摘要：We present a detailed orbital and stability analysis of the HD59686 binary-star planet system. HD59686 is a single-lined, moderately close (aB=13.6 au) eccentric (eB=0.73) binary, where the primary is an evolved K giant with mass M=1.9Me and the secondary is a star with a minimum mass of mB0.53Me. Additionally, on the basis of precise radial velocity (RV) data, a Jovian planet with a minimum mass of mp=7 MJup, orbiting the primary on a nearly circular S-type orbit with ep=0.05 and ap=1.09 au, has recently been announced. Weinvestigate large sets of orbital fits consistent with HD 59686ʼs RV data by applying bootstrap and systematic grid search techniques coupled with self-consistent dynamical fitting. We perform long-term dynamical integrations of these fits to constrain the permitted orbital configurations. We find that if the binary and the planet in this system have prograde and aligned coplanar orbits, there are narrow regions of stable orbital solutions locked in a secular apsidal alignment with the angle between the periapses, Δω, librating about 0°. We also test a large number of mutually inclined dynamical models in an attempt to constrain the three-dimensional orbital architecture. We find that for nearly coplanar and retrograde orbits with mutual inclination 145°Δi180°, the system is fully stable for a large range of orbital solutions.
关键词：planetary systems;planets and satellites: detection;planets and satellites: dynamical evolution and stability;techniques: radial velocities
