NEAR 3:2 AND 2:1 MEAN MOTION RESONANCE FORMATION IN THE SYSTEMS OBSERVED BY KEPLER
NEAR 3:2 AND 2:1 MEAN MOTION RESONANCE FORMATION IN THE SYSTEMS OBSERVED BY KEPLER
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DOI：
10.1088/0004-637x/795/1/85
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发表时间：
2014-09
期刊：
影响因子：
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通讯作者：
Su Wang;J. Ji
中科院分区：
文献类型：
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作者：
Su Wang;J. Ji
开普勒任务释放了凌日行星候选∼4229。大约有222个候选系统有三颗行星。其中，行星对周期比在1.5点和2.0点附近显示存在两个峰值，候选系统所占比例分别为∼7.0%和18.0%。在这项工作中，我们研究了平均运动共振(MMR)系统的形成，特别是对于接近3：2和2：1的行星组态，我们集中讨论了共振组态与恒星吸积率、恒星磁场、迁移速度和额外行星的组合之间的相互作用。我们假设一个系统有一颗类似太阳的恒星和三颗周围的行星，我们进行了超过1000次的运行。从统计结果中我们发现，在编队情景下，1.5和2.0附近的比例可以分别达到14.5%和26.0%。另外，有利于形成3：2共振，有利于形成2：1共振。I型迁移的减速系数F1⩾0.3有助于3：2 MMR，而F1⩾0.1有助于2：1 MMR。在一个由三颗行星组成的系统中，如果在最内层或最外层的轨道上存在额外的行星，则可以形成3：2：1的MMR，但被困在4：2：1 MMR中的原始系统不会受到假想行星的影响。总之，我们得出的结论是，这种形成情景将为2：1和3：2 MMR中涉及的开普勒候选者提供一个可能的解释。
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, is propitious toward the formation of 3:2 resonance, whereas contributes to the formation of 2:1 resonance. The speed-reduction factor of type I migration f1 ⩾ 0.3 facilitates 3:2 MMRs, whereas f1 ⩾ 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.