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The Configuration Formation of Planetary Systems Observed by Kepler

Published online by Cambridge University Press:  29 April 2014

Su Wang  and
Jianghui Ji
Su Wang
Affiliation:
Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210008, China email: [email protected]
Jianghui Ji
Affiliation:
Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210008, China email: [email protected]
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Abstract

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The Kepler mission has found many planetary systems, among them more than 80 systems host three planet candidates which reveal a configuration of near 4:2:1 mean motion resonance. In this paper, we focus on the configuration formation of resonant systems. As shown from our model and N-body simulations, we find that 3:2 mean motion resonance always forms at the early stage of star evolution and planets undergo high rate of migration, while 2:1 mean motion resonance happens at the late stage of the star formation, more often.

Keywords

(stars:) planetary systems: formation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S293: Formation, Detection, and Characterization of Extrasolar Habitable Planets , August 2012 , pp. 106 - 109
Copyright
Copyright © International Astronomical Union 2014 

References

Batalha, N. M., Rowe, J. F., Bryson, S. T., et al. 2012, ApJS 204 article id. 24Google Scholar
Fabrycky, D. C., Lissauer, J. J., Ragozzine, D., et al. 2012, arXiv:1202.6328Google Scholar
Lissauer, J. J., Ragozzine, D., Fabrycky, D. C., et al. 2011, ApJS, 197, 8CrossRefGoogle Scholar
Koenigl, A. 1991, ApJL, 370, L39Google Scholar
Kley, W., Bitsch, B., & Klahr, H. 2009, A&A, 506, 971Google Scholar
Kretke, K. A., Lin, D. N. C., Garaud, P., & Turner, N. J. 2009, ApJ, 690, 407Google Scholar
Wang, S. & Zhou, J. L. 2011, ApJ, 727, 108Google Scholar
Wang, S., Ji, J. H., & Zhou, J. L. 2012, ApJ, 753, 170CrossRefGoogle Scholar