Dynamically Unstable Planetary Systems Emerging Out of Gas Disks

Soko Matsumura, Edward W. Thommes, S. Chatterjee, Frederic A Rasio

Research output: Chapter in Book/Report/Conference proceedingConference contribution

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.
Original languageEnglish (US)
Title of host publicationExtreme Solar Systems
EditorsD Fischer, Frederic A Rasio, S E Thorsett, A Wolszczan
PublisherAstronomical Society of the Pacific
Pages301-307
Number of pages7
ISBN (Electronic)978-1-58381-667-7
ISBN (Print)978-1-58381-666-0
StatePublished - 2008

Publication series

NameAstronomical Society of the Pacific Conference Series
Volume398

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