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The late-type Be star $\beta$ CMi is remarkably stable compared to other Bestars that have been studied. This has led to a realistic model of theoutflowing Be disk by Klement et al. These results showed that the disk islikely truncated at a finite radius from the star, which Klement et al.~suggestis evidence for an unseen binary companion in orbit. Here we report on ananalysis of the Ritter Observatory spectroscopic archive of $\beta$ CMi tosearch for evidence of the elusive companion. We detect periodic Doppler shiftsin the wings of the H$\alpha$ line with a period of 170 d and an amplitude of2.25 km s$^{-1}$, consistent with a low-mass binary companion ($M\approx 0.42M_\odot$). We then compared the small changes in the violet-to-red peak heightchanges ($V/R$) with the orbital motion. We find weak evidence that it doesfollow the orbital motion, as suggested by recent Be binary models by Panoglouet al. Our results, which are similar to those for several other Be stars,suggest that $\beta$ CMi may be a product of binary evolution where Roche lobeoverflow has spun up the current Be star, likely leaving a hot subdwarf orwhite dwarf in orbit around the star. Unfortunately, no direct sign of thiscompanion star is found in the very limited archive of {\it InternationalUltraviolet Explorer} spectra.

A Spectroscopic Orbit for the late-type Be star $\beta$ CMi