  We show how the assumption of coeval formation can be used to constrain the
effective temperatures of the components of young eclipsing double-lined
spectroscopic binaries. Our method extends the approach of White et al. (1999)
to a two-step analysis. The first step compares evolutionary models to the
observed masses and radii and selects those models that predict ages that are
consistent with coeval formation. The second step then uses these models to
constrain the effective temperatures. We applied the method on literature
values of the stellar parameters of the eclipsing binaries RX J0529.4+0041 A
and V1174 Ori and confirm that V1174 Ori A has dwarf-like temperatures at an
age of 9 Myrs, while we cannot draw any conclusions for RX J0529.4+0041 A and
V1174 Ori B. Considering these binaries, we find that none of the evolutionary
models gives coeval solutions simultaneously in mass, radius and effective
temperature.
