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The High Eccentricity of the Planet Around 16 Cyg B

Tsevi Mazeh·Yuval Krymolowski·Gady Rosenfeld
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Abstract

We consider the high eccentricity, 0.66, of the newly discovered planet around 16 Cyg B, using the fact that the parent star is part of a wide binary. We show that the high eccentricity of the planet could be the result of tidal forces exerted on 16 Cyg B and its planet by 16 Cyg A, the distant companion in the system. By following stellar triple systems with parameters similar to those of 16 Cyg, we have established that the orbital eccentricity of the planet could have gone through strong modulation, with an amplitude of 0.8 or even larger, with typical timescale of tens of millions years. The amplitude of the planet eccentricity strongly depends on the relative inclination between the plane of motion of the planet and that of the wide binary 16 Cyg AB. To account for the present eccentricity of the planet we have to assume that the angle between the two planes of motion is large, at least 60 deg. We argue that this assumption is reasonable for wide binaries like 16 Cyg AB.

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Tsevi Mazeh, Yuval Krymolowski, Gady Rosenfeld. 1996-11-18. The High Eccentricity of the Planet Around 16 Cyg B. https://doi.org/10.1086/310536

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