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

Moore, Alexander; Quillen, Alice C.

doi:10.1093/mnras/sts625

Cited by 37 publications

(22 citation statements)

References 40 publications

(91 reference statements)

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“…Examining stability as a function of period ratio is also useful for identifying special locations where individual resonances come in to play. Due to the large scatter in stability timescales, detailed, system-specific dynamical modeling for high mass, multi-planet systems may often be necessary, particularly to assess stability in non-planar, resonant configurations such as in the case of the four planet system HR 8799 (Fabrycky & Murray-Clay 2010;Moore & Quillen 2013;Goździewski & Migaszewski 2014;Pueyo et al 2015).…”

Section: Discussionmentioning

confidence: 99%

Orbital Stability of Multi-Planet Systems: Behavior at High Masses

Morrison

Kratter

2016

ApJ

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In the coming years, high-contrast imaging surveys are expected to reveal the characteristics of the population of wide-orbit, massive, exoplanets. To date, a handful of wide planetary mass companions are known, but only one such multi-planet system has been discovered: HR 8799. For low mass planetary systems, multi-planet interactions play an important role in setting system architecture. In this paper, we explore the stability of these high mass, multi-planet systems. While empirical relationships exist that predict how system stability scales with planet spacing at low masses, we show that extrapolating to super-Jupiter masses can lead to up to an order of magnitude overestimate of stability for massive, tightly packed systems. We show that at both low and high planet masses, overlapping mean-motion resonances trigger chaotic orbital evolution, which leads to system instability. We attribute some of the difference in behavior as a function of mass to the increasing importance of second order resonances at high planet-star mass ratios. We use our tailored high mass planet results to estimate the maximum number of planets that might reside in double component debris disk systems, whose gaps may indicate the presence of massive bodies.

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Section: Discussionmentioning

confidence: 99%

Orbital Stability of Multi-Planet Systems: Behavior at High Masses

Morrison

Kratter

2016

ApJ

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“…The relationship has also been evaluated for different timescales and outcomes and extended into the brown dwarf regime . Planets and disks can interact in even more complex ways, and the long-term stability of the planetary system may depend on the underlying mass of the planetesimal disk producing the debris (Moore & Quillen 2013). The HR 8799 system is often considered to be a scaled-up Solar System analog, since it contains four giant planets orbiting between two debris belts, similar to the architecture of the outer Solar System although with larger radii and masses (e.g., Su et al 2009).…”

Section: Direct Observations Of Planet-disk Interactionmentioning

confidence: 99%

Debris Disks: Structure, Composition, and Variability

Hughes

Duchêne

Matthews

2018

Annu. Rev. Astron. Astrophys.

296

327

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Debris disks are tenuous, dust-dominated disks commonly observed around stars over a wide range of ages. Those around main sequence stars are analogous to the Solar System's Kuiper Belt and Zodiacal light. The dust in debris disks is believed to be continuously regenerated, originating primarily with collisions of planetesimals. Observations of debris disks provide insight into the evolution of planetary systems; the composition of dust, comets, and planetesimals outside the Solar System; as well as placing constraints on the orbital architecture and potentially the masses of exoplanets that are not otherwise detectable. This review highlights recent advances in multiwavelength, high-resolution scattered light and thermal imaging that have revealed a complex and intricate diversity of structures in debris disks, and discusses how modeling methods are evolving with the breadth and depth of the available observations. Two rapidly advancing subfields highlighted in this review include observations of atomic and molecular gas around main sequence stars, and variations in emission from debris disks on very short (days to years) timescales, providing evidence of non-steady state collisional evolution particularly in young debris disks.

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“…These resonant configurations are characterised by smallamplitude librations of one or more resonant arguments corresponding to two-, three-, or four-planet mean motion resonances, thus ensuring that systems remain protected for extended periods from close encounters between the planets. Moore & Quillen (2013) find stabilising effects from the outer debris disk, although this requires a very massive debris disk. In this paper we show simulations of planetary systems that look like the HR 8799 system, are stable for longer than the estimated age, and are not stabilised by strong resonant lock.…”

Section: Introductionmentioning

confidence: 96%

Long-term stability of the HR 8799 planetary system without resonant lock

Götberg

Davies

Mustill

et al. 2016

A&A

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HR 8799 is a star accompanied by four massive planets on wide orbits. The observed planetary configuration has been shown to be unstable on a timescale much shorter than the estimated age of the system (∼30 Myr) unless the planets are locked into mean motion resonances. This condition is characterised by small-amplitude libration of one or more resonant angles that stabilise the system by preventing close encounters. We simulate planetary systems similar to the HR 8799 planetary system, exploring the parameter space in separation between the orbits, planetary masses and distance from the Sun to the star. We find systems that look like HR 8799 and remain stable for longer than the estimated age of HR 8799. None of our systems are forced into resonances. We find, with nominal masses (M b = 5 M Jup and M c,d,e = 7 M Jup ) and in a narrow range of orbit separations, that 5 of 100 systems match the observations and lifetime. Considering a broad range of orbit separations, we find 12 of 900 similar systems. The systems survive significantly longer because of their slightly increased initial orbit separations compared to assuming circular orbits from the observed positions. A small increase in separation leads to a significant increase in survival time. The low eccentricity the orbits develop from gravitational interaction is enough for the planets to match the observations. With lower masses, but still comfortably within the estimated planet mass uncertainty, we find 18 of 100 matching and long-lived systems in a narrow orbital separation range. In the broad separation range, we find 82 of 900 matching systems. Our results imply that the planets in the HR 8799 system do not have to be in strong mean motion resonances. We also investigate the future of wide-orbit planetary systems using our HR 8799 analogues. We find that 80% of the systems have two planets left after strong planet-planet scattering and these are on eccentric orbits with semi-major axes of a 1 ∼ 10 AU and a 2 ∼ 30−1000 AU. We speculate that other wide-orbit planetary systems, such as AB Pic and HD 106906, are the remnants of HR 8799 analogues that underwent close encounters and dynamical instability.

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

Cited by 37 publications

References 40 publications

Orbital Stability of Multi-Planet Systems: Behavior at High Masses

Orbital Stability of Multi-Planet Systems: Behavior at High Masses

Debris Disks: Structure, Composition, and Variability

Long-term stability of the HR 8799 planetary system without resonant lock

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