  In this work we propose a new orbital architecture for the two proposed
circumbinary planets around the polar eclipsing binary HU Aquarii. We base the
new two-planet, light-travel time model on the result of a Monte Carlo
simulation driving a least-squares Levenberg-Marquardt minimisation algorithm
on the observed eclipse egress times. Our best-fitting model with
$\chi_{r}^2=1.43$ resulted in high final eccentricities for the two companions
leading to an unstable orbital configuration. From a large ensemble of initial
guesses we examined the distribution of final eccentricities and semi-major
axes for different $\chi_{r}^2$ parameter intervals and encountered
qualitatively a second population of best-fitting parameters. The main
characteristic of this population is described by low-eccentric orbits
favouring long-term orbital stability of the system. We present our
best-fitting model candidate for the proposed two-planet system and demonstrate
orbital stability over one million years using numerical integrations.
