 Solution

Assume a central eclipse and nearly uniform projected speed during it. Let $r$ be the smaller radius and $R$ the larger. First-to-second contact requires travel $2r$, whereas the totality interval requires $2(R-r)$. With relative speed 200 km s${}^{-1}$,The light curve has ingress, flat minimum and egress lasting 1.7, 0.8 and 1.7 hours. At the four contacts the projected center separations are $R+r,R-r,R-r,R+r$. A noncentral chord would require an impact parameter and changes the inferred radii; the data alone do not fix that geometry exactly. For comparable masses in an ordinary coeval system, a component larger than its main sequence companion suggests expansion away from the main sequence, conventionally toward a subgiant/early giant track. That is a conditional evolutionary interpretation: neither effective temperature nor a bolometric flux is supplied, so a unique position on the Hertzsprung-Russell diagram cannot be inferred from these radii alone. Binary interactions and the assumed central chord also matter; these numbers do not establish an ordinary single-star evolutionary model.