4.6 Article

TRAPPIST-1: Dynamical analysis of the transit-timing variations and origin of the resonant chain

期刊

ASTRONOMY & ASTROPHYSICS
卷 658, 期 -, 页码 -

出版社

EDP SCIENCES S A
DOI: 10.1051/0004-6361/202142377

关键词

celestial mechanics; planet-disk interactions; protoplanetary disks; planets and satellites: formation; planets and satellites: dynamical evolution and stability; planets and satellites: detection

资金

  1. Fonds de la Recherche Scientifique -FNRS Postdoctoral Research Fellowship
  2. Fonds de la Recherche Scientifique -FNRS [F.4523.20]
  3. NASA's NExSS Virtual Planetary Laboratory under NASA Astrobiology Institute [NNA13AA93A]
  4. NASA Astrobiology Program [80NSSC18K0829]
  5. FNRS-FRFC
  6. Walloon Region
  7. University of Namur [2.5020.11, GEQ U.G006.15, 1610468, RW/GEQ2016]

向作者/读者索取更多资源

Analysis of the TRAPPIST-1 system's posterior distribution reveals that the planets are in two-planet and three-planet resonances, with TTV signals showing common periods from days to decades. N-body simulations with migration forces suggest that under specific disk conditions, a resonance chain similar to the observed one can be formed.
We analyze solutions drawn from the recently published posterior distribution of the TRAPPIST-1 system, which consists of seven Earth-size planets appearing to be in a resonant chain around a red dwarf. We show that all the planets are simultaneously in two-planet and three-planet resonances, apart from the innermost pair for which the two-planet resonant angles circulate. By means of a frequency analysis, we highlight that the transit-timing variation (TTV) signals possess a series of common periods varying from days to decades, which are also present in the variations of the dynamical variables of the system. Shorter periods (e.g., the TTVs characteristic timescale of 1.3 yr) are associated with two-planet mean-motion resonances, while longer periods arise from three-planet resonances. By use of N-body simulations with migration forces, we explore the origin of the resonant chain of TRAPPIST-1 and find that for particular disc conditions, a chain of resonances - similar to the observed one - can be formed which accurately reproduces the observed TTVs. Our analysis suggests that while the 4-yr collected data of observations hold key information on the two-planet resonant dynamics, further monitoring of TRAPPIST-1 will soon provide signatures of three-body resonances, in particular the 3.3 and 5.1 yr periodicities expected for the current best-fit solution. Additional observations would help to assess whether the innermost pair of planets is indeed resonant (its proximity to the 8:5 resonance being challenging to explain), and therefore give additional constraints on formation scenarios.

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