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Origin Theories for the Eccentricities of Extrasolar Planets

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Topics in Gravitational Dynamics

Part of the book series: Lecture Notes in Physics ((LNP,volume 729))

Abstract

Half the known extrasolar planets have orbital eccentricities in excess of 0.3. Such large eccentricities are surprising as it is thought that planets form in a protoplanetary disk on nearly circular orbits much like the current states of the solar system planets.

Possible explanations for the large planetary eccentricities include the perturbations that accompany planet-planet scattering, the tidal interaction between the gas disk and the planets, Kozai’s secular eccentricity cycles, the eccentricity excitation during planetary pair migration in mean motion resonance, the perturbations by stellar encounters, stellar-like relaxation that occurs if planets formed through gravitational instability, and the relative acceleration by the stellar jet system of the host star with respect to the companion.

In this chapter, we comment on the relevance and characteristics of the various eccentricity origin theories.

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Author information

Authors and Affiliations

  1. CNRS,Observatoire de la Côte d’Azur, BP 4229, 06304 Nice, France

    Fathi Namouni

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  1. Fathi Namouni
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  1. OCA - Nice, Observatoire de la Cote d’Azur, 06304 Nice CX 4, France

    Daniel Benest , Claude Froeschle  & Elena Lega ,  & 

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Namouni, F. (2007). Origin Theories for the Eccentricities of Extrasolar Planets. In: Benest, D., Froeschle, C., Lega, E. (eds) Topics in Gravitational Dynamics. Lecture Notes in Physics, vol 729. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-540-72984-6_8

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