Astron. Astrophys. 323, 139-150 (1997)

Pleiades low-mass binaries: do companions affect the evolution of protoplanetary disks? ^{* **}

J. Bouvier ^{1, 2}, F. Rigaut ² and D. Nadeau <sup>3

1</sup> Laboratoire d'Astrophysique, Observatoire de Grenoble, Université Joseph Fourier, B.P. 53, F-38041 Grenoble Cedex 9, France (bouvier@gag.observ-gr.fr)
² Canada-France-Hawaii Telescope Corporation, P.O. Box 1597, Kamuela, HI 96743, USA (rigaut@cfht.hawaii.edu)
³ Observatoire du Mont Mégantic et Département de Physique, Université de Montréal, C.P. 6128, Succ. A, Montréal, QC, H3C 3J7, Canada (nadeaud@ere.umontreal.ca)

Received 3 December 1996 / Accepted 3 January 1997

Abstract

We have observed 144 G and K dwarf members of the Pleiades cluster to search for close multiple systems using CFHT's Adaptive Optics adaptor in the near-IR. We detected 22 binary systems and 3 triples, with a separation between 0.08 and 6.9 arcsec (11-910 AU). After correction for incompleteness, we derive a binary frequency in the orbital period range from 4.2 to 7.1 log days, of 28 4% for G and K Pleiades dwarfs, similar to that of field G-type dwarfs (27%). The distributions of both orbital periods and mass-ratios of the Pleiades systems also appear similar to those of G dwarf binaries of the field. The binary frequency in the 100 Myr-old Pleiades cluster is much lower than that observed for Myr-old pre-main sequence (PMS) stars in the Taurus-Auriga cloud. We argue that this difference does not result from the evolution of the binary systems during the pre-main sequence. Instead, we suggest that the low Pleiades binary frequency is typical of stellar populations formed in dense protoclusters, while the higher binary frequency observed among Tau-Aur PMS stars is more typical of loose T associations. The implication is that most field stars are born in dense protostellar clusters.

All 144 surveyed stars have known rotational velocities. Based on the current beliefs that i) the rotation rate of Pleiades late-type dwarfs is largely dictated by the lifetime of their pre-main sequence circumstellar disks and that ii) the evolution of the disks is affected by the presence of a close companion, we searched for a relationship between rotational velocity and binarity among Pleiades G and K dwarfs. We find no significant difference between the distribution of rotational velocities of single and binary stars. Unless current models of PMS angular momentum evolution are flawed, this indicates that the presence of a companion within a distance of 10-1000 AU does not prevent accretion from occurring onto the primary at a rate similar to that observed for single PMS stars. For the closest systems, this implies that accretion must proceed from the circumbinary disk onto the central stars. For slightly wider systems, it suggests that the truncated circumstellar disks of the primary and of the secondary are fed by an external (circumbinary) reservoir of mass.

Key words: stars: binaries: close stars: formation stars: pre-main sequence stars: rotation Galaxy: open clusters and associations: Pleiades (Melotte 22) circumstellar matter

* Based on observations obtained at the Canada-France-Hawaii Telescope.
** Table 3 is only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/Abstract.html

Send offprint requests to: J. Bouvier

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Contents

• 1. Introduction
• 2. Observations and data reduction
• 3. Results
  • 3.1. Binary frequency
  • 3.2. Binarity and rotation
• 4. Discussion
  • 4.1. Comparison with previous photometric and spectroscopic studies
  • 4.2. The formation and evolution of young multiple systems
  • 4.3. Binarity, rotation and the lifetime of circumstellar disks
• 5. Conclusion
• Acknowledgements
• References

© European Southern Observatory (ESO) 1997

Online publication: June 5, 1998

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