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R.T. Zavala, B.J. McNamara, J. Galvan, T.E. Harrison, O. Mireles, E. Silvave (NMSU)
Photometrically determined spectral types of Algol secondaries may be found from the temperature of the primary and the ratio of surface brightness of the stellar components using light curve analysis. These photometrically derived spectral classifications have been found to be systematically later than those determined directly by spectroscopic spectral typing (Yoon et al., PASP 106, 239). Modeling of complete BVRI orbital light curves allows a determination of binary inclination, and stellar radii as well as spectral types. Luminosity class cannot be determined from spectroscopy of the secondaries during eclipse. Photometric light curve solutions are therefore vital additions to spectroscopic observations of Algols. However, photometric monitoring with sufficient phase resolution and coverage to allow photometric modeling of binaries with several day periods requires many nights of observation. Fortunately, a number of these binaries are bright, allowing such a program to be performed with modest equipment. We present results of BVRI monitoring of the Algol binary WW Cyg from 1997 to 1998. A period of 3.3178 days is determined for this system in agreement with past determinations with no evidence for a substantial change in period. An O-C curve for WW Cyg shall be presented. Data shall also be presented for the Algol binaries X Tri and RV Psc. The observations were made using the New Mexico State University Clyde Tombaugh Campus Observatory 16 inch Meade telescope with an SBIG ST-8 CCD camera and Johnson BVRI filters. . We have used "Binary Maker 2.0" by D. Bradstreet to model our photometric data.