Stable Planetary Motion in Double Stars

Details Stable Planetary Motion in Double Stars Stable Planetary Motion in Double Stars

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aspc..321..410p&link_type=abstract

Extrasolar Planets: Today and Tomorrow, ASP Conference Proceedings, Vol. 321, held 30 June - 4 July 2003, Institut D'Astrophysiq

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The discovery of extra-solar planets in double star systems and the fact that double and multiple star systems are more numerous than single star systems like the sun (at least in the solar neighborhood) leads to a common interest of stability studies of such systems. As a global result we present the stable regions in binaries with different mass-ratios. Furthermore, we show the results of a numerical investigation for the binary γ Cephei. To distinguish between stable and chaotic motion we use different methods, i.e. the Fast Lyapunov Indicator (FLI), the Mean Exponential Growth Factor of Nearby Orbits (MEGNO), and straightforward orbital computations. The two chaos indicators are known to be fast methods for the determination of the orbital behavior.

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