Radial velocities and line profiles from spectrograms of the eclipsing WR binary star CQ Cephei are reported. Model stars and brightness ratios in the V band are used to obtain an internally consistent model for the system. The WR star appears to be a hydrogen-burning star with M(WR) = 13.6 solar masses, R(WR) = 5.5 solar radii, and T(eff) = 29,000 K, while the companion star has M(comp) = 16.0 solar masses, R(comp) = 6.4 solar radii, and T(eff) = 30,800 K. It is probably a B0 star. The sizes of the orbits are a(WR) = 9.7 solar radii and a(comp) = 8.2 solar radii. The complex shortward-displaced absorption components of He 5876 A indicate that the stars are buried in several streams of plasma.
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Underhill et al. (1990) studied this question.