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What Causes the Low Binary Frequency in the Orion Nebula Cluster?

Published online by Cambridge University Press:  22 February 2018

R. Köhler
R. Köhler*
Affiliation:
MPI für Astronomie, Heidelberg, Germany

Abstract

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We report on the results of a binary survey in the outer parts of the Orion Nebula Cluster, 0.7 to 2 pc from the cluster center. The results should help to decide if the binary formation rate was lower in Orion than in Taurus-Auriga, or if many binaries formed initially, but were destroyed in close stellar encounters. We find that the binary frequency of low-mass stars does not depend on the distance to the cluster center. The companion star frequency of intermediate- to high-mass stars shows a trend to decrease with cluster radius, but the statistical significance of this trend is rather weak.

Resumen

Resumen

Reportamos los resultados de un censo de binarias en la parte externa del Cúmulo de la Nebulosa de Orión, entre 0.7 y 2 pc del centro del cúmulo. Los resultados serán útiles para decidir si la tasa de formación de binarias fue menor en Orión que en Taurus-Auriga, o si se formaron inicialmente muchas binarias que después fueron destruidas por encuentros estelares cercanos. Encontramos que la frecuencia de binarias entre estrellas de baja masa no depende de la distancia al centro del cúmulo. La frecuencia de compañeras para las estrellas de masa grande tiende a decrecer con el radio, pero el significado estadístico de esta tendencia es pequeño.

Keywords

BinariesVisual — InfraredStars — StarsPre-Main Sequence — TechniquesHigh Angular Resolution
Type
Observational Results for Very Young Binaries
Information
International Astronomical Union Colloquium , Volume 191: The Environment and Evolution of Double and Multiple Stars , August 2004 , pp. 104 - 108
Copyright
Copyright © Instituto de Astronomia – Mexico 2004

References

Bouvier, J., Rigaut, F., & Nadeau, D. 1997, A&A, 323, 139 Google Scholar
Duchêne, G. 1999, A&A, 341, 547 Google Scholar
Duchêne, G., Bouvier, J., & Simon, T. 1999, A&A, 343, 831 Google Scholar
Duquennoy, A., & Mayor, M. 1991, A&A, 248, 485 Google Scholar
Durisen, R.H., & Sterzik, M.F. 1994, A&A, 286, 84 Google Scholar
Ghez, A.M., Neugebauer, G., & Matthews, K. 1993, AJ, 106, 2005 CrossRefGoogle Scholar
Hillenbrand, L. A. 1997, AJ, 113, 1733 Google Scholar
Jones, B.F., & Walker, M.F. 1988, AJ, 95, 1755 Google Scholar
Kroupa, P. 1995, MNRAS, 277, 1491 CrossRefGoogle Scholar
Kroupa, P., Petr, M., & McCaughrean, M. 1999, New Astronomy Reviews, 4, 495 Google Scholar
Leinert, Ch., Zinnecker, H., Weitzel, N., Christou, J., Ridgway, S.T., Jameson, R., Haas, M., & Lenzen, R. 1993, A&A, 278, 129 Google Scholar
McCaughrean, M.J. 2001, in The Formation of BinaryStars, proc. IAU Symp. No. 200, eds. Zinnecker, H. & Mathieu, R.D. (San Francisco: ASP), 169 Google Scholar
Patience, J., Ghez, A.M., Reid, I.N., Weinberger, A.J., & Matthews, K. 1998, AJ, 115, 1972 Google Scholar
Petr, M.G. 1998, PhD Thesis, University of Heidelberg Google Scholar
Petr, M.G., Coudé du Foresto, V., Beckwith, S.V.W., Richichi, A., & McCaughrean, M.J. 1998, ApJ, 500, 825 Google Scholar
Prosser, C.F., Stauffer, J.R., Hartmann, L., Soderblom, D.R., Jones, B.F., Werner, M.W., & McCaughrean, M.J. 1994, ApJ, 421, 517 CrossRefGoogle Scholar
Wizinowich, P., Acton, D.S., Lai, O., Gathright, J., Lup-ton, W., & Stomski, P. 2000, Proc. SPIE, 4007, 2 Google Scholar