The projected ellipticities and orientations of 11 young massive clust
ers in the Andromeda galaxy have been determined by using isodensity c
ontours and 2D Gaussian fitting techniques. One to five B plates taken
with the 2 m Ritchey-Chretien reflector of the Bulgarian National Ast
ronomical Observatory were digitized and processed for each blue clust
er. The derived ellipticities show that the blue massive disk clusters
are significantly more flattened than the true globulars in M 31. The
re is a statistically significant difference between the frequency dis
tributions of the ellipticities of blue clusters and true globulars. A
ccording to the evolutionary scenario of Shapiro and Marchant (1976) t
his means that the blue massive clusters are dynamically younger than
the others. There seems to be a tendency of grouping of the blue clust
ers in two relatively compact regions along the spirals of M 31, very
close to the star forming regions observed there.