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3 Vul is found to be a single-lined spectroscopic binary with a period of 367 days, very nearly equal to one year. Velocity observations over two decades, in combination with archival data, have produced sufficiently good phase coverage to yield a well-defined orbit. Nonetheless, residuals from a Keplerian velocity curve are larger than expected for the sharp-lined B6 III primary: Night-to-night and possibly more rapid non-Keplerian radial-velocity variations occur. High-resolution observations of Si II lines reveal marked line-profile changes during single and successive nights. Preliminary evidence suggests that low-amplitude photometric variations may be present also. It is suggested that the primary is a member of the nonradially pulsating "53 Persei" class of variable stars.

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