Origin theories for the eccentricities of extrasolar planets
arXiv:astro-ph/0702203 · doi:10.1007/978-3-540-72984-6_8
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.
23 pages, 8 figures. Review lecture at the 2006 Aussois Winter School "Open Problems in Celestial Mechanics". To appear in Lecture Notes in Physics, Springer
References in corpus (9)
- The N2K Consortium. II. A Transiting Hot Saturn Around HD 149026 With a Large Dense Core
- Giant Planet Companion to 2MASSW J1207334-393254
- High Orbital Eccentricities of Extrasolar Planets Induced by the Kozai Mechanism
- Excitation and Propagation of Eccentricity Disturbances in Planetary Systems
- Planetary formation in the Gamma-Cephei system
- Statistical properties of exoplanets IV. The period--eccentricity relations of exoplanets and of binary stars
- On the saturation of corotation resonances: a numerical study
- On the Origin of the Eccentricities of Extrasolar Planets
- Mass loss at the lowest stellar masses