|Authors||J. Bouvier1, G. Duchêne1, 2, J.-C. Mermilliod3, T. Simon4|
|Affiliation||1 Laboratoire d'Astrophysique, Observatoire de Grenoble, Univ. J. Fourier, B.P. 53, 38041 Grenoble Cedex 9, France|
2 UCLA Division of Astronomy and Astrophysics, Los Angeles, CA 90095-1562, USA
3 Institut d'Astronomie de l'Université de Lausanne, CH-1290 Chavannes-des-Bois, Switzerland
4 Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822, USA
|Accepted by||Astronomy & Astrophysics|
We compare the distribution of cluster binaries to the binary populations of star forming regions, most notably Orion and Taurus, to critically review current ideas regarding the binary formation process. We conclude that it is still unclear whether the lower binary fraction observed in young clusters compared to T associations is purely the result of the early dynamical disruption of primordial binaries in dense clusters or whether it reflects intrinsically different modes of star formation in clusters and associations. We also note that if Taurus binaries result from the dynamical decay of small-N protostellar aggregates, one would predict the existence of a yet to be found dispersed population of mostly single substellar objects in the Taurus cloud.