Planetary orbits in the elliptic restricted problem. V.
The ADS 11060 system
CNRS UMR 6529 “Cassini" OCA Observatoire de Nice, BP 4229, 06304 Nice Cedex 4, France
Corresponding author: firstname.lastname@example.org
Accepted: 19 December 2002
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. Large stable planetary orbits, already known to exist (more precisely, known to be possible from the 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.
Key words: celestial mechanics / stars: binaries: general / stars: individual: ADS 11060 / stars: planetary systems
© ESO, 2003