Other
Scientific paper
Sep 1985
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985mnras.216..521d&link_type=abstract
Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 216, Sept. 15, 1985, p. 521-527.
Other
4
Orbit Perturbation, Planetary Evolution, Planetary Orbits, Protoplanets, Solar System, Astronomical Models, Helium, Hydrogen, Stability, Three Body Problem, Planets, Orbits, Stability, Formation, Theoretical Studies, Evolution, Planetesimals, Volatiles, Evaporation, Analysis, Calculations, Models, Three-Body Problem, Terrestrial Planets, Hydrogen, Helium, Simulations
Scientific paper
One theory of planetary formation suggests that the planets evolved from giant gaseous protoplanets which lost their volatile elements. Analytical calculations of the hierarchical stability of three-body systems suggest that the most likely configuration to be unstable is that of a large protoplanet moving in close proximity to a forming terrestrial planet which has already lost most of its excess hydrogen and helium, and not two large protoplanets as originally suggested by the present authors and others. The orbital stability of such configurations was examined numerically for various combinations of planets and protoplanets in the inner Solar System. It was found that all the systems considered were stable for at least a period of 103yr.
Donnison J. R.
Williams Iwan P.
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