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The Use of Fabry-Perot Filters for Spectral Scanning

Published online by Cambridge University Press:  25 April 2016

M. D. Waterworth
M. D. Waterworth*
Affiliation:
Department of Physics, University of Tasmania
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Extract

In designing a stellar spectrograph, it is pointless to exceed the resolving power necessary to obtain all the information from the spectrum of a star. This is limited mainly by atomic thermal motions, giving rise to the Doppler broadening of spectral lines, by turbulence and rotation of the stellar atmospheres in which the lines are formed, and by collisional broadening.

Type
Contributions
Information
Publications of the Astronomical Society of Australia , Volume 1 , Issue 6 , September 1969 , pp. 293 - 294
Copyright
Copyright © Astronomical Society of Australia 1969

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References

1 Dunham, T. Jr., Vistas in Astronomy, Vol. 2, Pergamon, Oxford 1956.Google Scholar
2 Ramsay, J. V., and Mudgridge, E. G. V., J.Sci. Instr., 39, 636 (1962).Google Scholar
3 Ring, J., Astronomical Optics, (ed.) Kopal, Z., p: 381, 1956.Google Scholar
4 Ramsay, J. V., Applied Optics, 1, 4 (1962).Google Scholar