Hostname: page-component-78c5997874-8bhkd Total loading time: 0 Render date: 2024-11-05T15:29:07.197Z Has data issue: false hasContentIssue false
  • English
  • Français

Pre-main sequence multiple systems

Published online by Cambridge University Press:  27 April 2011

Hervé Bouy
Hervé Bouy*
Affiliation:
Centro de Astrobiologia, INTA-CSIC, P.O. Box - Apdo. de correos 78, Villanueva de la Cañada Madrid 28691, Spain email: [email protected]
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

It is now well established that the majority of young stars are found in multiple systems, so that any theory of stellar formation must account for their existence and properties. Studying the properties of multiple star systems therefore represents a very powerful approach to place observational constraints on star formation theories. Additionally, multiple systems offer other advantages. They provide the most accurate and unambiguous way to measure masses, using orbital fitting and Kepler's laws, and even the stellar radius in the special case of eclipsing binaries. They also allow to compare the properties of 2 coeval objects with different masses, providing important tests for the evolutionary models.

Keywords

Stars: binaries: generalStars: formation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S270: Computational Star Formation , May 2010 , pp. 41 - 44
Copyright
Copyright © International Astronomical Union 2011

References

Basri, G. & Reiners, A. 2006, AJ, 132, 663CrossRefGoogle Scholar
Bouy, H., Brandner, W., Martín, E. L., Delfosse, X., Allard, F., & Basri, G. 2003, AJ, 126, 1526CrossRefGoogle Scholar
Bouy, H., Martín, E. L., Brandner, W., Zapatero-Osorio, M. R., Béjar, V. J. S., Schirmer, M., Huélamo, N., & Ghez, A. M. 2006, A&A, 451, 177Google Scholar
Burgasser, Adam J., Kirkpatrick, J. Davy, Reid, I. Neill, Brown, Michael E., Miskey, Cherie L., Gizis, , & John, E. 2003, ApJ, 586, 512CrossRefGoogle Scholar
Connelley, Michael S., Reipurth, Bo, Tokunaga, , & Alan, T. 2008, AJ, 135, 2526CrossRefGoogle Scholar
Duquennoy, A. & Mayor, M. 1991, A&A, 248, 485Google Scholar
Fisher, D. & Marcy, G. 1992, ApJ, 396, 178CrossRefGoogle Scholar
Goldman, B., Bouy, H., Zapatero Osorio, M. R., Stumpf, M. B., Brandner, W., Henning, T. 2008, A&A, 490, 763Google Scholar
Joergens, V. 2006, A&A, 448, 655Google Scholar
Lafrenière, David, Jayawardhana, Ray, Brandeker, Alexis, Ahmic, Mirza, van, Kerkwijk, & Marten, H. 2008, ApJ, 643, 844CrossRefGoogle Scholar
Leinert, C., Henry, T., Glindemann, A., & McCarthy, D. W. Jr. 1997, AJ, 325, 159Google Scholar
MaízApellániz, J. Apellániz, J. 2010, A&A, arXiv:1004.5045Google Scholar
Mason, Brian D., Hartkopf, William I., Gies, Douglas R., Henry, Todd J.; Helsel, , & John, W. 2009, AJ, 137, 3358CrossRefGoogle Scholar
Maxted, P. F. L. & Jeffries, R. D. 2005, MNRAS, 362, 45CrossRefGoogle Scholar
Reid, I. N. & Gizis, J. 1997, AJ, 114, 1992CrossRefGoogle Scholar
Siegler, Nick, Close, Laird M., Cruz, Kelle L., Martín, Eduardo L., Reid, , & Neill, I. 2005, ApJ, 621, 1023CrossRefGoogle Scholar
Tokovinin, A. A. & Smekhov, M. G 2002, A&A, 382, 118Google Scholar