• DOI:10.1088/0004-637X/719/1/890
• Corpus ID: 118707953

THE LICK-CARNEGIE EXOPLANET SURVEY: A URANUS-MASS FOURTH PLANET FOR GJ 876 IN AN EXTRASOLAR LAPLACE CONFIGURATION

@article{Rivera2010THELE,
  title={THE LICK-CARNEGIE EXOPLANET SURVEY: A URANUS-MASS FOURTH PLANET FOR GJ 876 IN AN EXTRASOLAR LAPLACE CONFIGURATION},
  author={Eugenio Jose Rivera and Gregory P. Laughlin and R. Paul Butler and Steven S. Vogt and Nader Haghighipour and Stefano Meschiari},
  journal={The Astrophysical Journal},
  year={2010},
  volume={719},
  pages={890 - 899}
}

• E. Rivera, G. Laughlin, +3 authors S. Meschiari
• Published 22 June 2010
• Physics, Geology
• The Astrophysical Journal

Continued radial velocity (RV) monitoring of the nearby M4V red dwarf star GJ 876 with Keck/High Resolution Echelle Spectrograph has revealed the presence of a Uranus-mass fourth planetary companion in the system. The new planet has a mean period of Pe = 126.6 days (over the 12.6-year baseline of the RV observations), and a minimum mass of mesin ie = 12.9 ± 1.7 M⊕. The detection of the new planet has been enabled by significant improvements to our RV data set for GJ 876. The data have been augmented by 36 new high-precision measurements taken over the past five years. In addition, the precision of all of the Doppler measurements have been significantly improved by the incorporation of a high signal-to-noise template spectrum for GJ 876 into the analysis pipeline. Implementation of the new template spectrum improves the internal rms errors for the velocity measurements taken during 1998–2005 from 4.1 m s−1 to 2.5 m s−1. Self-consistent, N-body fits to the RV data set show that the four-planet system has an invariable plane with an inclination relative to the plane of the sky of i = 59.°5. The fit is not significantly improved by the introduction of a mutual inclination between the planets “b” and “c,” but the new data do confirm a non-zero eccentricity, ed = 0.207 ± 0.055 for the innermost planet, “d.” In our best-fit coplanar model, the mass of the new component is me = 14.6 ± 1.7 M⊕. Our best-fitting model places the new planet in a three-body resonance with the previously known giant planets (which have mean periods of Pc = 30.4 and Pb = 61.1 days). The critical argument, φLaplace = λc − 3λb + 2λe, for the Laplace resonance librates with an amplitude of ΔφLaplace = 40° ± 13° about φLaplace = 0°. Numerical integration indicates that the four-planet system is stable for at least a billion years (at least for the coplanar cases). This resonant configuration of three giant planets orbiting an M dwarf primary differs from the well-known Laplace configuration of the three inner Galilean satellites of Jupiter, which are executing very small librations about φLaplace = 180° and which never experience triple conjunctions. The GJ 876 system, by contrast, comes close to a triple conjunction between the outer three planets once per every orbit of the outer planet, “e.”