Steeper Scattered Disks Buckle Faster

Abstract

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 $\sim 10M_{\oplus }$ is sufficient for a primordial scattered disk in the trans-Neptunian region to have been unstable if $dN\propto a^{-2.5}da$.

5 pages, 4 figures, accepted by ApJL

References in corpus (5)

• Consequences of a Distant Massive Planet on the Large Semi-major Axis Trans-Neptunian Objects
• Orbital clustering in the distant solar system
• A Rogue Planet Helps Populate the Distant Kuiper Belt
• Giant Planet Influence on the Collective Gravity of a Primordial Scattered Disk
• Apsidal Clustering following the Inclination Instability