A pair of planets around HD 202206 or a circumbinary planet?

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  • 17 November 2004
Abstract
Long-term precise Doppler measurements with the CORALIE spectrograph reveal the presence of a second planet orbiting the solar-type star HD 202206. The radial-velocity combined fit yields companion masses of 17.4 M_Jup and 2.44 M_Jup, semi-major axis of a = 0.83 AU and 2.55 AU, and eccentricities of e = 0.43 and 0.27, respectively. A dynamical analysis of the system further shows a 5/1 mean motion resonance between the two planets. This system is of particular interest since the inner planet is within the brown-dwarf limits while the outer one is much less massive. Therefore, either the inner planet formed simultaneously in the protoplanetary disk as a superplanet, or the outer Jupiter-like formed in a circumbinary disk, the former explanation being favored by the observed mean-motion resonance. We believe this singular planetary system will provide important constraints upon planetary formation and migration scenarios.

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