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Formation of the Planetary Candidates Observed by Kepler Mission

Published online by Cambridge University Press:  27 October 2016

Su Wang  and
Jianghui Ji
Su Wang
Affiliation:
Key Laboratory of Planetary Sciences, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210008, China email: wangsu@pmo.ac.cn, jijh@pmo.ac.cn
Jianghui Ji
Affiliation:
Key Laboratory of Planetary Sciences, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210008, China email: wangsu@pmo.ac.cn, jijh@pmo.ac.cn
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Abstract

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The Kepler Mission which launched in 2009 March focuses on detecting potentially habitable terrestrial-sized planets. To date the Kepler mission has released more than 4000 planetary candidates. There are plenty of planet pairs trapped near the first order mean motion resonance (MMR). From the statistical results of numerical simulations based on the formation scenario we proposed for the planetary configurations near 3:2 and 2:1 MMRs, we find that the proportions of period ratios close to 1.5 and 2.0 can arrive at 14.5% and 26.0%, respectively. This scenario may explain the formation of Kepler candidates pairs in near 3:2 and 2:1 MMRs.

Keywords

(stars:) planetary systems: formationmethods: numerical
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , General Assembly A29A: Astronomy in Focus , August 2015 , pp. 27 - 29
Copyright
Copyright © International Astronomical Union 2016 

References

Batygin, K. & Morbidelli, A. 2013, AJ, 145, 1 CrossRefGoogle Scholar
Delisle, J. B. & Laskar, J. 2014, A&A, 570, L7 Google Scholar
Fabrycky, D. C., Lissauer, J. J., Ragozzine, D., et al. 2014, ApJ, 790, 146 CrossRefGoogle Scholar
Ida, S. & Lin, D. N. C. 2004, ApJ, 604, 388 CrossRefGoogle Scholar
Kretke, K. A. et al. 2009, ApJ, 690, 407 CrossRefGoogle Scholar
Lithwick, Y. & Wu, Y. 2012, ApJL, 756, 11 CrossRefGoogle Scholar
Masset, F. S. et al. 2006, ApJ, 642, 478 CrossRefGoogle Scholar
Pringle, J. E. 1981, ARA & A, 19, 137 CrossRefGoogle Scholar
Terquem, C. & Paploizou, J. C. B. 2007, ApJ, 654, 1110 CrossRefGoogle Scholar
Wang, S., Ji, J. H., & Zhou, J. L. 2012, ApJ, 753, 170 CrossRefGoogle Scholar
Wang, S. & Ji, J. H. 2014, ApJ, 795, 85 CrossRefGoogle Scholar