Short‐Period Variable Be Stars Discovered or Confirmed through Self‐Correlation Analysis ofHipparcosEpoch Photometry

We have surveyed 277 bright Be stars for short‐period (0.2–2 day) photometric variability using self‐correlation analysis ofHipparcosepoch photometry. This extends the work of Percy et al.; the methods are as described there. We report the discovery, timescale, and amplitude of short‐period variability in: HD 7636 (V764 Cas), HD 11606 (V777 Cas), HD 13661 (V549 Per), HD 34921, HD 36408, HD 40978, HD 58343 (FW CMa), HD 63460 (o Pup), HD 88195 (17 Sex), HD 89353 (AG Ant, HR 4049), HD 129954 (CO Cir), HD 158220 (V862 Ara), HD 173219 (V947 Sct), and HD 187567 (V1339 Aql). We report the confirmation of short‐period variability using an independent form of analysis in HD 52918 (19 Mon), HD 105382 (V863 Cen), HD 137387 (κ‐1 Aps), HD 157832 (V750 Ara), and HD 163868 (V3984 Sgr). These include a β Cephei star (19 Mon), a Vega‐type star (17 Sex), and a post‐asymptotic giant branch B star (HR 4049). We find that short‐period variability is more prevalent in early‐B stars than in late‐B stars. We have found no β Cephei type variables in our sample of Be stars, other than 19 Mon, which is apparently not a Be star.