We present a photometric and spectroscopic study of AzV322 , an emission line object located in the Small Magellanic Cloud previously classified between O9 and B0 . We analyze 17.5 years of I and V band OGLE-II , III and IV light curves and find four significant frequencies , viz . f _ { 1 } = 0.386549 \pm 0.000003 , f _ { 2 } = 0.101177 \pm 0.000005 , f _ { 3 } = 0.487726 \pm 0.000015 and f _ { 4 } = 0.874302 \pm 0.000020 c/d . The f _ { 1 } frequency ( period 2 \aas@@fstack { d } 58700 \pm 0 \aas@@fstack { d } 00002 ) provides the stronger periodogram peak and gives a single wave light curve of full amplitude 0.066 mag in the I -band . High-resolution optical spectroscopy confirms the early B-type spectral type and reveals prominent double peak Balmer , Paschen , OI 8446 and He I 5875 emissions . The spectral energy distribution shows significant color excess towards long wavelengths possibly attributed to free-free emission in a disk-like envelope . Our analysis yields T _ { eff } = 23 000 \pm 1500 K , log g = 3.0 \pm 0.5 , M = 16 \pm 1 M _ { \odot } , R = 31.0 \pm 1.1 R _ { \odot } , and L _ { bol } = 10 ^ { 4.87 \pm 0.06 } L _ { \odot } . AzV322 might be a member of the new class of slowly pulsating B supergiants introduced by Saio et al . ( 28 ) and documented by Lefever , Puls , & Aerts ( 16 ) , however its circumstellar disk make it an hitherto unique object . Furthermore , we notice that a O-C analysis for f _ { 1 } reveals quasi-cyclic changes for the times of maximum in a time scale of 20 years which might indicate a light-travel time effect in a very wide orbit binary with an undetected stellar component .