Dynamics of the Giant Planets of the Solar System in the Gaseous Proto-planetary Disk and Relationship to the Current Orbital Architecture

Details Dynamics of the Giant Planets of the Solar System in the Gaseous Proto-planetary Disk and Relationship to the Current Orbital Architecture Dynamics of the Giant Planets of the Solar System in the Gaseous Proto-planetary Disk and Relationship to the Current Orbital Architecture

Oct 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007dps....39.6004m&link_type=abstract

American Astronomical Society, DPS meeting #39, #60.04; Bulletin of the American Astronomical Society, Vol. 39, p.537

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We study the orbital evolution of the 4 giant planets of our solar system in a gas disk. Our investigation extends the previous works by Masset and Snellgrove (2001) and Morbidelli and Crida (2007, MC07), which focussed on the dynamics of the Jupiter-Saturn system. The only systems that we found to reach a steady state are those in which the planets are locked in a quadruple mean motion resonance (i.e. each planet is in resonance with its neighbor). In total we found 6 such configurations. For the gas disk parameters found in MC07, these configurations are characterized by a negligible migration rate. After the disappearance of the gas, and in absence of planetesimals, only two of these six configurations (the least compact ones) are stable for a time of hundreds of millions of years or more. The others become unstable on a timescale of a few My. Our preliminary simulations show that, when a planetesimal disk is added beyond the orbit of the outermost planet, the planets can evolve from the most stable of these configurations to their current orbits in a fashion qualitatively similar to that described in Tsiganis et al. (2005)

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