Rotation in the ZAMS: Be and Bn stars
  We show that Be stars belong to a high velocity tail of a single B-type star rotational velocity distribution in the MS. This implies that: 1) the number fraction N(Be)/N(Be+B) is independent of the mass; 2) Bn stars having ZAMS rotational velocities higher than a given limit might become Be stars. 
J. Zorec (IAP), Y. Fr\'emat (ROB), C. Martayan (GEPI), L. Cidale   (UNLP), A. Torres (UNLP)