Hostname: page-component-5c6d5d7d68-sv6ng Total loading time: 0 Render date: 2024-08-22T05:04:54.202Z Has data issue: false hasContentIssue false
  • English
  • Français

Relative Intensities of Lines in F I- B I-Like Ti, Cr, Fe, Ni, and Ge: A Comparison of Theory and Experiment

Published online by Cambridge University Press:  12 April 2016

B.C. Stratton ,
H.W. Moos ,
U. Feldman ,
J.F. Seely ,
S. Suckewer  and
M. Finkenthal
B.C. Stratton
Affiliation:
Department of Physics and Astronomy Johns Hopkins University Baltimore, Maryland
H.W. Moos
Affiliation:
Department of Physics and Astronomy Johns Hopkins University Baltimore, Maryland
U. Feldman
Affiliation:
E.O. Hulburt Center for Space Research Naval Research Laboratory Washington, D.C.
J.F. Seely
Affiliation:
E.O. Hulburt Center for Space Research Naval Research Laboratory Washington, D.C.
S. Suckewer
Affiliation:
Plasma Physics Laboratory, Princeton University, Princeton, N.J.
M. Finkenthal
Affiliation:
Racah Institute of Physics, Hebrew University Jerusalem, Israel

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Allowed 2s22pk − 2s2pk+1 transitions in the F I- B I-like ions of elements with Z ≥ 20 are often observed in spectra of high-temperature (Te ≥ 107 K) laboratory and astrophysical plasmas. Calculations of level populations in these ions are important in the interpretation of measured intensities of these lines for plasma diagnostics. Impurity ion densities and radiated power losses in tokamak plasmas, and the emission measure of astrophysical sources, can be derived from spectroscopic measurements using level population calculations. Certain line-intensity ratios can be used to measure the electron density in astrophysical plasmas; this technique may also be useful in some low-density laboratory plasmas. It is therefore important to experimentally check the level populations in high-Z ions using spectra from a well-diagnosed laboratory plasma, such as that of a tokamak. This has been previously done only for some transitions in Fe XVIII - Fe XXII (Suckewer and Hinnov 1979).

Type
Session 6. Poster Papers
Information
International Astronomical Union Colloquium , Volume 86: Eighth International Colloquium on Ultraviolet and X-ray Spectroscopy of Astrophysical and Laboratory Plasmas , 1984 , pp. 175 - 178
Copyright
Copyright © Naval Research Laboratory 1984. Publication courtesy of the Naval Research Laboratory, Washington, DC.

References

Bhatia, A.K., Feldman, U., and Doschek, G.A. 1980, J. Appl. Phys., 51, 1464.CrossRefGoogle Scholar
Bhatia, A.K., and Mason, H.E. 1980, Astr. Ap., 83, 380.Google Scholar
Feldman, U., Doschek, G.S., Cheng, C.C., and Bhatia, A.K. 1980, J. Appl. Phys., 51, 190.CrossRefGoogle Scholar
Feldman, U., Seely, J.F., and Bhatia, A.K. 1984, Atomic Data and Nuclear Data Tables, in press.Google Scholar
Hodge, W.L., Stratton, B.C., and Moos, H.W. 1984, Rev. Sci. Instr., 55, 16.CrossRefGoogle Scholar
Kastner, S.O., Neupert, W.M., and Swartz, M. 1974, Ap. J., 191, 261.CrossRefGoogle Scholar
Mason, H.E., Doschek, G.A., Feldman, U., and Bhatia, A.K. 1979, Astr. Ap., 73, 74.Google Scholar
Mason, H.E., and Storey, P.J. 1980, M.N.R.A.S., 191, 631.CrossRefGoogle Scholar
Stratton, B.C., Moos, H.W., and Finkenthal, M. 1984, Ap. J. (Letters), 279, L31.CrossRefGoogle Scholar
Suckewer, S., and Hinnov, E. 1979, Phys. Rev. A., 20, 578.CrossRefGoogle Scholar