Astronomy and Astrophysics – Astronomy
Scientific paper
Mar 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003mnras.340...43w&link_type=abstract
Monthly Notice of the Royal Astronomical Society, Volume 340, Issue 1, pp. 43-51.
Astronomy and Astrophysics
Astronomy
6
Methods: N-Body Simulations, Celestial Mechanics, Solar System: Formation
Scientific paper
The migration of planets has usually been considered in relation to circular orbits of protoplanets for which type I and II migration mechanisms are appropriate. There are theories for planetary origin in which protoplanets are produced in extended eccentric orbits requiring a different theoretical treatment. The basic mechanism for the action of a resisting medium involves gravitational interaction with the planet and the simple application of the principle of conservation of momentum. A gaseous resisting medium will be in the form of a flared disc with a three-dimensional structure. Such a medium is simulated by a distribution of non-interacting particles, initially in a stable orbit around the central star. Their gravitational interactions with the protoplanet are softened, as for particles in smoothed-particle hydrodynamics, to avoid gravitational singularities. Computations, in which parameters are varied in a systematic manner, give a range of final orbits similar to those observed and inferred for exoplanets. When the motion of the medium is affected by high luminosity and/or a strong stellar wind from an active young star, orbits of high eccentricity may be an outcome, as is observed for some exoplanets.
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