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AH Cep and CW Cep are both early B-type binaries with short orbital periodsof 1.8~d and 2.7~d, respectively. All four components are B0.5V types. Thebinaries are also double-lined spectroscopic and eclipsing. Consequently,solutions for orbital and stellar parameters make the pair of binaries idealtargets for a study of the colliding winds between two B~stars. {\em Chandra}ACIS-I observations were obtained to determine X-ray luminosities. AH~Cep wasdetected with an unabsorbed X-ray luminosity at a 90\% confidence interval of$(9-33)\times 10^{30}$ erg s$^{-1}$, or $(0.5-1.7)\times 10^{-7} L_{\rm Bol}$,relative to the combined Bolometric luminosities of the two components. Whileformally consistent with expectations for embedded wind shocks, or binary windcollision, the near-twin system of CW~Cep was a surprising non-detection. ForCW~Cep, an upper limit was determined with $L_X/L_{\rm Bol} < 10^{-8}$, againfor the combined components. One difference between these two systems is thatAH~Cep is part of a multiple system. The X-rays from AH~Cep may not arise fromstandard wind shocks nor wind collision, but perhaps instead from magnetism inany one of the four components of the system. The possibility could be testedby searching for cyclic X-ray variability in AH~Cep on the short orbital periodof the inner B~stars.

An X-ray Study of Two B+B Binaries: AH Cep and CW Cep