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The 2:1 librating-circulating planetary configuration produced by a hybrid scenario

Published online by Cambridge University Press:  10 November 2011

Jianghui Ji ,
Zhao Sun ,
Sheng Jin  and
Niu Zhang
Jianghui Ji
Affiliation:
Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing, 210008, China; email: [email protected].
Zhao Sun
Affiliation:
Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing, 210008, China; email: [email protected]. Graduate School of Chinese Academy of Sciences, Beijing 100049, China
Sheng Jin
Affiliation:
Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing, 210008, China; email: [email protected]. Graduate School of Chinese Academy of Sciences, Beijing 100049, China
Niu Zhang
Affiliation:
Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing, 210008, China; email: [email protected]. Graduate School of Chinese Academy of Sciences, Beijing 100049, China
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Abstract

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Different migration scenario of two giant planets may play a major role in forming the diverse resonant planetary configurations. The studies on the HD 128311 and HD 73526 systems show that two gas giants are captured in a 2:1 resonance but not in apsidal corotation, because one of the resonant argument circulates over the dynamical evolution. Herein we explore potential scenarios to produce the 2:1 librating-circulating resonance configuration. In the simulations, we find that both colliding or scattering events at early stage of dynamical evolution can induce the configurations trapped into resonance. In this sense, the librating-circulating resonance configuration is more likely to form by a hybrid mechanism of scattering and collision.

Keywords

celestial mechanicsplanetary systems: formation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S276: The Astrophysics of Planetary Systems: Formation, Structure, and Dynamical Evolution , October 2010 , pp. 501 - 503
Copyright
Copyright © International Astronomical Union 2011

References

Chambers, J. E. 1999, MNRAS, 304, 793CrossRefGoogle Scholar
Kley, W., Lee, M. H., Murray, N., & Peale, S. J. 2005, A&A, 437, 727Google Scholar
Lee, M. H. 2004, ApJ, 611, 517CrossRefGoogle Scholar
Marcy, G. W., Butler, R. P., Fischer, D. A., et al. 2001, ApJ, 556, 296Google Scholar
Mayor, M., Udry, S., Naef, D., et al. 2004, A&A, 415, 391Google Scholar
Sándor, Z. & Kley, W. 2006, A&A, 451, L31Google Scholar
Sándor, Z., Kley, W., & Klagyivik, P. 2007, A&A, 472, 981, 28Google Scholar
Tinney, C. G., Butler, R. P., Marcy, G. W., et al. 2006, ApJ, 647, 594CrossRefGoogle Scholar
Vogt, S. S., Butler, R. P., Marcy, G. W., et al. 2005, ApJ, 632, 638Google Scholar
Zhang, N., Ji, J. & Sun, Z. 2010, MNRAS, 405, 2016Google Scholar