Abstract
Projected rotational velocities, v sin i, have been determined for 40 component stars in 29 early-type binary systems in order to study the state of axial-orbital synchronism. Most of the systems are eclipsing binaries with periods between one and six days and hot components in the range from O9 to F0. Calibrated 20 Â/mm spectrograms were obtained with the X-spectrograph and the 60inch Mount Wilson reflector. Direct-intensity tracings of these spectrograms were made with the microphotometer and digitizer of the University of Illinois Observatory. The intensity linearization and plotting was done by computer, using a program developed by Yoss (1966). Rotational velocities were determined using the method described by Huang and Struve (1960). Profiles of lines observed in slowly-rotating stars were numerically broadened with the well-known broadening function, and the relations between usini and the total half-width obtained. Half -widths measured
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