The dynamical stability of extra-solar planets in binary systems

Details The dynamical stability of extra-solar planets in binary systems The dynamical stability of extra-solar planets in binary systems

Jun 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004coska..34..105s&link_type=abstract

Contributions of the Astronomical Observatory Skalnaté Pleso, vol. 34, no. 2, p. 105-118.

Astronomy and Astrophysics

Astronomy

2

Three-Body Problem, Extra-Solar Planets, Dynamical Stability, Gliese 86, Γ Cephei, 61 Cygni

Scientific paper

The question about dynamical stability of extra-solar planets is considered in the frame of the general three-body problem, i.e. a planet in the binary system revolves around one of the components. The distance between the star's components is much longer than between the orbiting star and the planet. In the differential equations with regard to the eccentricity and the argument of the perigee we used the Hamiltonian without the short-periodic terms, excluded by von Zeipel's method.
The possible conditions of the dynamical stability of extra-solar planets are presented by their orbital parameters -- the mutual inclination of orbits and the argument of the perigee of the planet.
The theory has been applied to the systems Gliese 86, γ Cephei, and 61 Cygni. The results were verified by the numerical integration.

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