On the migration of three planets in a protoplanetary disc and the formation of chains of mean motion resonances

Migaszewski, Cezary

doi:10.1093/mnras/stw386

Cited by 39 publications

(22 citation statements)

References 44 publications

(59 reference statements)

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“…the planets to migrate. However, orbital migration may not be convergent (Migaszewski 2015(Migaszewski , 2016, that is, not leading to resonant capture. Moreover, some mechanisms have been proposed to inhibit the capture even in the case of convergent migration, such as turbulence in the disk or e-dependent migration rates.…”

Section: Discussionmentioning

confidence: 99%

The role of dissipative evolution for three-planet, near-resonant extrasolar systems

Pichierri

Batygin

Morbidelli

2019

A&A

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Early dynamical evolution of close-in planetary systems is shaped by an intricate combination of planetary gravitational interactions, orbital migration, and dissipative effects. While the process of convergent orbital migration is expected to routinely yield resonant planetary systems, previous analyses have shown that the semi-major axes of initially resonant pairs of planets will gradually diverge under the influence of long-term energy damping, producing an overabundance of planetary period ratios in slight excess of exact commensurability. While this feature is clearly evident in the orbital distribution of close-in extrasolar planets, the existing theoretical picture is limited to the specific case of the planetary three-body problem. In this study, we generalise the framework of dissipative divergence of resonant orbits to multi-resonant chains, and apply our results to the current observational census of well-characterised three-planet systems. Focusing on the 2:1 and 3:2 commensurabilities, we identify three 3-planet systems, whose current orbital architecture is consistent with an evolutionary history wherein convergent migration first locks the planets into a multiresonant configuration and subsequent dissipation repels the orbits away from exact commensurability. Nevertheless, we find that the architecture of the overall sample of multi planetary systems is incompatible with this simple scenario, suggesting that additional physical mechanisms must play a dominant role during the early stages of planetary systems' dynamical evolution.

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Section: Discussionmentioning

confidence: 99%

The role of dissipative evolution for three-planet, near-resonant extrasolar systems

Pichierri

Batygin

Morbidelli

2019

A&A

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“…The curve corresponds to the Laplace three-body resonance, for which the mean motions of the planets obey the relation n 1 − 3 n 2 + 2 n 3 = 0. A three-planet system that is initially involved in this chain of MMRs would evolve divergently along a curve y −1 = 3/2 − x/2, where x ≡ P 2 /P 1 = n 1 /n 2 and y ≡ P 3 /P 2 = n 2 /n 3 (Migaszewski 2016). We can see that even though τ 1 > τ 2 , P 2 /P 1 increases and the observed configuration is omitted.…”

Section: Formation Of the Kepler-30 Systemmentioning

confidence: 93%

“…Slowing down the migration of this planet does not necessarily lead to an increase of P 3 /P 2 without changing P 2 /P 1 . The divergent migration of three planets away from a given chain of MMRs can occur along certain paths at the period ratio-period ratio diagram (Migaszewski 2016). It is then possible that P 2 /P 1 would also increase, even though τ 1 > τ 2 .…”

Section: Formation Of the Kepler-30 Systemmentioning

confidence: 99%

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The architecture and formation of the Kepler-30 planetary system

