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A Survey of Young Stars in Taurus for Multiplicity

Published online by Cambridge University Press:  12 April 2016

Ch. Leinert ,
N. Weitzel ,
M. Haas ,
R. Lenzen ,
H. Zinnecker ,
J. Christou ,
S.T. Ridgway ,
R. Jameson  and
A. Richichi
Ch. Leinert
Affiliation:
Max-Planck-Institut für Astronomie, Königstuhl, D-6900 Heidelberg 1, Germany
N. Weitzel
Affiliation:
Max-Planck-Institut für Astronomie, Königstuhl, D-6900 Heidelberg 1, Germany
M. Haas
Affiliation:
Max-Planck-Institut für Astronomie, Königstuhl, D-6900 Heidelberg 1, Germany
R. Lenzen
Affiliation:
Max-Planck-Institut für Astronomie, Königstuhl, D-6900 Heidelberg 1, Germany
H. Zinnecker
Affiliation:
Institut für Astronomie und Astrophysik der Universität Würzburg, Am Hubland, D-8700, Würzburg, Germany
J. Christou
Affiliation:
Steward Observatory, University of Arizona, Tucson AZ, 85721, USA
S.T. Ridgway
Affiliation:
National Optical Astronomy Observatories, P.O. Box 26732, Tucson AZ, 85726, USA
R. Jameson
Affiliation:
Astronomy Group, University of Leicester, University Road, Leicester LEI 7RH, England
A. Richichi
Affiliation:
Osservatorio Astrofisico di Arcetri, Largo Enrico Fermi 5, 1-50125 Firenze, Italy

Abstract

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We surveyed all stars in Taurus (3h 45m < α < 4h 15m, 15° < δ < 35°) for multiplicity which are contained in the Herbig-Bell catalogue of young stars and have a 2 micron brightness of K ≤ 9.5 mag. This sample consists of 106 stellar systems (single or multiple), of which 43 are double or multiple according to the criteria of our survey, i.e. with separations of ≈0″.2 ≤ d ≤ 10″. Of these, 23 binaries are new detections found in this survey. The resulting degree of multiplicity, 43/106 = 41±6%, is higher than found for main-sequence stars. Provided that the period distribution is the same for young stars as on the main sequence, our result implies that the vast majority of stars are born in binary or multiple systems.

Type
Pre-Main Sequence & Young Binaries
Information
International Astronomical Union Colloquium , Volume 135: Complementary Approaches to Double and Multiple Star Research , 1992 , pp. 21 - 29
Copyright
Copyright © Astronomical Society of the Pacific 1992

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