  We describe an automated method for assigning the most probable physical
parameters to the components of an eclipsing binary, using only its photometric
light curve and combined colors. With traditional methods, one attempts to
optimize a multi-parameter model over many iterations, so as to minimize the
chi-squared value. We suggest an alternative method, where one selects pairs of
coeval stars from a set of theoretical stellar models, and compares their
simulated light curves and combined colors with the observations. This approach
greatly reduces the parameter space over which one needs to search, and allows
one to estimate the components' masses, radii and absolute magnitudes, without
spectroscopic data. We have implemented this method in an automated program
using published theoretical isochrones and limb-darkening coefficients. Since
it is easy to automate, this method lends itself to systematic analyses of
datasets consisting of photometric time series of large numbers of stars, such
as those produced by OGLE, MACHO, TrES, HAT, and many others surveys.