Panichi

Goździewski

Migaszewski

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We study the orbital architecture, physical characteristics of planets, formation and long-term evolution of the Kepler-30 planetary system, detected and announced in 2012 by the KEPLER team. We show that the Kepler-30 system belongs to a particular class of very compact and quasi-resonant, yet long-term stable planetary systems. We re-analyse the light curves of the host star spanning Q1-Q17 quarters of the KEPLER mission. A huge variability of the Transit Timing Variations (TTV) exceeding 2 days is induced by a massive Jovian planet located between two Neptune-like companions. The innermost pair is near to the 2:1 mean motion resonance (MMR), and the outermost pair is close to higher order MMRs, such as 17:7 and 7:3. Our re-analysis of photometric data allows us to constrain, better than before, the orbital elements, planets' radii and masses, which are 9.2 ± 0.1, 536 ± 5, and 23.7 ± 1.3 Earth masses for Kepler-30b, Kepler-30c and Kepler-30d, respectively. The masses of the inner planets are determined within ∼ 1% uncertainty. We infer the internal structures of the Kepler-30 planets and their bulk densities in a wide range from (0.19 ± 0.01) g·cm −3 for Kepler-30d, (0.96 ± 0.15) g·cm −3 for Kepler-30b, to (1.71 ± 0.13) g·cm −3 for the Jovian planet Kepler-30c. We attempt to explain the origin of this unique planetary system and a deviation of the orbits from exact MMRs through the planetary migration scenario. We anticipate that the Jupiter-like planet plays an important role in determining the present dynamical state of this system. tems make it possible to further refine their orbital parameters and masses (e.g., Borsato et al. 2014;Barros et al. 2014).In this paper, we report on a new and up-to-date characterization of the Kepler-30 system composed of three planets. These planets have been validated by Fabrycky et al. (2012) on the basis of the very initial Q1-Q6 KEPLER data quarters ( 600 days) as well as by Tingley et al. (2011) on the basis of the first Q0-Q2 quarters.The early studies on this system were focused on the orbital-spin alignment and star-spots detection (Sanchis-Ojeda et al. 2012) or on differential rotation of the parent star (Lanza et al. 2014). Here, we take full advantage of the available light curves of Kepler-30, spanning Q1-Q17 quarters ( 1600 days) to constrain better the masses and orbital elements of the planets.We find the Kepler-30 system particularly interesting and unique in the KEPLER sample for several reasons. One of them is the huge TTV full-amplitude of the innermost planet of 2 days (48 hours), which is two times larger than the TTV fullamplitude of 1 day for the innermost planet in the Kepler-88 system (Nesvorný et al. 2013) dubbed as "the king of the transit c 2017 RAS

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“…More recently, Migaszewski (2015Migaszewski ( , 2016 studied the effect of more complex disk models on migration of planetary pairs, including photo-evaporation and different opacity laws. They found that several regions of divergent migration appear in the disk that may lead to departure from exact resonance and even ejection from the commensurabilities.…”

Section: Introductionmentioning

confidence: 99%

Planetary migration and the origin of the 2:1 and 3:2 (near)-resonant population of close-in exoplanets

Ramos

Charalambous

Benítez-Llambay

et al. 2017

A&A

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We present an analytical and numerical study of the orbital migration and resonance capture of fictitious two-planet systems with masses in the super-Earth range undergoing Type-I migration. We find that, depending on the flare index and proximity to the central star, the average value of the period ratio, P 2 /P 1 , between both planets may show a significant deviation with respect to the nominal value. For planets trapped in the 2:1 commensurability, offsets may reach values on the order of 0.1 for orbital periods on the order of 1 day, while systems in the 3:2 mean-motion resonance (MMR) show much smaller offsets for all values of the semimajor axis. These properties are in good agreement with the observed distribution of near-resonant exoplanets, independent of their detection method. We show that 2:1-resonant systems far from the star, such as HD82943 and HR8799, are characterized by very small resonant offsets, while higher values are typical of systems discovered by Kepler with orbital periods approximately a few days. Conversely, planetary systems in the vicinity of the 3:2 MMR show little offset with no significant dependence on the orbital distance. In conclusion, our results indicate that the distribution of Kepler planetary systems around the 2:1 and 3:2 MMR are consistent with resonant configurations obtained as a consequence of a smooth migration in a laminar flared disk, and no external forces are required to induce the observed offset or its dependence with the commensurability or orbital distance from the star.

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On the migration of three planets in a protoplanetary disc and the formation of chains of mean motion resonances

Cited by 39 publications

References 44 publications

The role of dissipative evolution for three-planet, near-resonant extrasolar systems

The role of dissipative evolution for three-planet, near-resonant extrasolar systems

The architecture and formation of the Kepler-30 planetary system

Planetary migration and the origin of the 2:1 and 3:2 (near)-resonant population of close-in exoplanets

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