Comparative Studies of Young Open Clusters - Part Two - an Atlas of Composite Colour-Magnitude Diagrams

Details Comparative Studies of Young Open Clusters - Part Two - an Atlas of Composite Colour-Magnitude Diagrams Comparative Studies of Young Open Clusters - Part Two - an Atlas of Composite Colour-Magnitude Diagrams

Jun 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981a%26as...44..467m&link_type=abstract

Astronomy and Astrophysics Supplement, Vol. 44, P. 467, 1981

Astronomy and Astrophysics

Astrophysics

135

Scientific paper

75 young open clusters, with ages between those of the Hyades and NGC 6231, have been divided into 14 age groups according to the morphology of their MV vs. (U-B)0 diagrams. New estimations of the colour excesses and distances have been obtained after a careful analysis of the photometric data and of membership. Composite MV vs. (B-V)0 and MV vs. (U-B)0 diagrams have been formed by superimposition of 4 to 8 clusters per group. look much like individual clusters, owing to the small age intervals considered. However the main sequence in the MV vs. (U-B)0 composite diagram of the NGC 2516 age group is unusually dispersed. This fact may be related to the existence of the B7-B8 gap, since the turn-up temperature corresponds to the gap temperature.
The analysis of the stellar content resulted in forming tables which indicate in which age group evolved, variable and abnormal stars are to be found or looked for.
In a preliminary discussion of the stellar content, it is shown that blue stragglers are also present in young open clusters. Be stars are found to be most abundant in young clusters with turn-up types between B0.5 and B2. Other concentrations of Be stars, such as in the Pleiades are group, lead one to think that a high rotational velocity is not a sufficient condition, although a necessary one, for the presence of the Be phenomenon.

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