Planetary Orbits Due to Interactions with Their Parent Stars

Details Planetary Orbits Due to Interactions with Their Parent Stars Planetary Orbits Due to Interactions with Their Parent Stars

Jan 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004iaus..219..781c&link_type=abstract

Stars as suns : activity, evolution and planets, Proceedings of the 219th symposium of the International Astronomical Union held

Physics

Condensed Matter

Statistical Mechanics

Scientific paper

The motion of a protoplanet orbiting its parent star taking into account the tidal forces due to its finite size is analysed by unifying two 3-dimensional spaces corresponding to orbital motion of the protoplanet and its finite size in extended 6-dimensional space. Using the variational principle a criterion is formulated which tends towards energy minimization of the system. As the protoplanet condenses and approches a point the 6-dimensional space reduces to our usual 3-dimensional space and the criterion towards energy minimization requires a circular orbit. An application of statistical mechanics indicates that the thermal distribution function favors high eccentricities and circularization takes place in the adiabatic regimen. This indicates a scenerio in which the protoplanets are formed in highly elongated orbits and circularize their orbits in an effort to attain the ground state in a large timescale (as also indicated by simulations). The theory is applied to many astrometric binaries (e.g. Gliese 569 LHS 1047 BD+66°34) and suspected pulser-planatery systems (e.g.1257+12); whence it is found that many of them are close to the ground state.

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