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F. Tam (Stanford U. \& Maria Mitchell Obs.), N. Samus (Institute of Astronomy, Russia Ac.Sci. \& Maria Mitchell Obs.)
Several ``lost" variable stars previously discovered at the Maria Mitchell Observatory and at Harvard Observatory were reinvestigated. These variables had not been studied for decades, and accurate coordinates and light elements were unknown for them. We rediscovered these stars as variables using the MMO photographic plate collection, and further study was accomplished with both the MMO and the Moscow University plate collection. The stars were identified in positional catalogs and their light elements were improved based on new photographic estimates. Two types of variables were revealed: eclipsing binaries and miras. Two very interesting eclipsers were studied, VX Sct and V936 Aql. The former is characterized by a period exceeding one month, and thus it probably contains a giant component. V936 Aql shows a light curve characteristic of Algol variables with ellipsoidal components or \betaLyrae variables, with a distinct secondary minimum. However, it possesses a rather short period (0.48 days), more typical of W Ursae Majoris stars or cataclysmic variables. Of the six miras studied, AO Sct, AV Sct, and SW Sct had experienced period changes over the course of several decades. AV Sct actually underwent two period changes in 35 years. BI Sct has maintained its period since it was previously studied. The light elements and positions of CV Sgr and VV Sct were determined reliably for the first time.