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We constrain the binary parameters of the eclipsing accreting X-ray binaryIGR J17451--3022 and the nature of its donor star. The donor mass, its radius,and the system inclination angle are computed based on the system orbitalperiod and eclipse duration recently reported by Bozzo et al.\ (2016). We findthat the donor is most likely a main-sequence star with the mass comprisedwithin the range $\sim$(0.5--$0.8){\rm M}_{\odot}$ and the radius of $\sim\!0.7{\rm R}_{\odot}$. Assuming that the accreting compact object in IGRJ17451--3022 is a neutron star, the duration of the nearly total rectangulareclipses yields the inclination angle of the system of $71^\circ\lesssimi\lesssim 76^\circ$, compatible with the presence of dips in this system. Werule out the presence of either brown or white dwarf. However, we find analternative possibility that the donor star in IGR J17451--3022 could be apartially stripped giant with a very low mass, $\sim\! 0.2{\rm M}_{\odot}$.This case requires a substantial mass loss prior to the formation of thegiant-star He core. According to that solution, the radius would be $\sim\!0.4{\rm R}_{\odot}$, at $i\sim 80^\circ$. We additionally show that thewell-known approximate dependence of the giant-star radius exclusively on itscore mass breaks down below $\sim\!0.3{\rm M}_{\odot}$.

IGR J17451--3022: constraints on the nature of the donor star