Near mean motion resonance of terrestrial planet pair induced by giant planet: application to Kepler-68 system

Pan, Mengrui; Wang, Su; Ji, Jianghui

doi:10.1093/mnras/staa1884

Cited by 16 publications

(7 citation statements)

References 81 publications

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“…We adopt a reasonable reduction factor f1 = 0.3 in Eqn. 4 (Pan et al 2020), where the gas accretion of planets is not considered.…”

Section: Inward Migration Formationmentioning

confidence: 99%

“…Furthermore, inside-out planetary formation model indicates that planets in the inner disk are produced sequentially at the pressure maximum by pebble collision or near snow line by streaming instabilities, thereby revealing formation of tightly-packed planetary system (Chatterjee & Tan 2014;Ormel et al 2017). Besides, tidal circularization, secular resonance sweeping, planetary interaction as well as stellar magnetosphere may also rebuild planetary configurations to yield compact and close-in systems (Nagasawa & Ida 2011;Pan et al 2020;Liu & Ji 2020).…”

Section: Introductionmentioning

confidence: 99%

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The Terrestrial Planet Formation around M Dwarfs: In-situ, Inward Migration or Reversed Migration

Pan,

Wang,

2021

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Terrestrial planets are commonly observed to orbit M dwarfs with close-in trajectories. In this work, we extensively perform N-body simulations of planetesimal accretion with three models of in-situ, inward migration and reversed migration to explore terrestrial formation in tightly compact systems of M dwarfs. In the simulations, the solid disks are assumed to be 0.01% of the masses of host stars and spread from 0.01 to 0.5 AU with the surface density profile scaling with r −k according to the observations. Our results show that in-situ scenario may produce 7.77 +3.23 −3.77 terrestrial planets with an average mass of 1.23 +4.01 −0.93 M ⊕ around M dwarfs. The number of planets tends to increase as the disk slope is steeper or with a larger stellar mass. Moreover, we show that 2.55 +1.45 −1.55 planets with mass of 3.76 +8.77 −3.46 M ⊕ are formed in the systems via inward migration, while 2.85 +1.15 −0.85 planets with 3.01 +13.77 −2.71 M ⊕ are yielded under reversed migration. Migration scenarios can also deliver plentiful water from the exterior of ice line to the interior due to more efficient accretion. The simulation outcomes of reversed migration model produce the best matching with observations, being suggestive of a likely mechanism for planetary formation around M dwarfs.

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“…We adopt a reasonable reduction factor f1 = 0.3 in Eqn. 4 (Pan et al 2020), where the gas accretion of planets is not considered.…”

Section: Inward Migration Formationmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

The Terrestrial Planet Formation around M Dwarfs: In-situ, Inward Migration or Reversed Migration

Pan,

Wang,

2021

Preprint

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“…4.1 we already have shown that there are different ways to establish the separation between planets c and d, although the small distant migration torque favours a scenario with high 𝐴 e . In addition, the radial gravity from the exterior disc on the planets in the cavity (Nagasawa et al 2003;Pan et al 2020) might play an important role in 3BRs trapping and escape, which has not been investigated in this study. A setup alternative to dCav_gImp_cOL would be for planet d and e to become trapped in 4:3 MMR, instead of 3:2, after planet formation and to let three planets fall in the cavity during Stage II, such that the cavity radius coincides with the current location of planet e. This would at first glance be more natural as the 3BR Φ 2,5,3 b,c,d and Φ 2,6,4 c,d,e which form during Stage I remain librating.…”

