  We present a preliminary statistical analysis of a period change of eclipsing
binaries from the ASAS Catalog of Variable Stars. For each contact and
semidetached system brighter than 13.3$mag$ (in V) with a period shorter than
0.4 days and at least 300 observation points we have found an angular velocity
$\omega$ and its time derivative $\frac{d\omega}{dt}$. According to our
accuracy there is no evidence that average $\frac{d\omega}{dt}$ differs from 0.
Light curves for selected stars are presented.
