2008/04/30 by Roman V. Baluev · 2 citations
Physics and Astronomy · #Apsidal precession #Astro and Planetary Science #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Atomic physics #Celestial mechanics #Eccentricity (behavior) #Mean motion #Orbital eccentricity #Orbital elements #Outer planets #Physics #Planet #Planetary system #Radial velocity #Resonance (particle physics) #Stars #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1007/s10569-008-9163-4
published as Celest. Mech. Dynam. Astron., 2008, Vol. 102, Issue 4, pp. 297-325 · 28 pages, 10 figures, 3 tables; Accepted to Celestial Mechanics and Dynamical Astronomy
arxiv created 2008/09/11 · openalex publication_date 2008/11/20 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
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.