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Angular Diameters and Effective Temperatures of Some Bright Stars

Published online by Cambridge University Press:  25 April 2016

R. Hanbury Brown
R. Hanbury Brown*
Affiliation:
Chatterton Astronomy Department, University of Sydney
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Extract

The Stellar Interferometer at Narrabri Observatory consists of two large reflectors which focus the light from a star on to two photoelectric detectors. The output currents from these detectors contain fluctuations which correspond to fluctuations in the starlight itself. The fluctuations from the two detectors are amplified in the frequency range 10-100 Mc/s and their correlation is measured by a linear multiplier. This correlation is measured as a function of the separation between the two detectors. It can be shown theoretically that the correlation at any given baseline is proportional to the square of the fringe visibility which would be observed by a classical Michelson interferometer. It is therefore possible from observations of the correlation at different baselines to find the angular diameter of a star.

Type
Invited Papers
Information
Publications of the Astronomical Society of Australia , Volume 1 , Issue 1 , January 1967 , pp. 7 - 8
Copyright
Copyright © Astronomical Society of Australia 1967

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References

1 Hanbury Brown, R., and Browne, A., Philips Tech. Rev., 27, 141 (1966).Google Scholar
2 Mihalas, D., Ap. J. Supplement No. 114, 13, 1–30 (1966).CrossRefGoogle Scholar
3 Harris, D. L., in ‘Stars and Stellar Systems’, Vol 3: ‘Basic Astronomical Data’ (Ed K. Aa. Strand), Ch 14, Chicago, 1963.Google Scholar