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1 Introduction

The behaviour of orbital periods of early-type binaries is still very little known; in some cases, perhaps shallow minima or long periods make these variables not much attractive for observers. Nevertheless, interesting results were obtained for this type of binaries - e.g., in several cases, light-time effect due to a third body, or variations of O-C values significantly larger than measuring errors were found. Some of the present authors have already discussed the subject (Mayer 1980, 1987; Mayer et al. 1991, hereafter MWTN). In this note we give newly measured times of minima for six variables and also discuss the periods in cases where more data are available. The stars selected are those with a longer observing history among the OB eclipsing binaries; they are also included in our program to determine absolute dimensions and evolutionary properties of such systems. The only exception, AQ Cir, is a candidate to be included in the program.

Table 1: Observed times of minima

Variable & HJD$-$2400000 & m.e. & Epoch & O$-$C...
 ...& 49913.4785 & .0010 & 6947 & .0285 & .0019 &
Ond\v{r}ejov\\ \hline\end{tabular}

a phase in the third-body orbit.

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