Traditional formation scenarios fail to explain 4:3 mean motion resonances

Rein, Hanno; Payne, Matthew J.; Veras, Dimitri

doi:10.1111/j.1365-2966.2012.21798.x

Cited by 51 publications

(40 citation statements)

References 67 publications

(94 reference statements)

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“…Emelyanenko 2012). In addition there are two known systems in 3:2 resonance , Rein et al 2012, Robertson et al 2012a) and one in a 4:3 resonance (Johnson et al 2011, Rein et al 2012 consistent with the systems in 2:1 resonance being the most commonly observed commensurability.…”

Section: Introductionmentioning

confidence: 91%

On the orbital evolution of a pair of giant planets in mean motion resonance

André

Papaloizou

2016

Mon. Not. R. Astron. Soc.

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Pairs of extrasolar giant planets in a mean motion commensurability are common with 2:1 resonance occurring most frequently. Disc-planet interaction provides a mechanism for their origin. However, the time scale on which this could operate in particular cases is unclear. We perform 2D and 3D numerical simulations of pairs of giant planets in a protoplanetary disc as they form and maintain a mean motion commensurability. We consider systems with current parameters similar to those of HD 155358, 24 Sextantis and HD 60532, and disc models of varying mass, decreasing mass corresponding to increasing age. For the lowest mass discs, systems with planets in the Jovian mass range migrate inwards maintaining a 2:1 commensurability. Systems with the inner planet currently at around 1 au from the central star could have originated at a few au and migrated inwards on a time scale comparable to protoplanetary disc lifetimes. Systems of larger mass planets such as HD 60532 attain 3:1 resonance as observed. For a given mass accretion rate, results are insensitive to the disc model for the range of viscosity prescriptions adopted, there being good agreement between 2D and 3D simulations. However, in a higher mass disc a pair of Jovian mass planets passes through 2:1 resonance before attaining a temporary phase lasting a few thousand orbits in an unstable 5:3 resonance prior to undergoing a scattering. Thus finding systems in this commensurability is unlikely.

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Section: Introductionmentioning

confidence: 91%

On the orbital evolution of a pair of giant planets in mean motion resonance

André

Papaloizou

2016

Mon. Not. R. Astron. Soc.

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“…The origin of the compact planetary configuration in the HD 200964 system was first investigated by Rein et al (2012). Various models for the formation of systems in the 4/3 MMR based on traditional type II migration scenarios or in situ formation of the planets were explored.…”

Section: Formation Scenario Of the Hd 200964 Systemmentioning

confidence: 99%

“…The issue was extensively explored in Rein et al (2012), where the model of formation of planetary pairs in the 4/3 MMR based on the traditional type II migration scenario was investigated. However, even employing non-conventional scenarios, such as formation in situ and planetary scattering, these attempts to simulate the formation of two giant planets in the stable 4/3 resonance configuration have failed.…”

Section: Introductionmentioning

confidence: 99%

Formation and evolution of the two 4/3 resonant giants planets in HD 200964

Santos

Correa-Otto

Michtchenko

et al. 2014

A&A

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Context. It has been suggested that HD 200964 is the first exoplanetary system with two Jovian planets evolving in the 4/3 meanmotion resonance (MMR). Previous scenarios to simulate the formation of two giant planets in the stable 4/3 resonance configuration have failed. Moreover, the orbital parameters available in the literature point out an unstable configuration of the planetary pair. Aims. The purpose of this paper is i) to determine the orbits of the planets from the radial velocity measurements and update the value of the stellar mass (1.57 M ); ii) to analyse the stability of the planetary evolution in the vicinity and inside the 4/3 MMR; and iii) to elaborate a possible scenario for the formation of systems in the 4/3 MMR. Methods. We use a previous model to simulate the formation of the stable planetary pair trapped inside the 4/3 resonance. Our scenario includes an interaction between the type I and type II of migration, planetary growth and stellar evolution from the main sequence to the sub-giant branch. The redetermination of the orbits is done using a biased Monte Carlo procedure, while the planetary dynamics is studied using numerical tools, such as dynamical maps and dynamical power spectra. Results. The results of the formation simulations are able to very closely reproduce the 4/3 resonant dynamics of the best-fit configuration obtained in this paper. Moreover, the confidence interval of the fit matches well with the very narrow stable region of the 4/3 MMR. Conclusions. The formation process of the HD 200964 system is very sensitive to the planetary masses and protoplanetary disk parameters. Only a thin, flat disk allows the embryo-sized planets to reach the 4/3 resonant configuration. The stable evolution of the resonant planets is also sensitive to the mass of the central star, because of overlapping high-order resonances inside the 4/3 resonance. Regardless of the very narrow domain of stable motion, the confidence interval of our fit closely matches the stability area.

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“…Convergent migration in protoplanetary discs is an effective and popular MMR formation mechanism (Snellgrove et al 2001), and can also achieve three-body resonances (Peale & Lee 2002;Libert & Tsiganis 2011), although some MMRs are harder to lock into than others (Rein et al 2012; Tadeu dos Santos et al 2015). Forming the 3:2 MMR in particular through energy dissipation has been widely investigated (Papaloizou & Szuszkiewicz 2005;Hadjidemetriou & Voyatzis 2010;Emel'yanenko 2012;Ogihara & Kobayashi 2013;Wang & Ji 2014;Zhang et al 2014).…”

Section: Introductionmentioning

confidence: 99%

One of the closest exoplanet pairs to the 3:2 mean motion resonance: K2-19b and c

Armstrong

Santerne

Veras

et al. 2015

A&A

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Aims. The K2 mission has recently begun to discover new and diverse planetary systems. In December 2014, Campaign 1 data from the mission was released, providing high-precision photometry for ∼22 000 objects over an 80-day timespan. We searched these data with the aim of detecting more important new objects. Methods. Our search through two separate pipelines led to the independent discovery of K2-19b and c, a two-planet system of Neptune-sized objects (4.2 and 7.2 R ⊕ ), orbiting a K dwarf extremely close to the 3:2 mean motion resonance. The two planets each show transits, sometimes simultaneously owing to their proximity to resonance and the alignment of conjunctions. Results. We obtained further ground-based photometry of the larger planet with the NITES telescope, demonstrating the presence of large transit timing variations (TTVs), and used the observed TTVs to place mass constraints on the transiting objects under the hypothesis that the objects are near but not in resonance. We then statistically validated the planets through the PASTIS tool, independently of the TTV analysis.

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Traditional formation scenarios fail to explain 4:3 mean motion resonances

Cited by 51 publications

References 67 publications

On the orbital evolution of a pair of giant planets in mean motion resonance

On the orbital evolution of a pair of giant planets in mean motion resonance

Formation and evolution of the two 4/3 resonant giants planets in HD 200964

One of the closest exoplanet pairs to the 3:2 mean motion resonance: K2-19b and c

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