Section: Discussionmentioning

confidence: 93%

The dynamics of the TRAPPIST-1 system in the context of its formation

Huang,

Ormel

2021

Preprint

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TRAPPIST-1 is an 0.09 𝑀 star, which harbours a system of seven Earth-sized planets. Two main features stand out: (i) all planets have similar radii, masses, and compositions; and (ii) all planets are in resonance. Previous works have outlined a pebble-driven formation scenario where planets of similar composition form sequentially at the H 2 O snowline (∼0.1 au for this low-mass star). It was hypothesized that the subsequent formation and migration led to the current resonant configuration. Here, we investigate whether the sequential planet formation model is indeed capable to produce the present-day resonant configuration, characterized by its two-body and three-body mean motion resonances structure. We carry out N-body simulations, accounting for type-I migration, stellar tidal damping, disc eccentricity damping, and featuring a migration barrier located at the disc's inner edge. We demonstrate that the present-day dynamical configuration of the TRAPPIST-1 system is in line with the sequential formation/migration model. First, a chain of first-order resonances was formed at the disc inner edge by convergent migration. We argue that TRAPPIST-1b and c marched across the migration barrier, into the gas-free cavity, during the dispersal of the gas disc. The dispersing disc then pushed planets b and c inward until they settled in a configuration close to the observed resonances. Thereafter, the stellar tidal torque also attributed towards a modest separation of the inner system. We argue that our scenario is also applicable to other compact resonant planet systems.

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“…From the statistic results, we find that there are plenty of planet pairs in the configuration of near MMRs especially the first order resonances, such as 2:1 and 3:2 MMRs (Lissauer et al 2011;Wang et al 2012;Lee et al 2013;Wang & Ji 2014, 2017Antoniadou & Libert 2020). However, the peaks in the distribution of period ratios are shown not in the exact location of MMRs, but a little departure from them (Wang et al 2012;Lee et al 2013;Steffen et al 2013;Wu et al 2019;Pan et al 2020). Most of the planet pairs pipe up at the location larger than the exact MMRs.…”

Section: Introductionmentioning

confidence: 88%

“…If planets migrate to the inner region of the system, the effect of the tidal raised by the star can destroy the configuration of MMRs and become near MMRs configuration. Based on this formation scenario, we investigated the configuration formation of KOI-152 system with planets in near 4:2:1 MMRs (Wang et al 2012), the formation of near 2:1 and 3:2 MMRs effected by the properties of star, the speed of type I migration (Wang & Ji 2014), the effect caused by the mass accretion process and the possible outward migration , and the existence of giant planets in planetary systems (Sun et al 2017;Pan et al 2020).…”

Section: Introductionmentioning

confidence: 99%

Departure from the Exact Location of Mean Motion Resonances Induced by the Gas Disk in the Systems Observed by Kepler

Wang,

Lin,

Zheng

et al. 2020

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The statistical results of transiting planets show that there are two peaks around 1.5 and 2.0 in the distribution of orbital period ratios. A large number of planet pairs are found near the exact location of mean motion resonances (MMRs). In this work, we find out that the depletion and structures of gas disk play crucial roles in driving planet pairs out of exact location of MMRs. Under such scenario, planet pairs are trapped into exact MMRs during orbital migration firstly and keep migrating in a same pace. The eccentricities can be excited. Due to the existence of gas disk, eccentricities can be damped leading to the change of orbital period. It will make planet pairs depart from the exact location of MMRs. With depletion timescales larger than 1 Myr, near MMRs configurations are formed easily. Planet pairs have higher possibilities to escape from MMRs with higher disk aspect ratio. Additionally, with weaker corotation torque, planet pairs can depart farther from exact location of MMRs. The final location of the innermost planets in systems are directly related to the transition radius from optically thick region to inner optically thin disk. While the transition radius is smaller than 0.2 AU at the late stage of star evolution process, the innermost planets can reach around 10 days. Our formation scenario is a possible mechanism to explain the formation of near MMRs configuration with the innermost planet farther than 0.1 AU.

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Near mean motion resonance of terrestrial planet pair induced by giant planet: application to Kepler-68 system

Cited by 16 publications

References 81 publications

The Terrestrial Planet Formation around M Dwarfs: In-situ, Inward Migration or Reversed Migration

The Terrestrial Planet Formation around M Dwarfs: In-situ, Inward Migration or Reversed Migration

The dynamics of the TRAPPIST-1 system in the context of its formation

Departure from the Exact Location of Mean Motion Resonances Induced by the Gas Disk in the Systems Observed by Kepler

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