期刊
ASTRONOMY & ASTROPHYSICS
卷 563, 期 -, 页码 -出版社
EDP SCIENCES S A
DOI: 10.1051/0004-6361/201322067
关键词
planets and satellites: detection; techniques: radial velocities; techniques: photometric; stars: individual: HD 13908; stars: individual: HD 159243; stars: individual: HIP 91258
资金
- Swiss National Foundation
- Agence Nationale de la Recherche [ANR-08-JCJC-0102-01]
- CNES
- European Research Council/European Community [239953]
- Fundacao para a Ciencia e a Tecnologia (FCT)
- FCT/MCTES (Portugal)
- POPH/FSE (EC)
- Programme National de Planetologie
- [PTDC/CTE-AST/66643/2006]
- [PTDC/CTE-AST/098528/2008]
- [SFRH/BPD/81084/2011]
- Fundação para a Ciência e a Tecnologia [SFRH/BPD/81084/2011] Funding Source: FCT
We present high-precision radial-velocity measurements of three solar-type stars: HD 13908, HD 159243, and HIP 91258. The observations were made with the SOPHIE spectrograph at the 1.93 m telescope of the Observatoire de Haute-Provence (France). They show that these three bright stars host exoplanetary systems composed of at least two companions. HD 13908 b is a planet with a minimum mass of 0.865 +/- 0.035 M-Jup on a circular orbit with a period of 19.382 +/- 0.006 days. There is an outer massive companion in the system with a period of 931 +/- 17 days, e = 0.12 +/- 0.02, and a minimum mass of 5.13 +/- 0.25 M-Jup. The star HD 159243 also has two detected companions with respective masses, periods, and eccentricities of M-p= 1.13 +/- 0.05 and 1.9 +/- 0.13 M-Jup, P = 12.620 +/- 0.004 and 248.4 +/- 4.9 days, and e = 0.02 +/- 0.02 and 0.075 +/- 0.05. Finally, the star HIP 91258 has a planetary companion with a minimum mass of 1.068 +/- 0.038 M-Jup, an orbital period of 5.0505 +/- 0.0015 days, and a quadratic trend indicating an outer planetary or stellar companion that is as yet uncharacterized. The planet-hosting stars HD 13908, HD 159243, and HIP 91258 are main-sequence stars of spectral types F8V, G0V, and G5V, respectively, with moderate activity levels. HIP 91258 is slightly over-metallic, while the other two stars have solar-like metallicity. The three systems are discussed in the frame of formation and dynamical evolution models of systems composed of several giant planets.
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