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How planet–planet scattering can create high-inclination as well as long-period orbits

Published online by Cambridge University Press:  10 November 2011

Sourav Chatterjee ,
Eric B. Ford  and
Frederic A. Rasio
Sourav Chatterjee
Affiliation:
University of Florida, 211 Bryant Space Science Center, Florida, USA email: [email protected], [email protected]
Eric B. Ford
Affiliation:
University of Florida, 211 Bryant Space Science Center, Florida, USA email: [email protected], [email protected]
Frederic A. Rasio
Affiliation:
CIERA, Northwestern University, Evanston, IL 60208, USA email: [email protected]
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Abstract

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Recent observations have revealed two new classes of planetary orbits. Rossiter-Mclaughlin (RM) measurements have revealed hot Jupiters in high-obliquity orbits. In addition, direct-imaging has discovered giant planets at large (~ 100 AU) separations via direct-imaging technique. Simple-minded disk-migration scenarios are inconsistent with the high-inclination (and even retrograde) orbits as seen in recent RM measurements. Furthermore, forming giant planets at large semi-major axis (a) may be challenging in the core-accretion paradigm. We perform many N-body simulations to explore the two above-mentioned orbital architectures. Planet–planet scattering in a multi-planet system can naturally excite orbital inclinations. Planets can also get scattered to large distances. Large-a planetary orbits created from planet–planet scattering are expected to have high eccentricities (e). Theoretical models predict that the observed long-period planets, such as Fomalhaut-b have moderate e ≈ 0.3. Interestingly, these are also in systems with disks. We find that if a massive-enough outer disk is present, a scattered planet may be circularized at large a via dynamical friction from the disk and repeated scattering of the disk particles.

Keywords

scatteringmethods: n-body simulationsmethods: numericalplanetary systems
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. 225 - 229
Copyright
Copyright © International Astronomical Union 2011

References

Chambers, J. E. 1999, MNRAS, 304, 793CrossRefGoogle Scholar
Chatterjee, S., Ford, E. B., Matsumura, S., & Rasio, F. A. 2008, ApJ, 686, 580CrossRefGoogle Scholar
Dodson-Robinson, S. E., Veras, D., Ford, E. B., & Beichman, C. A. 2009, ApJ, 707, 79CrossRefGoogle Scholar
Ducourant, C., et al. 2008, A&A, 477, L1Google Scholar
Ireland, M. J., et al. 2011, ApJ, 726, id.113CrossRefGoogle Scholar
Jurić, M. & Tremaine, S. 2008, ApJ, 686, 603CrossRefGoogle Scholar
Kalas, P., et al. 2008, Science, 322, 1345CrossRefGoogle Scholar
Lai, D., Foucart, F., & Lin, D. N. C. 2011, MNRAS, 412, 2790CrossRefGoogle Scholar
Levison, H. F. & Stewart, G. R. 2001, Icarus, 153, 224CrossRefGoogle Scholar
Marois, C., et al. 2008, Science, 322, 1348CrossRefGoogle Scholar
Mayor, M. & Queloz, D. 1995, Nature, 378, 355CrossRefGoogle Scholar
McArthur, B. E., et al. 2010, ApJ, 715, 1203CrossRefGoogle Scholar
Morton, T. D. & Johnson, J. A. 2011, ApJ, 729, id.138CrossRefGoogle Scholar
Nagasawa, M., Ida, S., & Bessho, T. 2008, ApJ, 678, 498CrossRefGoogle Scholar
Triaud, A. H. M. J., et al. 2010, A&A, 524, A25Google Scholar
Winn, J. N., Fabrycky, D., Albrecht, S., & Johnson, J. A. 2010, ApJL, 718, L145CrossRefGoogle Scholar