About the Hill stability of extrasolar planets in stellar binary systems

Details About the Hill stability of extrasolar planets in stellar binary systems About the Hill stability of extrasolar planets in stellar binary systems

Jul 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008cemda.101..273s&link_type=abstract

Celestial Mechanics and Dynamical Astronomy, Volume 101, Issue 3, pp.273-287

Astronomy and Astrophysics

Astronomy

12

Extrasolar Planets, Elliptic Restricted Three-Body Problem, Hill Stability, Planets In Stellar Binary Systems

Scientific paper

We use a three dimensional generalization of Szebehely’s invariant relation obtained by us (Makó and Szenkovits, Celest. Mech. Dyn. Astron. 90, 51, 2004) in the elliptic restricted three-body problem, to establish more accurate criterion of the Hill stability. By using this criterion, the Hill stability of four extrasolar planets ( γ Cephei Ab, Gliese 86 Ab, HD 41004 Ab and HD 41004 Bb) is investigated.

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