A new scenario for the origin of the 3/2 resonant system HD 45364

Correa-Otto, J. A.; Michtchenko, T. A.; Beaugé, C.

doi:10.1051/0004-6361/201321917

Cited by 10 publications

(10 citation statements)

References 46 publications

(106 reference statements)

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“…For the origin of the HD 200964 system, we considered the scenario of formation of close planetary systems developed in Correa-Otto et al (2013). This formation model was chosen after the detailed investigation of the planetary dynamics in the neighborhood of the 4/3 MMR.…”

Section: Discussionmentioning

confidence: 99%

“…From these, the second-order 5/3 MMR is also sufficiently strong to capture the system during slow migration. It should be emphasized that resonant captures are fairly robust when a slow type II migration is considered (see Emelýanenko 2012;Correa-Otto et al 2013, among others).…”

Section: Dynamical Map Of the Region Between The 2/1 And 4/3 Resonancesmentioning

confidence: 99%

“…As the migration is slow, the evolution of the eccentricities (bottom-left panel) closely follows the family of stationary solutions of the conservative 4/3 resonant problem, the ACR family Michtchenko et al 2006). The different rates of the mass accretion, when the inner planet grows more rapidly, are responsible for the excitation and the continuous increase of the eccentricity of the less massive outer planet (see Correa-Otto et al 2013, for details). During the whole second stage the system remains inside the resonance, what is confirmed by the evolution of the characteristic angles σ 1 and ∆ (Fig.…”

Section: Stage Ii: Runaway Mass Growth and Type II Migrationmentioning

confidence: 99%

“…For instance, the scenario of formation of close planetary systems formed of two giants has been developed in Correa-Otto et al (2013). It includes an interaction between different planetary migration types (types I and II), planetary growth, and gap formation in the protoplanetary disk.…”

Section: Introductionmentioning

confidence: 99%

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

Santos

Correa-Otto

Michtchenko

et al. 2014

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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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Section: Discussionmentioning

confidence: 99%

Section: Dynamical Map Of the Region Between The 2/1 And 4/3 Resonancesmentioning

confidence: 99%

Section: Stage Ii: Runaway Mass Growth and Type II Migrationmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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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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“…(See eg. Ward 1997; Papaloizou and Terquem 2006;Correa-Otto et al 2013;Baruteau et al 2014). While the orbital circularization of low mass protoplanets may be robustly estimated from a linear response calculation (see Sect.…”

Section: Orbital Migration and Circularization Due To Tidal Interactimentioning

confidence: 99%

Consequences of tidal interaction between disks and orbiting protoplanets for the evolution of multi-planet systems with architecture resembling that of Kepler 444

Papaloizou

2016

Celest Mech Dyn Astr

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We study orbital evolution of multi-planet systems with masses in the terrestrial planet regime induced through tidal interaction with a protoplanetary disk assuming that this is the dominant mechanism for producing orbital migration and circularization. We develop a simple analytic model for a system that maintains consecutive pairs in resonance while undergoing orbital circularization and migration. This model enables migration times for each planet to be estimated once planet masses, circularization times and the migration time for the innermost planet are specified. We applied it to a system with the current architecture of Kepler 444 adopting a simple protoplanetary disk model and planet masses that yield migration times inversely proportional to the planet mass, as expected if they result from torques due to tidal interaction with the protoplanetary disk. Furthermore the evolution time for the system as a whole is comparable to current protoplanetary disk lifetimes. In addition we have performed a number of numerical simulations with input data obtained from this model. These indicate that although the analytic model is inexact, relatively small corrections to the estimated migration rates yield systems for which period ratios vary by a minimal extent. Because of relatively large deviations from exact resonance in the observed system of up to 2 %, the migration times obtained in this way indicate only weak convergent migration such that a system for which the planets did not interact would contract by only ∼1 % although undergoing significant inward migration as a whole. We have also performed additional simulations to investigate conditions under which the system could undergo significant convergent migration before reaching its final state. These indicate that migration times have to be significantly shorter and resonances between planet pairs significantly closer during such an evolutionary phase. Relative migration rates would then have to decrease allowing period ratios to increase to become more distant from resonances as the system approached its final state in the inner regions of the protoplanetary disk.

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Vertical instability and inclination excitation during planetary migration

Voyatzis

Antoniadou

Tsiganis

2014

Celest Mech Dyn Astr

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We consider a two-planet system, which migrates under the influence of dissipative forces that mimic the effects of gas-driven (Type II) migration. It has been shown that, in the planar case, migration leads to resonant capture after an evolution that forces the system to follow families of periodic orbits. Starting with planets that differ slightly from a coplanar configuration, capture can, also, occur and, additionally, excitation of planetary inclinations has been observed in some cases. We show that excitation of inclinations occurs, when the planar families of periodic orbits, which are followed during the initial stages of planetary migration, become vertically unstable. At these points, vertical critical orbits may give rise to generating stable families of 3D periodic orbits, which drive the evolution of the migrating planets to non-coplanar motion. We have computed and present here the vertical critical orbits of the 2/1 and 3/1 resonances, for various values of the planetary mass ratio. Moreover, we determine the limiting values of eccentricity for which the "inclination resonance" occurs.

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A new scenario for the origin of the 3/2 resonant system HD 45364

Cited by 10 publications

References 46 publications

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

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

Consequences of tidal interaction between disks and orbiting protoplanets for the evolution of multi-planet systems with architecture resembling that of Kepler 444

Vertical instability and inclination excitation during planetary migration

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