Abstract
Numerical simulations are made within the framework of the elliptic plane restricted three-body problem, in order to determine whether stable orbits exist for planets around one of the two components in double stars. The ADS 11060 system is investigated here. Largestable planetary orbits, already known to exist (more precisely, known to be possible fromthe dynamical point of view) through a systematic exploration of the circular model and for several cases of the elliptic model (Sun-Jupiter, α Centauri, Sirius, η Coronae Borealis and ADS 12033), are found to exist around ADS 11060 A and ADS 11060 B up to distances from each star of the order of more than half the binary's periastron separation. But, in this case, nearly circular stable planetary orbits are not found to exist either in the so-called habitable zone around each star or anywhere else; this is very likely due to the high value of the eccentricity of the binary's orbit.
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