更陡峭的散射盘屈曲得更快
Steeper Scattered Disks Buckle Faster
AI总结：
研究低质量天体散射盘的屈曲不稳定性，发现径向面密度越中心密集，屈曲时标越短；考虑巨行星的差分近点进动，海王星外原始散射盘在约10倍地球质量下即可不稳定。
摘要：
被巨行星散射至大半长轴和恒定近点幅角轨道的低质量天体盘容易发生屈曲不稳定性。这种不稳定性使轨道倾角呈指数增长，增大近点距，并使轨道发生相干倾斜，从而导致近点幅角的聚集。随后，这个动力学热系统容易形成偏侧模式。在此我们表明，随着群体径向面密度变得更加中心密集，屈曲不稳定性的时标会减小，即更陡峭的散射盘屈曲得更快。考虑到巨行星驱动的差分近点进动，我们发现如果 $dN \propto a^{-2.5} da$，那么对于海王星外区域的原始散射盘，约 $\sim\\!10\\,M_\oplus$ 就足以使其变得不稳定。
英文摘要：
Disks of low-mass bodies scattered by giant planets to large semi-major axis and constant periapsis orbits are vulnerable to a buckling instability. This instability exponentially grows orbital inclinations, raises periapsis distances, and coherently tilts orbits resulting in clustering of arguments of periapsis. The dynamically hot system is then susceptible to the formation of a lopsided mode. Here we show that the timescale of the buckling instability decreases as the radial surface density of the population becomes more centrally dense, i.e., steeper scattered disks buckle faster. Accounting for differential apsidal precession driven by giant planets, we find that $\sim\!10\,M_\oplus$ is sufficient for a primordial scattered disk in the trans-Neptunian region to have been unstable if $dN \propto a^{-2.5} da$.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
