Eccentricity Trap: Trapping of Resonantly Interacting Planets Near the Disk Inner Edge

Ogihara, Masahiro; Duncan, Martin J.; Ida, Shigeru

doi:10.1088/0004-637x/721/2/1184

Cited by 64 publications

(67 citation statements)

References 24 publications

(49 reference statements)

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“…2, the former can become positive owing to the corotation torque, which depends on the slope of the gas surface density. The latter is a torque recently found by Ogihara et al (2010). When a body with non-zero eccentricity straddles a sharp disk inner edge, the body gains a net positive torque from the disk depending on the sharpness of the edge and on the eccentricity.…”

Section: Orbital Evolutionmentioning

confidence: 72%

Formation of terrestrial planets in disks evolving via disk winds and implications for the origin of the solar system’s terrestrial planets

Ogihara

Kobayashi

Inutsuka

et al. 2015

A&A

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Context. Recent three-dimensional magnetohydrodynamical simulations have identified a disk wind by which gas materials are lost from the surface of a protoplanetary disk, which can significantly alter the evolution of the inner disk and the formation of terrestrial planets. A simultaneous description of the realistic evolution of the gaseous and solid components in a disk may provide a clue for solving the problem of the mass concentration of the terrestrial planets in the solar system. Aims. We simulate the formation of terrestrial planets from planetary embryos in a disk that evolves via magnetorotational instability and a disk wind. The aim is to examine the effects of a disk wind on the orbital evolution and final configuration of planetary systems. Methods. We perform N-body simulations of sixty 0.1 Earth-mass embryos in an evolving disk. The evolution of the gas surface density of the disk is tracked by solving a one-dimensional diffusion equation with a sink term that accounts for the disk wind. Results. We find that even in the case of a weak disk wind, the radial slope of the gas surface density of the inner disk becomes shallower, which slows or halts the Type I migration of embryos. If the effect of the disk wind is strong, the disk profile is significantly altered (e.g., positive surface density gradient, inside-out evacuation), leading to outward migration of embryos inside ∼1 AU. Conclusions. Disk winds play an essential role in terrestrial planet formation inside a few AU by changing the disk profile. In addition, embryos can undergo convergent migration to ∼1 AU in certainly probable conditions. In such a case, the characteristic features of the solar system's terrestrial planets (e.g., mass concentration around 1 AU, late giant impact) may be reproduced.

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Section: Orbital Evolutionmentioning

confidence: 72%

Formation of terrestrial planets in disks evolving via disk winds and implications for the origin of the solar system’s terrestrial planets

Ogihara

Kobayashi

Inutsuka

et al. 2015

A&A

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“…In the case of a smooth density profile (q ≈ 0), explicit expressions for the forces acting on the planetary masses can be found in Ogihara & Ida (2009) and Ogihara et al (2010), while the applications of the model can be found in Giuppone et al (2012). In our simulation, we assume a scale height h = H/r = 0.05 and a constant surface density profile Σ(r) = Σ 0 (r/1 AU) −q with q = 0 and Σ 0 = 300 g/cm 2 , which corresponds to two minimum mass solar nebula at 5 AU (MMSN, Hayashi 1981).…”

Section: Hd 200964 Star Mass Evaluationmentioning

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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“…It is worth mentioning that the model is valid only for low eccentricities (e < ∼ 0.05) and small planetary masses ( < ∼ 13 M ⊕ ). In the case of a smooth density profile, explicit expressions for the forces acting on the planetary masses can be found in Ogihara & Ida (2009) and Ogihara et al (2010), while model applications can be found in Giuppone et al (2012). In our simulation, we assumed a scale height h = H/r = 0.05 and a constant surface density profile Σ(r) = Σ 0 (r/1 AU) −q with q = 0 and Σ 0 = 150 g/cm 2 , which corresponds to the minimum mass solar nebula at 5 AU (MMSN, Hayashi 1981).…”

Section: Scenario 2 For the Origin Of The 3/2 Resonance For The Hd 45mentioning

confidence: 99%

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

Correa-Otto

Michtchenko

Beaugé

2013

A&A

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We revise the model for the origin of the HD 45364 exoplanetary system proposed by Rein et al. (2010, A&A, 510, A4), which is currently known to host two planets close to the 3/2 mean-motion resonance (MMR). We show that due to the high surface density of the protoplanetary disk needed for type III migration, this model can only lead to planets in a quasi-resonant regime of motion and thus is not consistent with the resonant configuration obtained by Correia et al. (2009, A&A, 496, 521). Although both resonant and quasi-resonant solutions are statistically indistinguishable with respect to radial velocity measurements, their distinct dynamical behavior is intriguing. We used the semi-analytical model to confirm the quantitative difference between two configurations. To form a system that evolves inside the 3/2 resonance, we developed a different model. Our scenario includes an interaction between different (but slower) planetary migration types, planet growth, and gap formation in the protoplanetary disk. The evolutionary path was chosen due to a detailed analysis of the phase space structure in the vicinity of the 3/2 MMR that employed dynamical mapping techniques. The outcomes of our simulations are able to very closely reproduce the 3/2 resonant dynamics obtained from the best fit presented by Correia et al. In addition, by varying the strength of the eccentricity damping, we can also simulate the quasi-resonant configuration similar to that reported in Rein et al. We furthermore show that our scenario is reliable with respect to the physical parameters involved in the resonance-trapping process. However, our scenario can only be confirmed with additional radial velocities measurements.

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Eccentricity Trap: Trapping of Resonantly Interacting Planets Near the Disk Inner Edge

Cited by 64 publications

References 24 publications

Formation of terrestrial planets in disks evolving via disk winds and implications for the origin of the solar system’s terrestrial planets

Formation of terrestrial planets in disks evolving via disk winds and implications for the origin of the solar system’s terrestrial planets

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

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

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