Abstract
The evolution of the orbital eccentricity of a planet due to tidal interaction with a protoplanetary disk is modeled. It is found that the eccentricity of the planet tends to increase when the mass of the planet is large enough to make a gap in the disk, i.e., is larger than about a Saturn mass. The tidal interaction with the protoplanetary disk explains the high eccentricities of the extra-solar planets.
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References
Artymowicz, P. 1993, ApJ 419, 166
Goldreich, P., & Tremaine, S. 1980, ApJ 241, 425
Mazeh, T., Mayor, M., & Latham, D. W. 1997, ApJ 478, 367
Stone, J. M., & Norman, M. L. 1992, ApJS, 80, 753
Takeuchi, T., Miyama, S. M., & Lin, D. N. C. 1996, ApJ 460, 832
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© 1999 Springer Science+Business Media Dordrecht
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Takeuchi, T. (1999). Evolution of Orbital Eccentricity of a Protoplanet. In: Miyama, S.M., Tomisaka, K., Hanawa, T. (eds) Numerical Astrophysics. Astrophysics and Space Science Library, vol 240. Springer, Dordrecht. https://doi.org/10.1007/978-94-011-4780-4_48
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DOI: https://doi.org/10.1007/978-94-011-4780-4_48
Publisher Name: Springer, Dordrecht
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