Clearing residual planetesimals by sweeping secular resonances in transitional disks: a lone-planet scenario for the wide gaps in debris disks around Vega and Fomalhaut

Abstract

Extended gaps in the debris disks of both Vega and Fomalhaut have been observed. These structures have been attributed to tidal perturbations by multiple super-Jupiter gas giant planets. Within the current observational limits, however, no such massive planets have been detected. Here we propose a less stringent `lone-planet' scenario to account for the observed structure with a single eccentric gas giant and suggest that clearing of these wide gaps is induced by its sweeping secular resonance. During the depletion of the disk gas, the planet's secular resonance propagates inward and clears a wide gap over an extended region of the disk. Although some residual intermediate-size planetesimals may remain in the gap, their surface density is too low to either produce super-Earths or lead to sufficiently frequent disruptive collisions to generate any observable dusty signatures. The main advantage of this lone-planet sweeping-secular-resonance model over the previous multiple gas giant tidal truncation scenario is the relaxed requirement on the number of gas giants. The observationally inferred upper mass limit can also be satisfied provided the hypothetical planet has a significant eccentricity. A significant fraction of solar or more massive stars bear gas giant planets with significant eccentricities. If these planets acquired their present-day kinematic properties prior to the depletion of their natal disks, their sweeping secular resonance would effectively impede the retention of neighboring planets and planetesimals over a wide range of orbital semi-major axes.

arXiv comment20 pages, 12 figures. Accepted for publication in ApJ

References in corpus (31)

• Direct Imaging of Multiple Planets Orbiting the Star HR 8799
• Angular Differential Imaging: a Powerful High-Contrast Imaging Technique
• Images of a fourth planet orbiting HR 8799
• Optical Images of an Exosolar Planet 25 Light Years from Earth
• Origin of the Structure of the Kuiper Belt during a Dynamical Instability in the Orbits of Uranus and Neptune
• Dust Filtration by Planet-Induced Gap Edges: Implications for Transitional Disks
• Transitional and Pre-Transitional disks: Gap Opening by Multiple Planets?
• The Debris Disk Around HR 8799
• Fomalhaut's Debris Disk and Planet: Constraining the Mass of Fomalhaut b From Disk Morphology
• Asteroid Belts in Debris Disk Twins: VEGA and FOMALHAUT
• Constructing the secular architecture of the solar system II: The terrestrial planets
• Epsilon Eridani's Planetary Debris Disk: Structure and Dynamics based on Spitzer and CSO Observations
• Constraining the Planetary System of Fomalhaut Using High-Resolution ALMA Observations
• Herschel imaging of 61 Vir: implications for the prevalence of debris in low-mass planetary systems
• Confirmation of the planet around HD 95086 by direct imaging
• On the Migration of Jupiter and Saturn: Constraints from Linear Models of Secular Resonant Coupling with the Terrestrial Planets
• Infrared Non-detection of Fomalhaut b -- Implications for the Planet Interpretation
• Synthesizing Exoplanet Demographics: A Single Population of Long-Period Planetary Companions to M Dwarfs Consistent with Microlensing, Radial Velocity, and Direct Imaging Surveys
• Dynamical Shakeup of Planetary Systems II. N-body simulations of Solar System terrestrial planet formation induced by secular resonance sweeping
• Planetary chaotic zone clearing: destinations and timescales
• Debris Distribution in HD 95086 - A Young Analog of HR 8799
• Eccentricity Evolution of Extrasolar Multiple Planetary Systems due to the Depletion of Nascent Protostellar Disks
• Belt(s) of debris resolved around the Sco-Cen star HIP 67497
• Fomalhaut b as a Dust Cloud: Frequent Collisions within the Fomalhaut Disk
• Constraints on the architecture of the HD 95086 planetary system with the Gemini Planet Imager
• Deep L' and M-band Imaging for Planets Around Vega and epsilon Eridani
• Terrestrial planet formation: Dynamical shake-up and the low mass of Mars
• The Inner 25 AU Debris Distribution in the epsilon Eri System
• Planetesimal clearing and size-dependent asteroid retention by secular resonance sweeping during the depletion of the solar nebula
• MMT/AO 5 micron Imaging Constraints on the Existence of Giant Planets Orbiting Fomalhaut at ~13-40 AU
• The formation of an eccentric gap in a gas disk by a planet in an eccentric orbit

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• Empty gaps? Depleting annular regions in debris discs by secular resonance with a two-planet system
• Secular transport during disk dispersal: the case of Kepler-419
• The influence of the secular perturbation of an intermediate-mass companion: I. Eccentricity excitation of disk stars at the Galactic center
• The ALMA survey to Resolve exoKuiper belt Substructures (ARKS) II. The radial structure of debris discs
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• Limits on the presence of planets in systems with debris disks: HD 92945 and HD 107146
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