High-resolution measurements, line identification, and spectral modeling of K-alpha transitions in Fe XVIII-Fe XXV

Details High-resolution measurements, line identification, and spectral modeling of K-alpha transitions in Fe XVIII-Fe XXV High-resolution measurements, line identification, and spectral modeling of K-alpha transitions in Fe XVIII-Fe XXV

Jun 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...409..846b&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 409, no. 2, p. 846-859.

Astronomy and Astrophysics

Astrophysics

40

Electron Transitions, Emission Spectra, Iron, Line Spectra, Spectrum Analysis, Electron Density (Concentration), Ground State, Ionic Diffusion, Solar Spectra, Tokamak Devices

Scientific paper

A detailed analysis of the iron K-alpha emission spectrum covering the wavelength region from 1.840 to 1.940 A is presented. Measurements are made with a high-resolution Bragg crystal spectrometer on the Princeton Large Torus (PLT) tokamak for plasma conditions which closely resemble those of solar flares. A total of 40 features are identified, consisting of either single or multiple lines from eight charge states in iron, Fe XVIII - Fe XXV, and their wavelengths are determined with an accuracy of 0.1-0.4 mA. Many of these features are identified for the first time. In the interpretation of our observations we rely on model calculations that determine the ionic species abundances from electron density and temperature profiles measured independently with nonspectroscopic techniques and that incorporate theoretical collisional excitation and dielectronic recombination rates resulting in the excitation of the 1s2sr2ps configurations. The model calculations also include the effect of diffusive ion transport. Good overall agreement between the model calculations and the observations is obtained, which gives us confidence in our line identifications and spectral modeling capabilities. The results are compared with earlier analyses of the K-alpha emission from the Sun.

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