  In this work, we investigate the eclipse timing of the polar binary HU
Aquarii that has been observed for almost two decades. Recently, Qian et al.
attributed large (O-C) deviations between the eclipse ephemeris and
observations to a compact system of two massive jovian companions. We improve
the Keplerian, kinematic model of the Light Travel Time (LTT) effect and
re-analyse the whole currently available data set. We add almost 60 new, yet
unpublished, mostly precision light curves obtained using the time
high-resolution photo-polarimeter OPTIMA, as well as photometric observations
performed at the MONET/N, PIRATE and TCS telescopes. We determine new
mid--egress times with a mean uncertainty at the level of 1 second or better.
We claim that because the observations that currently exist in the literature
are non-homogeneous with respect to spectral windows (ultraviolet, X-ray,
visual, polarimetric mode) and the reported mid--egress measurements errors,
they may introduce systematics that affect orbital fits. Indeed, we find that
the published data, when taken literally, cannot be explained by any unique
solution. Many qualitatively different and best-fit 2-planet configurations,
including self-consistent, Newtonian N-body solutions may be able to explain
the data. However, using high resolution, precision OPTIMA light curves, we
find that the (O-C) deviations are best explained by the presence of a single
circumbinary companion orbiting at a distance of ~4.5 AU with a small
eccentricity and having ~7 Jupiter-masses. This object could be the next
circumbinary planet detected from the ground, similar to the announced
companions around close binaries HW Vir, NN Ser, UZ For, DP Leo or SZ Her, and
planets of this type around Kepler-16, Kepler-34 and Kepler-35.
