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In recent years, several protoplanetary discs have been observed to exhibitspirals, both in scattered light and (sub)millimetre continuum data. The HD100453 binary star system hosts such a disc around its primary. Previous workhas argued that the spirals were caused by the gravitational interaction of thesecondary, which was assumed to be on a circular orbit, coplanar with the disc(meaning here the large outer disc, as opposed to the very small inner disc).However, recent observations of the CO gas emission were found incompatiblewith this assumption. In this paper, we run SPH simulations of the gas and dustdisc for seven orbital configurations taken from astrometric fits and computesynthetic observations from their results. Comparing to high-resolution ALMA$^{12}$CO data, we find that the best agreement is obtained for an orbit witheccentricity $e=0.32$ and semi-major axis $a=207$ au, inclined by $61^\circ$relative to the disc plane. The large misalignment between the disc and orbitplanes is compatible with the tidal evolution of a circumprimary disc in aneccentric, unequal-mass binary star.

Spirals, shadows & precession in HD 100453 -- I. The orbit of the binary