Density diagnostic of astrophysical plasmas

Details Density diagnostic of astrophysical plasmas Density diagnostic of astrophysical plasmas

Jan 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997aipc..386..419l&link_type=abstract

The 13th international conference on spectral line shapes. AIP Conference Proceedings, Volume 386, pp. 419-420 (1997).

Statistics

Computation

Line Shapes, Widths, And Shifts, Stellar Atmospheres, Radiative Transfer, Opacity And Line Formation, Solar Electromagnetic Emission, Visible And Ultraviolet Spectra

Scientific paper

The Arcetri Spectral Code, that evaluates XUV line and continuum emission of thin plasmas in the range 1-2000 Å, has been recently updated and includes detailed computation of levels populations for the Iron lines from Fe IX to Fe XXIII and the most important Be-like, C-like, and N-like ions (1). A new technique is developed to evaluate the electron density, comparing observations and theoretical predictions for a set of density dependent lines of selected ions. Examples are given for Fe XIII and Si IX using recent observations of the solar corona with the S.E.R.T.S. spectrometers.

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