Effects of a planetesimal debris disk on stability scenarios for the extrasolar planetary system HR 8799

Abstract

HR 8799 is a four planet system that also hosts a debris disk. By numerically integrating both planets and a planetesimal disk, we find interactions between an exterior planetesimal disk and the planets can influence the lifetime of the system. We first consider resonant planetary configurations that remained stable for at least 7 Myrs sans debris disk. An exterior debris disk with only 1 per cent the mass of the outermost planet (approximately a Neptune mass) was sufficiently large enough to pull the system out of resonance after 2 to 6 Myrs. Secondly, we consider configurations which are unstable in less than a few hundred thousand years. We find that these can be stabilized by a debris disk with a mass of more than 10 per cent that of the outermost planet. Our two sets of simulations suggest that estimates of the long term stability of a planetary system should take into account the role of the debris disk.

11 pages, 5 figures

References in corpus (3)

• Direct Imaging of Multiple Planets Orbiting the Star HR 8799
• Debris Disk Evolution Around A Stars
• From mean-motion resonances to scattered planets: Producing the Solar System, eccentric exoplanets and Late Heavy Bombardments

Cited by in corpus (15)

• Debris Disks: Structure, Composition, and Variability
• Atmospheric Retrieval Analysis of the Directly Imaged Exoplanet HR 8799b
• Multiple mean motion resonances in the HR 8799 planetary system
• The effects of external planets on inner systems: multiplicities, inclinations, and pathways to eccentric warm Jupiters
• Stirring in massive, young debris discs from spatially resolved Herschel images
• Debris Distribution in HD 95086 - A Young Analog of HR 8799
• A resolved debris disk around the candidate planet-hosting star HD95086
• Limits on orbit crossing planetesimals in the resonant multiple planet system, KOI-730
• The Debris Disk of Solar Analogue $\tau$ Ceti: Herschel Observations and Dynamical Simulations of the Proposed Multiplanet System
• Stability and Occurrence Rate Constraints on the Planetary Sculpting Hypothesis for "Transitional" Disks
• Orbital Stability of Multi-Planet Systems: Behavior at High Masses
• Long-term stability of the HR 8799 planetary system without resonant lock
• The post-main-sequence fate of the HR 8799 planetary system
• Gap Formation in Planetesimal Disks Via Divergently Migrating Planets
• 94 Ceti: a triple star with a planet and dust disc