Dynamical Stability of Earth-like Orbits in Binary Systems

Details Dynamical Stability of Earth-like Orbits in Binary Systems Dynamical Stability of Earth-like Orbits in Binary Systems

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aas...201.4614d&link_type=abstract

American Astronomical Society, 201st AAS Meeting, #46.14; Bulletin of the American Astronomical Society, Vol. 34, p.1177

Astronomy and Astrophysics

Astronomy

Scientific paper

We explore the stability of an Earth-like planet orbiting a solar mass star in the presence of an outer-lying intermediate mass companion. Specifically, we numerically determine the planet's ejection time for an extensive range of companion masses, eccentricities, and semi-major axes. We find power-law relations between the ejection time and the companion's perihelion distance to the solar mass star. Although the numerically intensive nature of our calculation limits most of our integration times to 10 million years, we extrapolate our results to draw conclusions about the habitability of Earth-like planets.

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