On the Dynamical Stability of Gamma Cephei, an S-Type Binary Planetary System

Details On the Dynamical Stability of Gamma Cephei, an S-Type Binary Planetary System On the Dynamical Stability of Gamma Cephei, an S-Type Binary Planetary System

2004-03-12

arxiv.org/abs/astro-ph/0403312v1

AIP Conf.Proc. 713 (2004) 269

Astronomy and Astrophysics

Astrophysics

5 pages, 3 figures, to appear in the proceedings of "The Search For Other Worlds." The 14th Annual October Astrophysics Confer

Scientific paper

10.1063/1.1774536

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 ~2.14 AU semimajor axis and 0.12 eccentricity (hatzes et al. 2003). 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.

Affiliated with

Also associated with

No associations

Rating

On the Dynamical Stability of Gamma Cephei, an S-Type Binary Planetary System does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with On the Dynamical Stability of Gamma Cephei, an S-Type Binary Planetary System, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and On the Dynamical Stability of Gamma Cephei, an S-Type Binary Planetary System will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-161139