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The Culgoora Magnetograph

Published online by Cambridge University Press:  14 August 2015

J. V. Ramsay ,
R. G. Giovanelli  and
H. R. Gillett
J. V. Ramsay
Affiliation:
CSIRO Division of Physics, National Standards Laboratory, Sydney, Australia 2008
R. G. Giovanelli
Affiliation:
CSIRO Division of Physics, National Standards Laboratory, Sydney, Australia 2008
H. R. Gillett
Affiliation:
CSIRO Division of Physics, National Standards Laboratory, Sydney, Australia 2008

Abstract

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The magnetograph is based on a high-resolution filter which serves in place of a spectrograph, except that a reasonably large field of view (one-quarter of the Sun's diameter) can be observed at the one instant. Observations are made by obtaining filtergrams of opposite circular polarizations simultaneously in the wing of a magnetically sensitive line. Exposure times are about 0.3 s, the angular resolution of the magnetic field is about 2 arc s, closest frame repetition rates about 8 s. The filtergrams are processed subsequently by photographic or television subtraction. Semiautomatic photographic and/or TV subtractions yield magnetograms suitable for cinematographic projection though the subtractions are not yet as perfect as those obtained by individual subtraction.

Type
Part I: Instrumentation – Measurement Fields in the Solar Atmosphere
Information
Symposium - International Astronomical Union , Volume 43: Solar Magnetic Fields , 1971 , pp. 24 - 29
Copyright
Copyright © Reidel 1971 

References

Leighton, R. B.: 1959, Astrophys. J. 130, 366.Google Scholar
Ramsay, J. V., Kobler, H., and Mugridge, E. G. V.: 1970, Solar Phys. 12, 492.Google Scholar
Steel, W. H., Giovanelli, R. G., and Smartt, R. N.: 1961, Australian J. Phys. 14, 201.CrossRefGoogle Scholar