  In a recent paper Martin & Lubow showed that a circumbinary disc around an
eccentric binary can undergo damped nodal oscillations that lead to the polar
(perpendicular) alignment of the disc relative to the binary orbit. The disc
angular momentum vector aligns to the eccentricity vector of the binary. We
explore the robustness of this mechanism for a low mass disc (0.001 of the
binary mass) and its dependence on system parameters by means of hydrodynamic
disc simulations. We describe how the evolution depends upon the disc
viscosity, temperature, size, binary mass ratio, orbital eccentricity and
inclination. We compare results with predictions of linear theory. We show that
polar alignment of a low mass disc may occur over a wide range of binary-disc
parameters. We discuss the application of our results to the formation of
planetary systems around eccentric binary stars.
