的星子会翻转到反向旋转轨道。假设踢动呈各向同性分布，我们预测大约 80% 的白矮星碎片盘应表现出明显的近轴排列和一小部分反向旋转轨道。偏心盘能够高效、连续地将星子扭转到径向掠星轨道上。我们表明，冲击会导致潮汐破坏事件的最初爆发以及长达 100 Myr 的延长期，其中潮汐破坏率与观测到的受污染白矮星的质量吸积率一致。