  Phenomenological modeling of variable stars allows determination of a set of
the parameters, which are needed for classification in the "General Catalogue
of Variable Stars" and similar catalogs. We apply a recent method NAV ("New
Algol Variable") to eclipsing binary stars of different types. Although all
periodic functions may be represented as Fourier series with an infinite number
of coefficients, this is impossible for a finite number of the observations.
Thus one may use a restricted Fourier series, i.e. a trigonometric polynomial
(TP) of order s either for fitting the light curve, or to make a periodogram
analysis. However, the number of parameters needed drastically increases with
decreasing width of minimum. In the NAV algorithm, the special shape of minimum
is used, so the number of parameters is limited to 10 (if the period and
initial epoch are fixed) or 12 (not fixed). We illustrate the NAV method by
application to a recently discovered Algol-type eclipsing variable 2MASS
J11080308-6145589 (in the field of previously known variable star RS Car) and
compare results to that obtained using the TP fits. For this system, the
statistically optimal number of parameters is 44, but the fit is still worse
than that of the NAV fit. Application to the system GSC 3692-00624 argues that
the NAV fit is better than the TP one even for the case of EW-type stars with
much wider eclipses. Model parameters are listed.
