EDP Sciences
Free Access
Volume 375, Number 3, September 2001
Page(s) 989 - 998
Section Formation, structure and evolution of stars
DOI https://doi.org/10.1051/0004-6361:20010915

A&A 375, 989-998 (2001)
DOI: 10.1051/0004-6361:20010915

The formation and evolution of binary systems

III. Low-mass binaries in the Praesepe cluster
J. Bouvier1, G. Duchêne1, 2, J.-C. Mermilliod3 and T. Simon4

1  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

(Received 3 April 2001 / 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 $\log P$ (days) range from 4.4 to 6.9 of $25.3 \pm 5.4$% , which is similar to that of field G-type dwarfs (23.8% , Duquennoy & Mayor 1991). 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

Offprint request: J. Bouvier, jbouvier@laog.obs.ujf-grenoble.fr

SIMBAD Objects
Tables at the CDS

© ESO 2001

Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.

Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.

Initial download of the metrics may take a while.