Near 3:2 and 2:1 mean motion resonances formation in the systems observed by Kepler

Abstract

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, $\dot{M}=0.1\times 10^{-8}{M}_{\odot }\mathrm{y}{\mathrm{r}}^{-1}$ is propitious toward the formation of 3:2 resonance, whereas $\dot{M}=2\times 10^{-8}{M}_{\odot }\mathrm{y}{\mathrm{r}}^{-1}$ contributes to the formation of 2:1 resonance. The speed-reduction factor of type I migration $f_1\ge 0.3$ facilitates 3:2 MMRs, whereas $f_1\ge 0.1$ 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.

13 pages, 8 figures, accepted for publication in ApJ

References in corpus (9)

• Toward a Deterministic Model of Planetary Formation V. Accumulation Near the Ice Line
• Accretion in the Rho-Oph pre-main sequence stars
• Detailed Models of super-Earths: How well can we infer bulk properties?
• Grain Retention and Formation of Planetesimals near the Snow Line in MRI-driven Turbulent Protoplanetary Disks
• Resonant Repulsion of Kepler Planet Pairs
• Constraints on resonant-trapping for two planets embedded in a protoplanetary disc
• Assembling the Building Blocks of Giant Planets around Intermediate Mass Stars
• The Dynamical Simulations of the Planets Orbiting GJ 876
• The Librating Companions in HD 37124, HD 12661, HD 82943, 47 Uma and GJ 876: Alignment or Antialignment?

Cited by in corpus (11)

• Obliquity-Driven Sculpting of Exoplanetary Systems
• A Tale of Planet Formation: From Dust to Planets
• When, where, and how many planets end up in first-order resonances?
• Near Mean-motion Resonances in the Systems Observed by Kepler: Affected by Mass Accretion and Type I Migration
• Dynamical Evolution of Closely Packed Multiple Planetary Systems Subject to Atmospheric Mass-Loss
• Terrestrial Planets Formation under Migration: the Systems near 4:2:1 Mean Motion Resonance
• The scattering outcomes of Kepler circumbinary planets: planet mass ratio
• Departure from the Exact Location of Mean Motion Resonances Induced by the Gas Disk in the Systems Observed by Kepler
• Near Mean Motion Resonance of Terrestrial Planet Pair Induced by Giant Planet: Application to Kepler-68 System
• Dynamical rearrangement of super-Earths during disk dispersal II. Assessment of the magnetospheric rebound model for planet formation scenarios
• Transit timing variations, radial velocities and long-term dynamical stability of the system Kepler-410