Planetary orbits in the elliptic restricted problem. III. The η Coronae Borealis system.

Details Planetary orbits in the elliptic restricted problem. III. The η Coronae Borealis system. Planetary orbits in the elliptic restricted problem. III. The η Coronae Borealis system.

Oct 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996a%26a...314..983b&link_type=abstract

Astronomy and Astrophysics, v.314, p.983-988

Astronomy and Astrophysics

Astrophysics

21

Stars: Individual: {Eta} Crb, Celestial Mechanics, Binaries: General, Planetary Systems

Scientific paper

Numerical simulations are made within the frame of the elliptic plane restricted three-body problem, in order to search if stable orbits exist for planets around one of the two components in double stars. The η Coronae Borealis system is investigated here. Large stable planetary orbits, already known to exist through a systematic exploration of the circular model and for the Sun-Jupiter, the α Centauri and the Sirius elliptic cases, are found to exist around η CrB A and η CrB B up to distances from each star of the order of more than half the binary's periastron separation. Moreover, nearly circular stable planetary orbits are found to exist in the so-called "habitable zone" around each star.

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