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The Potential of Long–Baseline Optical Interferometry of Binary Stars

Published online by Cambridge University Press:  12 April 2016

H.A. McAlister
H.A. McAlister*
Affiliation:
Center for High Angular Resolution Astronomy, Georgia State University, Atlanta, GA, 30303, USA

Abstract

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Interferometric arrays possessing sub-milliarcsecond resolution are either about to be fully scientifically productive, as in the case of the Sydney University Stellar Interferometer, or are under various stages of planning and development. The 1990’s will thus witness a hundred–fold gain in resolution over speckle interferometry at the largest telescopes and 5,000 times the resolution of classical direct imaging. Where speckle interferometry can now resolve binary stars with periods of 1 to 2 years, interferometric arrays with baselines of hundreds of meters will resolve binaries with periods of a few hours. Arrays will resolve the majority of the known spectroscopic binaries, providing a substantial increase in the quantity and quality of stellar mass determinations. Surveys for new binaries among the field stars and other restricted samples will be accomplished with unprecedented completeness. The remarkable enhancement in resolution we are about to witness from facilities like SUSI and our own proposed CHARA Array will quite literally revolutionize the field of double and multiple star research.

Type
High Resolution At Visual Wavelengths
Information
International Astronomical Union Colloquium , Volume 135: Complementary Approaches to Double and Multiple Star Research , 1992 , pp. 527 - 535
Copyright
Copyright © Astronomical Society of the Pacific 1992

References

Andersen, J. 1991, A&AR, 3, 91 Google Scholar
Batten, A.H., Fletcher, J.M., and Mann, P.J. 1978, Pub. Dominion Astrophys. Obs., 15, No. 5 Google Scholar
Cole, W.A., Fekel, F.C., Hartkopf, W.I., McAlister, H.A., & Tomkin, J. 1992, AJ, 103, 1357 CrossRefGoogle Scholar
Halbwachs, J.L. 1981, A&AS, 44, 47 Google Scholar
Harrington, R.S. 1977, AJ, 82, 753 Google Scholar
Heintz, W.D. 1985, IAU Symposium No. 1ll, Calibration of Fundamental Stellar Quantities, eds. Hayes, D.S., Pasinetti, L.E. and Davis Phillip, A.G. (Reidel, Dordrecht) p. 71 Google Scholar
Herbison–Evans, D., Hanbury Brown, R., Davis, J., & Allen, L.R. 1971, MNRAS, 151, 161 Google Scholar
Popper, D.M. 1980, ARA&A, 18, 115 Google Scholar
Popper, D.M. 1985, IAU Symposium No. 1ll, Calibration of Fundamental Stellar Quantities, eds. Hayes, D.S., Pasinetti, L.E., and Davis Phillip, A.G. (Reidel, Dordrecht) p. 81 Google Scholar
Thompson, R.J. 1976, Ph.D. dissertation, University of SydneyGoogle Scholar