Volume 375, Number 3, September 2001
|Page(s)||989 - 998|
|Section||Interstellar and circumstellar matter|
|Published online||15 September 2001|
The formation and evolution of binary systems*
III. Low-mass binaries in the Praesepe cluster
Laboratoire d'Astrophysique, Observatoire de Grenoble, Université Joseph Fourier, BP 53, 38041 Grenoble Cedex 9, France http://www-laog.obs.ujf-grenoble.fr/
2 UCLA Division of Astronomy and Astrophysics, Los Angeles, CA 90095-1562, USA
3 Institut d'Astronomie de l'Université de Lausanne, 1290 Chavannes-des-Bois, Switzerland
4 Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822, USA
Corresponding author: J. Bouvier, firstname.lastname@example.org
Accepted: 22 June 2001
With the aim of investigating the binary population of the 700 Myr old Praesepe cluster, we have observed 149 G and K-type cluster members using adaptive optics. We detected 26 binary systems with an angular separation ranging from less than 0.08 to 3.3 arcsec (15-600 AU). After correcting for detection biases, we derive a binary frequency (BF) in the (days) range from 4.4 to 6.9 of % , which is similar to that of field G-type dwarfs (23.8% , Duquennoy & Mayor [CITE]). This result, complemented by similar ones obtained for the 2 Myr old star forming cluster IC 348 (Paper II) and the 120 Myr old Pleiades open cluster (Paper I), indicates that the fraction of long-period binaries does not significantly evolve over the lifetime of galactic open clusters. 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.
Key words: stars: binaries: close / stars: formation / stars: low-mass, brown dwarfs / galaxy: open clusters and associations: individual: Praesepe, M 44
© ESO, 2001
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