  The young star PDS110 in the Ori OB1a association underwent two similar
eclipses in 2008 and 2011, each of which lasted for a period of at least 25
days. One plausible explanation for these events is that the star was eclipsed
by an unseen giant planet (named PDS110b) circled by a ring system that fills a
large fraction of its Hill sphere. Through thousands of numerical simulations
of the three-body problem, we constrain the mass and eccentricity of this
planet as well the size and inclination of its ring, parameters that are not
well determined by the observational data alone. We carried out a broad range
of different configurations for the PDS110b ring system and ruled out all that
did not match with the observations. The result shows that the ring system
could be prograde or retrograde; the preferred solution is that the ring has an
inclination lower than $60^\circ$ and a radius between 0.1 and 0.2 au and that
the planet is more massive than $35 M_\mathrm{Jup}$ and has a low eccentricity
(<0.05).
