期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 445, 期 1, 页码 749-760出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stu1751
关键词
methods: numerical; planets and satellites: dynamical evolution and stability; planets and satellites: formation; planets and satellites: individual: Kepler-11; planets and satellites: individual: Kepler-32; planets and satellites: individual: Kepler-80
资金
- Science & Technology Facilities Council (STFC)
- STFC [ST/G00711X/1]
- Leverhulme Trust through a Philip Leverhulme Prize
- STFC Consolidated Grant [ST/K001000/1]
- STFC
- Large Facilities Capital Fund of BIS
- BIS National E-Infrastructure capital grant [ST/K000373/1]
- STFC DiRAC Operations grant [ST/K0003259/1]
- National Aeronautics and Space Administration
- Science and Technology Facilities Council [ST/M006948/1, ST/H00856X/1, ST/H002235/1, ST/K001000/1, PP/E00119X/1, ST/K502121/1, ST/G00711X/1, ST/K000373/1] Funding Source: researchfish
- STFC [ST/K502121/1, ST/H00856X/1, PP/E00119X/1, ST/H002235/1, ST/G00711X/1, ST/K000373/1, ST/K001000/1, ST/M006948/1] Funding Source: UKRI
The Kepler mission has recently discovered a number of exoplanetary systems, such as Kepler-11 and Kepler-32, in which ensembles of several planets are found in very closely packed orbits (often within a few per cent of an au of one another). These compact configurations present a challenge for traditional planet formation and migration scenarios. We present a dynamical study of the assembly of these systems, using an N-body method which incorporates a parametrized model of planet migration in a turbulent protoplanetary disc. We explore a wide parameter space, and find that under suitable conditions it is possible to form compact, close-packed planetary systems via traditional disc-driven migration. We find that simultaneous migration of multiple planets is a viable mechanism for the assembly of tightly packed planetary systems, as long as the disc provides significant eccentricity damping and the level of turbulence in the disc is modest. We discuss the implications of our preferred parameters for the protoplanetary discs in which these systems formed, and comment on the occurrence and significance of mean-motion resonances in our simulations.
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