Evidence for Multiple Companions to υ Andromedae

The bright F8 V star t Andromedae was previously reported to have a 4.6 day Doppler velocity periodicity, consistent with having a Jupiter-mass companion orbiting at 0.059 AU. Follow-up obser- vations by both the Lick and Advanced Fiber-Optic Echelle spectrometer (AFOE) planet survey pro- grams con—rm this periodicity and reveal additional periodicities at 241 and 1267 days. These periodicities are consistent with Keplerian orbital motion and imply two additional companions orbiting at 0.83 and 2.5 AU, with minimum (M sin i) masses of 2.0 and 4.6 respectively. Non-Keplerian M JUP , explanations for the observed Doppler velocity variations, including radial and nonradial pulsations, rotational modulation of surface features, and stellar magnetic cycles, are examined. These explanations seem unlikely based on the observed photometric and chromospheric stability of the star. This putative three-planet system is found to be dynamically stable by both analytic techniques and numerical simula- tions. The outer two companions both reside in eccentric orbits, as do all nine known extrasolar planet candidates in distant orbits. If real, this multiple-planet system is the —rst around a main-sequence star, and its study should oUer insights into planet formation, planet-planet interactions, and the observed eccentricities of planetary orbits. Subject headings: binaries: spectroscopicplanetary systemsstars: individual (t Andromedae)

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