No Difference in Orbital Parameters of RV-detected Giant Planets between 0.1 and 5 au in Single versus Multi-stellar Systems

作者：Ngo Henry; Knutson Heather A; Bryan Marta L; Blunt Sarah; Nielsen Eric L; Batygin Konstantin; Bowler Brendan P; Crepp Justin R; Hinkley Sasha; Howard Andrew W; Mawet Dimitri

来源：Astronomical Journal, 2017, 153(6): 242.

DOI：10.3847/1538-3881/aa6cac

• binaries: close
• binaries: eclipsing
• methods: observational
• planetary systems
• planets and satellites: dynamical evolution and stability
• techniques: high angular resolution

Our Keck/NIRC2 imaging survey searches for stellar companions around 144 systems with radial velocity (RV) detected giant planets to determine whether stellar binaries influence the planets' orbital parameters. This survey, the largest of its kind to date, finds eight confirmed binary systems and three confirmed triple systems. These include three new multi-stellar systems (HD 30856, HD 86081, and HD 207832) and three multi-stellar systems with newly confirmed common proper motion (HD 43691, HD 116029, and HD 164509). We combine these systems with seven RV planet-hosting multi-stellar systems from the literature in order to test for differences in the properties of planets with semimajor axes ranging between 0.1 and 5 au in single versus multi-stellar systems. We find no evidence that the presence or absence of stellar companions alters the distribution of planet properties in these systems. Although the observed stellar companions might influence the orbits of more distant planetary companions in these systems, our RV observations currently provide only weak constraints on the masses and orbital properties of planets beyond 5 au. In order to aid future efforts to characterize long-period RV companions in these systems, we publish our contrast curves for all 144 targets. Using four years of astrometry for six hierarchical triple star systems hosting giant planets, we fit the orbits of the stellar companions in order to characterize the orbital architecture in these systems. We find that the orbital plane of the secondary and tertiary companions are inconsistent with an edge-on orbit in four out of six cases.

• 出版日期2017-6