  Phenomenological characteristics of the sample of the Algol-type stars are
revised using a recently developed NAV ("New Algol Variable") algorithm
(2012Ap.....55..536A, 2012arXiv 1212.6707A) and compared to that obtained using
common methods of Trigonometric Polynomial Fit (TP) or local Algebraic
Polynomial (A) fit of a fixed or (alternately) statistically optimal degree
(1994OAP.....7...49A, 2003ASPC..292..391A). The computer program NAV is
introduced, which allows to determine the best fit with 7 "linear" and 5
"non-linear" parameters and their error estimates. The number of parameters is
much smaller than for the TP fit (typically 20-40, depending on the width of
the eclipse, and is much smaller (5-20) for the W UMa and beta Lyrae - type
stars. This causes more smooth approximation taking into account the reflection
and ellipsoidal effects (TP2) and generally different shapes of the primary and
secondary eclipses. An application of the method to two-color CCD photometry to
the recently discovered eclipsing variable 2MASS J18024395 + 4003309 = VSX
J180243.9 +400331 (2015JASS...32..101A) allowed to make estimates of the
physical parameters of the binary system based on the phenomenological
parameters of the light curve. The phenomenological parameters of the light
curves were determined for the sample of newly discovered EA and EW - type
stars (VSX J223429.3+552903, VSX J223421.4+553013, VSX J223416.2+553424,
US-NO-B1.0 1347-0483658, UCAC3-191-085589, VSX J180755.6+074711= UCAC3
196-166827). Despite we have used original observations published by the
discoverers, the accuracy estimates of the period using the NAV method are
typically better than the original ones.
