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

We constrain the binary parameters and the nature of the donor star of the eclipsing accreting X-ray binary IGR J17451-3022. The donor mass, its radius, and the system inclination angle are computed based on the system orbital period and eclipse duration recently reported. We find that the donor is most likely a main-sequence star with the mass comprised within the range similar to(0.5-0.8) M-circle dot and a radius of similar to 0.7 R-circle dot. Assuming that the accreting compact object in IGR J17451-3022 is a neutron star, the duration of the nearly total rectangular eclipses yields an inclination angle of the system of 71 degrees less than or similar to i less than or similar to 76 degrees, compatible with the presence of dips in this system. We rule out the presence of either a brown or white dwarf. However, we find an alternative possibility that the donor star in IGR J17451-3022 could be a partially stripped giant with a very low mass, similar to 0.2 M-circle dot. This case requires a substantial mass loss prior to the formation of the giant-star He core. According to that solution, the radius would be similar to 0.4 R-circle dot, at i similar to 80 degrees. We additionally show that the well-known approximate dependence of the giant-star radius exclusively on its core mass, breaks down below similar to 0.3 M-circle dot.