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The Classification of Fe IX to XVI Emission Lines and Isoelectronic Lines in Laboratory and Solar Spectra

Published online by Cambridge University Press:  12 April 2016

B. C. Fawcett
B. C. Fawcett*
Affiliation:
Astrophysics Research Unit, Culham Laboratory, Abingdon, Berks., England

Extract

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The spectra of Feix to xvi which dominate the XUV spectrum include the 3pn–3p-1 3d transitions studied earlier (Fawcett et al., 1966, 1967, 1968) (Gabriel et al., 1966) and the 3s23pn–3s3pn transitions. A comprehensive classification of spectra from both these configurations is now completed at the Astrophysics Research Unit. The experimental method used to extend the classification of the 3s23pn–3s3pn+1 lines in the period between potassium and vanadium was to compare the spectra of laser produced plasmas which possessed lines belonging to different ionization stages and is described by Fawcett (1970). Too many lines due to low stages of ionization obscured the 3s23pn–3s3pn+1 lines in chromium, manganese, iron, cobalt and nickel in these laser produced spectra for successful analysis. Volatile compounds of these elements were therefore added to the filling gas of a specially designed theta-pinch (Fawcett et al., 1971). Separation of lines of different stages of ionization was accomplished through the application of a microsecond shutter and adjusting the theta-pinch parameters. Radiation from the cooler ends of the plasma was avoided through viewing the theta-pinch from the side.

Type
Section III / Stellar and Solar UV Radiation
Information
International Astronomical Union Colloquium , Volume 14: Special Issue: Ultraviolet and X-Ray Spectroscopy of Astrophysical and Laboratory Plasmas , November 1972 , pp. 606 - 607
Copyright
Copyright © Reidel 1972

References

Fawcett, B. C.: 1970, J. Phys. B, Atom. Molec. Phys. 3, 1732.Google Scholar
Fawcett, B. C.: 1971a, J. Phys. B, Atom. Molec. Phys., 4, 1577.Google Scholar
Fawcett, B. C.: 1971b, Astrophysics Research Unit Report ARU R3. Available from Her Majesty’s Stationary Office.Google Scholar
Fawcett, B. C. and Hayes, R. W.: 1971, J. Phys. B. 5, 366.Google Scholar
Fawcett, B. C. and Gabriel, A. H.: 1966, Proc. Phys. Soc. 88, 262.Google Scholar
Fawcett, B. C., Gabriel, A. H., and Saunders, P. A. H.: 1967, Proc. Phys. Soc. 90, 863.Google Scholar
Fawcett, B. C., Peacock, N. J., and Cowan, R. D.: 1968, J. Phys. B, Atom. Molec. Phys. 1, 295.Google Scholar
Fawcett, B. C., Gabriel, A. H., and Paget, T. M.: 1971, J. Phys. B, Atom. Molec. Phys. 4 986.Google Scholar
Gabriel, A. H., Fawcett, B. C., and Jordan, C.: 1966, Proc. Phys. Soc. 87, 825.Google Scholar
Gabriel, A. H., Garton, W. R. S., Goldberg, L., Jones, T. J. L., Jordan, C., Morgan, F. J., Nicholls, R. W., Parkinson, W., Paxton, H. J. B., Reeves, E. M., Shenjon, D. B., Speer, R. J., and Wilson, R.: 1971, Astrophys. J. 3, 545.Google Scholar
Jordan, C.: 1971, Solar Phys. 21, 381.Google Scholar
Svensson, L. A.: 1971, Solar Phys. 18, 232.Google Scholar