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Article

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Available under a Creative Commons Attribution Non-Commercial Share Alike 4.0 International Licence

Publication Details

Astronomy & Astrophysics Volume 398, Number 3, February II 2003 Page(s) 1179 - 1184 Section Celestial mechanic . doi:http://dx.doi.org/10.1051/0004-6361:20021654

Abstract

On the basis of the observed asymmetry of the measured spectral line profiles we have obtained the ion contribution to the (26 lines), (19 lines) and (20 lines) spectral line broadening due to the quasi-static ion approximation and ion-dynamical effects. The ion broadening parameters ( A) and the ion dynamic coefficients ( D) have been obtained directly by the use of our line deconvolution procedure which allows the determination of the basic physical properties that characterize the line profile and also the relevant plasma parameters. We are the first to publish experimental data, viz. D and A values for the , and lines. The 26 , 6 and 9 A values are the first measured data and many of them are the first published data in this field. We have found clear evidence of the quasi-static ion and ion-dynamical effects on the investigated line shapes; they play a much more important role than the approaches based on semiclassical theory provide, especially in the case of the spectral lines. This is of importance for astrophysical plasma modeling and diagnostics.

DOI

https://doi.org/10.1051/0004-6361:20021654

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