A Lopsided Outer Solar System
arXiv:2106.09739 · doi:10.3847/1538-3881/ac2def
Abstract
Axisymmetric disks of eccentric orbits in near-Keplerian potentials are unstable to an out-of-plane buckling. Recently, Zderic et al. (2020) showed that an idealized disk saturates to a lopsided mode. Here we show that this apsidal clustering also occurs in a primordial scattered disk in the outer solar system which includes the orbit-averaged gravitational influence of the giant planets. We explain the dynamics using Lynden-Bell (1979)'s mechanism for bar formation in galaxies. We also show surface density and line of sight velocity plots at different times during the instability, highlighting the formation of concentric circles and spiral arms in velocity space.
17 pages, 13 figures
References in corpus (13)
- The Planet Nine Hypothesis
- Resonant relaxation near a massive black hole: the dependence on eccentricity
- Discovery of A New Retrograde Trans-Neptunian Object: Hint of A Common Orbital Plane for Low Semi-Major Axis, High Inclination TNOs and Centaurs
- ALMA Detection of Extended Millimeter Halos in the HD 32297 and HD 61005 Debris Disks
- Observational bias and the clustering of distant eccentric Kuiper belt objects
- Consequences of a Distant Massive Planet on the Large Semi-major Axis Trans-Neptunian Objects
- Orbital clustering in the distant solar system
- OSSOS XV: Probing the Distant Solar System with Observed Scattering TNOs
- Outer Solar System Perihelion Gap Formation Through Interactions with a Hypothetical Distant Giant Planet
- Giant Planet Influence on the Collective Gravity of a Primordial Scattered Disk
- Apsidal Clustering following the Inclination Instability
- The Lynden-Bell bar formation mechanism in simple and realistic galactic models
- Interactions Among Non-Interacting Particles in Planet Formation Simulations