Eccentricity Damping of Extra-solar Planets

Details Eccentricity Damping of Extra-solar Planets Eccentricity Damping of Extra-solar Planets

Sep 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998dps....30.2308w&link_type=abstract

American Astronomical Society, DPS meeting #30, #23.08; Bulletin of the American Astronomical Society, Vol. 30, p.1057

Astronomy and Astrophysics

Astronomy

1

Scientific paper

Although tidal dissipation is a plausible source of orbit circularization for some close companions, rho Cr B at 0.23 AU is too distant from its primary for this mechanism to be effective. An alternative mechanism that can operate when a planet orbits near a disk, is described. The planet excites a one-armed spiral apsidal wave in the vicinity of a secular resonance where the periastron precessions rates of planet and disk match. The resulting reaction torque on the planet can affect a rapid change in its eccentricity. The possible relevance of this to the orbits of extra-solar planets is discussed.

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