Precision radial velocity measurements of the \gamma Cephei ( HR8974 ) binary system suggest the existence of a planetary companion with a minimum mass of 1.7 Jupiter-mass on an elliptical orbit with a \sim 2.14 AU semimajor axis and 0.12 eccentricity [ ] .
I present in this paper a summary of the results of an extensive numerical study of the orbital stability of this three-body system for different values of the semimajor axis and orbital eccentricity of the binary , and also the orbital inclination of the planet .
Numerical integrations indicate that the system is stable for the planet ’ s orbital inclination ranging from 0 to 60 degrees , and for the binary ’ s orbital eccentricity less than 0.5 .
The results also indicate that for large values of the inclination , the system may be locked in a Kozai resonance .