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Fabry-Pérot interferograms of the solar Mgii resonance lines

Published online by Cambridge University Press:  14 August 2015

B. Bates
Affiliation:
Department of Pure and Applied Physics, The Queen's University of Belfast, Belfast, N. Ireland
D. J. Bradley
Affiliation:
Department of Pure and Applied Physics, The Queen's University of Belfast, Belfast, N. Ireland
C. D. McKeith
Affiliation:
Department of Pure and Applied Physics, The Queen's University of Belfast, Belfast, N. Ireland
N. E. McKeith
Affiliation:
Department of Pure and Applied Physics, The Queen's University of Belfast, Belfast, N. Ireland
W. M. Burton
Affiliation:
Astrophysics Research Unit, Culham Laboratory, Abingdon, Berks., England
H. J. B. Paxton
Affiliation:
Astrophysics Research Unit, Culham Laboratory, Abingdon, Berks., England
D. B. Shenton
Affiliation:
Astrophysics Research Unit, Culham Laboratory, Abingdon, Berks., England
R. Wilson
Affiliation:
Astrophysics Research Unit, Culham Laboratory, Abingdon, Berks., England

Extract

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The resonance lines of Mgii occur at wavelengths (2802.7 Å, 2795.5 Å) just beyond the extinction limit of the Earth's atmosphere. At such wavelengths sophisticated optical techniques can now be employed and this fact, together with the high cosmic abundance of magnesium, makes these lines particularly important for study in UV Astronomy. In the case of the Sun, the lines consist of a broad absorption with a pronounced emission core.

Type
Part II: Stellar Line Spectra
Copyright
Copyright © Reidel 1970 

References

Purcell, J. D., Garrett, D. L., and Tousey, R.: 1962, in Space Research, vol. III, p. 781.Google Scholar
Lemaire, P.: 1969, Astrophys. Letters 3, 43.Google Scholar
Lemaire, P. and Blamont, J. E.: 1967, Astrophys. J. 150, L129.CrossRefGoogle Scholar