Abstract
High-dispersion spectrograms are used to derive the distribution of rotational velocities for a sample of 256 late B-type stars. Approximately half the stars have sharp lines (upsilon sini<100 km s/sup -1/), and a statistical treatment of the data shows that the distribution of true rotational velocities psi (upsilon) reaches a maximum in the velocity interval 300.1 is marginally higher among the HgMn stars (31%) than among normal B-type stars (19%) in the same temperature range, probably because slow rotation, which is characteristic of such binaries, favors the appearance of HgMn anomalies. However, the majority of HgMn stars are single, and their slow rotation cannot be attributed to tidal interactions. The HgMn stars are single, and their slow rotation cannot be attributed to tidal interactions. The HgMn stars are found throughout the main-sequence band from the zero- to the terminal age main sequence. The present observations show that HgMn stars are not distinguished from normal ones by their age, duplicity, rotation, or any combination of these characteristics.
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