|Authors||Pavel Kroupa 1, Sverre Aarseth 2 and Jarrod Hurley 2|
|Affiliation||1 University of Kiel,|
2 University of Cambridge
|Accepted by||Monthly Notices of the Royal Astronomical Society|
|Links||Orion Nebula Cluster / Pleiades Cluster|
The results have wide implications, also for the formation of globular clusters and the Galactic field and halo stellar populations. In view of this, the distribution of binary orbital periods and the mass function within and outside the model ONC and Pleiades is quantified, finding consistency with observational constraints. Advanced mass segregation is evident in one of the ONC models. The calculations show that the primordial binary population of both clusters could have been much the same as is observed in the Taurus--Auriga star forming region. The computations also demonstrate that the binary proportion of brown dwarfs is depleted significantly for all periods, whereas massive stars attain a high binary fraction.