Origin scenarios for the Kepler 36 planetary system

Quillen, Alice C.; Bodman, Eva H. L.; Moore, Alexander

doi:10.1093/mnras/stt1442

Cited by 45 publications

(18 citation statements)

References 56 publications

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“…The giant impact hypothesis is consistent with the chaotic dynamics exhibited in the Kepler-36 system (Deck et al 2012). Hydrodynamic and N-body simulations have revealed that stochastic/convergent migration can lead to close encounters between the two planets and physical collisions with other embryos (Paardekooper et al 2013;Quillen et al 2013).…”

supporting

confidence: 69%

Giant Impact: An Efficient Mechanism for the Devolatilization of Super-Earths

Liu

Hori

Lin

et al. 2015

ApJ

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Mini-Neptunes and volatile-poor super-Earths coexist on adjacent orbits in proximity to host stars such as Kepler-36 and Kepler-11. Several post-formation processes have been proposed for explaining the origin of the compositional diversity between neighboring planets: the mass loss via stellar XUV irradiation, degassing of accreted material, and in-situ accumulation of the disk gas. Close-in planets are also likely to experience giant impacts during the advanced stage of planet formation. This study examines the possibility of transforming volatile-rich super-Earths / mini-Neptunes into volatile-depleted super-Earths through giant impacts. We present the results of three-dimensional hydrodynamic simulations of giant impacts in the accretionary and disruptive regimes. Target planets are modeled with a three-layered structure composed of an iron core, silicate mantle and hydrogen/helium envelope. In the disruptive case, the giant impact can remove most of the H/He atmosphere immediately and homogenize the refractory material in the planetary interior. In the accretionary case, the planet is able to retain more than half of the original gaseous envelope, while a compositional gradient suppresses efficient heat transfer as the planetary interior undergoes double-diffusive convection. After the giant impact, a hot and inflated planet cools and contracts slowly. The extended atmosphere enhances the mass loss via both a Parker wind induced by thermal pressure and hydrodynamic escape driven by the stellar XUV irradiation. As a result, the entire gaseous envelope is expected to be lost due to the combination of those processes in both cases. Based on our results, we propose that Kepler-36b may have been significantly devolatilized by giant impacts, while a substantial fraction of Kepler-36c's atmosphere may remain intact. Furthermore, the stochastic nature of giant impacts may account for the observed large dispersion in the mass-radius relationship of close-in super-Earths and mini-Neptunes (at least to some extent).

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supporting

confidence: 69%

Giant Impact: An Efficient Mechanism for the Devolatilization of Super-Earths

Liu

Hori

Lin

et al. 2015

ApJ

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“…Assuming flat disks ( f = 0) and typical values of H 0 ∼ 0.05, we obtain factors on the order of K i ∼ 300 for any distance from the star, which are the values usually employed in N-body simulations of planetary migration and resonance capture (e.g., Quillen et al 2013;Silburt & Rein 2015). A flared disk ( f > 0) not only leads to a dependence of K i on the semimajor axis, but also increases its value for close-in planets.…”

Section: Offset and The K-factorsmentioning

confidence: 87%

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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“…In this population, there are 974 multiple planetary systems, including 652 two-planet systems, 222 three-planet systems and 75 four-planet systems. As previously mentioned, most of the planetary candidates in the multiple planetary systems are believed to be real planets Ciardi et al 2013;Quillen et al 2013). Based on current data, in Figure 1, we show the distribution of the period ratios of the planet pairs for all of the planetary candidates (the upper panel ) and for all of the three-planet systems (the lower panel ).…”

Section: Introductionmentioning

confidence: 94%

NEAR 3:2 AND 2:1 MEAN MOTION RESONANCE FORMATION IN THE SYSTEMS OBSERVED BYKEPLER

Wang¹,

2014

ApJ

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The Kepler mission has released ∼ 4229 transiting planet candidates. There are approximately 222 candidate systems with three planets. Among them, the period ratios of planet pairs near 1.5 and 2.0 reveal that two peaks exist for which the proportions of the candidate systems are ∼ 7.0% and 18.0%, respectively. In this work, we study the formation of mean motion resonance (MMR) systems, particularly for the planetary configurations near 3:2 and 2:1 MMRs, and we concentrate on the interplay between the resonant configuration and the combination of stellar accretion rate, stellar magnetic field, speed of migration and additional planets. We perform more than 1000 runs by assuming a system with a solar-like star and three surrounding planets. From the statistical results, we find that under the formation scenario, the proportions near 1.5 and 2.0 can reach 14.5% and 26.0%, respectively. In addition,Ṁ = 0.1 × 10 −8 M ⊙ yr −1 is propitious toward the formation of 3:2 resonance, whereasṀ = 2 × 10 −8 M ⊙ yr −1 contributes to the formation of 2:1 resonance. The speed-reduction factor of type I migration f 1 ≥ 0.3 facilitates 3:2 MMRs, whereas f 1 ≥ 0.1 facilitates 2:1 MMRs. If additional planets are present in orbits within the innermost or beyond the outermost planet in a three-planet system, 3:2:1 MMRs can be formed, but the original systems trapped in 4:2:1 MMRs are not affected by the supposed planets. In summary, we conclude that this formation scenario will provide a likely explanation for Kepler candidates involved in 2:1 and 3:2 MMRs.

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Origin scenarios for the Kepler 36 planetary system

Cited by 45 publications

References 56 publications

Giant Impact: An Efficient Mechanism for the Devolatilization of Super-Earths

Giant Impact: An Efficient Mechanism for the Devolatilization of Super-Earths

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

NEAR 3:2 AND 2:1 MEAN MOTION RESONANCE FORMATION IN THE SYSTEMS OBSERVED BYKEPLER

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