Astronomy and Astrophysics – Astrophysics
Scientific paper
Oct 1981
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981phys...24..615c&link_type=abstract
Physica Scripta, vol. 24, no. 4, Oct. 1981, p. 615-621.
Astronomy and Astrophysics
Astrophysics
9
Ions, Plasma Density, Plasma Diagnostics, Plasma Spectra, Plasma Temperature, Spectroscopic Analysis, Autoionization, Isoelectronic Sequence, Line Spectra, Space Plasmas, Thermonuclear Reactions, Tokamak Devices
Scientific paper
During the past two decades, spectroscopic observations in high temperature astrophysical and thermonuclear-type plasmas have provided great impetus to the laboratory observation and analysis of spectra, especially those of highly ionized atoms. Thus the number of ions for which at least a few spectral lines have been identified has increased from 511 in 1959 to 648 in 1969 and to about 1019 in 1981. Much of the recent effort has gone into analyses for particular elements of interest (e.g., Fe and Ni for solar plasmas, and Cr, Fe, Ni, Mo, W, and Au for tokamak plasmas), or for simple isoelectronic sequences (e.g., those of neutral Ne, Na, Cu, Zn, Ag, and Tm). Some information now exists on atoms as highly ionized as Mo(41+), W(46+), and Au(51+). Although line identification work is far from complete, the interests of the user community are turning more and more toward the use of line intensities as diagnostics for determining plasma temperatures and densities. Very few of the required rate coefficients are known experimentally. It is important in theoretical calculations to include the resonance effects of autoionizing states, as these resonances frequently provide the dominant contribution to excitation, ionization, and recombination processes in low-density, high-temperature plasmas
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