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Dynamics of the giant planets of the solar system in the gaseous proto-planetary disk and relationship to the current orbital architecture
- Source :
- Astron.J.134:1790-1798,2007
- Publication Year :
- 2007
-
Abstract
- 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).<br />Comment: The Astronomical Journal (17/07/2007) in press
- Subjects :
- Astrophysics
Subjects
Details
- Database :
- arXiv
- Journal :
- Astron.J.134:1790-1798,2007
- Publication Type :
- Report
- Accession number :
- edsarx.0706.1713
- Document Type :
- Working Paper
- Full Text :
- https://doi.org/10.1086/521705