  We investigate the orbital stability of a putative Jovian planet in a compact
binary \nu Octantis reported by Ramm et al. We re-analyzed published radial
velocity data in terms of self-consistent Newtonian model and we found stable
best-fit solutions that obey observational constraints. They correspond to
retrograde orbits, in accord with an earlier hypothesis of Eberle & Cuntz, with
apsidal lines anti-aligned with the apses of the binary. The best-fit solutions
are confined to tiny stable regions of the phase space. These regions have a
structure of the Arnold web formed by overlapping low-order mean motion
resonances and their sub-resonances. The presence of a real planet is still
questionable, because its formation would be hindered by strong dynamical
perturbations. Our numerical study makes use of a new computational Message
Passing Interface (MPI) framework MECHANIC developed to run massive numerical
experiments on CPU clusters.
