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Paper: Dynamically Unstable Planetary Systems Emerging Out of Gas Disks
Volume: 398, Extreme Solar Systems
Page: 301
Authors: Matsumura, S.; Thommes, E.W.; Chatterjee, S.; Rasio, F.A.
Abstract: One of the most surprising properties of extrasolar planets is the eccentricity of their orbits, which vary from nearly circular (e ∼ 0) to highly eccentric ones (up to e ∼ 0.9). Planet-planet scattering with no gas disk has successfully reproduced the observed eccentricity distribution. However, this scenario alone cannot explain the distribution of planetary semi-major axes if giant planets form outside of ∼ 1 AU. Taking into account the effects of a residual gas disk after planet formation, we investigate the onset of dynamical instability in young planetary systems. Using a hybrid symplectic integrator + gas dynamics code, we demonstrate how planet-disk interactions along with planet-planet dynamical interactions could explain both the observed semi-major axis and eccentricity distributions of extrasolar planets.
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