A statistical examination of the short-term stability of the v Andromedae planetary system

Because of the high eccentricities (similar to0.3) of two of the possible p lanets about the star v Andromeda, the stability of the system requires car eful study. We present results of 1000 numerical simulations which explore the orbital parameter space as constrained by the observations. The orbital parameters of each planet are chosen from a Gaussian error distribution, a nd the resulting configuration is integrated for 1 Myr. We find that 84% of these integrations are stable. Configurations in which the eccentricity of the third planet is less than or similar to0.3 are always stable, but when the eccentricity is greater than or similar to0.45, the system is always u nstable, typically producing a close encounter between the second and third planets. A similar exercise with the gas giants in our solar system sample d with the same error distribution was performed. Approximately 81% of thes e simulations were stable for 10(6) yr.