Limits on orbit-crossing planetesimals in the resonant multiple planet system, KOI-730

Moore, Alexander; Hasan, Imran; Quillen, Alice C.

doi:10.1093/mnras/stt535

Cited by 39 publications

(15 citation statements)

References 33 publications

(66 reference statements)

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“…We solved it with the Migration Constrained Optimization Algorithm (MCOA), as dubbed earlier in (Goździewski & Migaszewski 2014). The MCOA makes use of a heuristic model of the planetary migration (Beaugé et al 2006;Moore et al 2013) and theoretical estimates of the planetary masses, consistent with the recent cooling theory (Marois et al 2010;Baines et al 2012;Marleau & Cumming 2014).…”

Section: The Migration Algorithm Revisitedmentioning

confidence: 99%

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The Orbital Architecture and Debris Disks of the HR 8799 Planetary System

Goździewski

Migaszewski

2018

ApJS

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The HR 8799 planetary system with four 10 m Jup planets in wide orbits up to 70 au, and orbital periods up to 500 yrs has been detected with the direct imaging. Its intriguing orbital architecture is not yet fully resolved due to time-limited astrometry covering only 20 years. Earlier, we constructed a heuristic model of the system based on rapid, convergent migration of the planets. Here we developed a better structured and CPU-efficient variant of this model. With the updated approach, we reanalyzed the self-consistent, homogeneous astrometric dataset in (Konopacky et al. 2016). The bestfitting configuration agrees with our earlier findings. The HR 8799 planets are likely involved in dynamically robust Laplace 8e:4d:2c:1b resonance chain. Hypothetical planets with masses below the current detection limit of 0.1-3 Jupiter masses, within the observed inner, or beyond the outer orbit, respectively, do not influence the long term stability of the system. We predict positions of such nondetected objects. The long-term stable orbital model of the observed planets helps to simulate the dynamical structure of debris disks in the system. A CPU-efficient fast indicator technique makes it possible to reveal their complex, resonant shape in 10 6 particles scale. We examine the inner edge of the outer disk detected between 90 and 145 au. We also reconstruct the outer disk assuming that it has been influenced by convergent migration of the planets. A complex shape of the disk strongly depends on various dynamical factors, like orbits and masses of non-detected planets. It may be highly non-circular and its models are yet non-unique, regarding both observational constraints, as well as its origin.

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Section: The Migration Algorithm Revisitedmentioning

confidence: 99%

“…The crucial point is that the planetary migration leads to the MMR capture, and establishes stable systems. In order to mimic the migration with the N -body code, we modify the astrocentric equations of motion with a force term (Papaloizou & Terquem 2006;Beaugé et al 2006;Moore et al 2013)…”

Section: A Set Of Mmr Captured Systemsmentioning

confidence: 99%

The Orbital Architecture and Debris Disks of the HR 8799 Planetary System

Goździewski

Migaszewski

2018

ApJS

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“…A further question is which role the debris disc may have played in the evolution of the system. It might have circularised the orbits of scattered planets or facilitated migration (Moore et al 2013).…”

Section: Introductionmentioning

confidence: 99%

The scattered disc of HR 8799

Geiler

Krivov

Booth

et al. 2018

Monthly Notices of the Royal Astronomical Society

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HR 8799 is a young F0-type star with four directly imaged giant planets and two debris belts, one located exterior and another one interior to the region occupied by the planetary orbits. Having an architecture similar to that of our Solar System, but also revealing dissimilarities such as high masses of planets, a huge radial extent and a high mass of the outer debris belt, HR 8799 is considered to be a benchmark to test formation and evolution models of planetary systems. Here we focus on the outer debris ring and its relation to the planets. We demonstrate that the models of the outer disc, proposed previously to reproduce Herschel observations, are inconsistent with the ALMA data, and vice versa. In an attempt to find a physically motivated model that would agree with both observational sets, we perform collisional simulations. We show that a narrow planetesimal belt and a radiation pressure induced dust halo cannot account for the observed radial brightness profiles. A single, wide planetesimal disc does not reproduce the data either. Instead, we propose a two-population model, comprising a Kuiper-Belt-like structure of a low-eccentricity planetesimal population ("the classical Kuiper Belt") and a high-eccentricity population of comets ("scattered disc"). We argue that such a structure of the exo-Kuiper belt of HR 8799 could be explained with planet migration scenarios analogous to those proposed for the Kuiper Belt of the Solar System.

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“…To reproduce the observational Kepler-29 system, and its features discussed in Section 3, we conducted migration simulations within a simple parametric model of the force which mimics the planetdisc interactions (e.g., Beaugé et al 2006;Moore et al 2013) …”

Section: Planetary Migrationmentioning

confidence: 99%

The origin and 9:7 MMR dynamics of the Kepler-29 system

Migaszewski

Goździewski

Panichi

2016

Mon. Not. R. Astron. Soc.

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We analyse the Transit Timing Variation (TTV) measurements of a system of two super-Earths detected as Kepler-29, in order to constrain the planets' masses and orbital parameters. A dynamical analysis of the best-fitting configurations constrains the masses to be ∼ 6 and ∼ 5 Earth masses for the inner and the outer planets, respectively. The analysis also reveals that the system is likely locked in the 9:7 mean motion resonance. However, a variety of orbital architectures regarding eccentricities and the relative orientation of orbits is permitted by the observations as well as by stability constraints. We attempt to find configurations preferred by the planet formation scenarios as an additional, physical constraint. We show that configurations with low eccentricities and anti-aligned apsidal lines of the orbits are a natural and most likely outcome of the convergent migration. However, we show that librations of the critical angles are not necessary for the Kepler-29 system to be dynamically resonant, and such configurations may be formed on the way of migration as well. We argue, on the other hand, that aligned configurations with e 0.03 may be not consistent with the migration scenario.

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Limits on orbit-crossing planetesimals in the resonant multiple planet system, KOI-730

Cited by 39 publications

References 33 publications

The Orbital Architecture and Debris Disks of the HR 8799 Planetary System

The Orbital Architecture and Debris Disks of the HR 8799 Planetary System

The scattered disc of HR 8799

The origin and 9:7 MMR dynamics of the Kepler-29 system

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