Laboratory astrophysics: Measurements of N = n(prime) to N = 2 line emission in Fe-16(+) to Fe-23(+)

Details Laboratory astrophysics: Measurements of N = n(prime) to N = 2 line emission in Fe-16(+) to Fe-23(+) Laboratory astrophysics: Measurements of N = n(prime) to N = 2 line emission in Fe-16(+) to Fe-23(+)

Mar 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996stin...9719716s&link_type=abstract

Conference Paper, Atomic Processes and Plasmas

Astronomy and Astrophysics

Astrophysics

Emission Spectra, Galactic Clusters, Iron Isotopes, Solar Corona, X Ray Spectra, High Resolution, Astrophysics, Energy Levels, Energy Transfer, Data Acquisition, Galactic Nuclei, Stars, X Ray Spectroscopy, Trapped Particles, Spectral Bands, Electron Beams

Scientific paper

One of the dominant forms of astronomical line emission in the 6A to 18A spectral region is line emission produced by n = n(prime) to n = 2 transitions in Fe-16(+) to Fe-23(+) (i.e., Fe L-shell n-2 line emission). Using the Lawrence Livermore National Laboratory Electron Beam Ion Trap (EBIT) facility, the authors have carried out a number of measurements designed to address astrophysical issues concerning Fe L-shell line emission. Desired ions are produced and trapped using the nearly monoenergetic electron beam of EBIT. Trapped ions are collisionally excited and the resulting X-ray line emission detected using Bragg crystal spectrometers. They have recently completed a line survey of Fe L-shell 3-2 line emission. The line survey will allow a more reliable accounting of line blending in astronomical spectra. They have now begun a series of broadband, high resolution line ratio measurements. These measurements are designed to benchmark atomic calculations used in astronomical plasma emission codes and also for comparison with X-ray spectral observations of astronomical objects. Initial measurements have been carried out in Fe-23(+). Preliminary results agree with distorted wave calculations to within 20% and better.

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