The full set of published radial velocity data (52 measurements from Keck + 58 ones from ELODIE + 17 ones from CORALIE) for the star HD37124 is analysed. Two families of dynamically stable high-eccentricity orbital solutions for the planetary system are found. In the first one, the outer planets c and d are trapped in the 2/1 mean-motion resonance. The second family of solutions corresponds to the 5/2 mean-motion resonance between these planets. In both families, the planets are locked in (or close to) an apsidal corotation resonance. In the case of the 2/1 MMR, it is an asymmetric apsidal corotation (with the difference between the longitudes of periastra Δω ~ 60°), whereas in the case of the 5/2 MMR it is a symmetric antialigned one (Δω = 180°). It remains also possible that the two outer planets are not trapped in an orbital resonance. Then their orbital eccentricities should be relatively small (less than, say, 0.15) and the ratio of their orbital periods is unlikely to exceed 2.3 - 2.5.

Original languageEnglish
Pages (from-to)297-325
Number of pages29
JournalCelestial Mechanics and Dynamical Astronomy
Volume102
Issue number4
DOIs
StatePublished - 1 Dec 2008

    Research areas

  • Exoplanets, HD37124, Periodic orbits, Planetary systems, Resonance, Stability, Statistical methods

    Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

ID: 36296952