摘要：Observations of Kuiper Belt objects (KBOs) in Neptune’s 5:2 resonance present two puzzles: this third-order resonance hosts a surprisingly large population, comparable to the prominent populations of Plutinos and Twotinos in the first order 3:2 and 2:1 resonances, respectively; second, their eccentricities are concentrated near 0.4. To shed light on these puzzles, we investigate the phase space near this resonance with use of Poincaré sections of the circular planar restricted three-body model. We find several transitions in the phase space structure with increasing eccentricity, which we explain with the properties of the resonant orbit relative to Neptune’s. The resonance width is narrow for very small eccentricities but widens dramatically for e 0.2, reaching a maximum near e≈0.4, where it is similar to the maximum widths of the 2:1 and 3:2 resonances. We confirm these results with N-body numerical simulations, including the effects of all four giant planets and a wide range of orbital inclinations of the KBOs. We find that the boundaries of the stable resonance zone are not strongly sensitive to inclination and remain very similar to those found with the simplified three-body model, with the caveat that orbits of eccentricity above ∼0.53 are unstable; higher-eccentricity orbits are phase-protected from destabilizing encounters with Neptune but not with Uranus. These results show that the 5:2 resonant KBOs are not more puzzling than the Plutinos and Twotinos; however, detailed understanding of the origins of eccentric, inclined resonant KBOs remains a challenge.
关键词：Kuiper belt: general;Kuiper belt objects: individual (2013 UR15);planets and satellites: dynamical evolution and stability;planets and satellites: formation
