Numerical simulations are made within the framework of the plane restricted three-body problem, in order to find out if stable orbits for planets around one of the two components in double stars can exist. For any given set of initial parameters (the mass ratio of the two stars and the eccentricity of their orbit around each other), the phase-space of initial positions and velocities is systematically explored.
In previous works, systematic exploration of the circular model as well as studies of more realistic (elliptic) cases such as Sun-Jupiter and the nearby α Centauri and Sirius systems, large stable planetary orbits were found to exist around both components of the binary, up to distances from each star of the order or more than half the binary's periastron separation.
The first results presented here for the η Coronae Borealis system confirm the previous studies.
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Benest, D. Stable planetary orbits around one component in nearby binary stars. II. Celestial Mech Dyn Astr 56, 45–50 (1993). https://doi.org/10.1007/BF00699718
- Restricted problem
- planets of double stars