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Several laboratory facilities were used to benchmark theoretical spectral models those extensively used by astronomical communities. However there are still many differences between astrophysical environments and laboratory miniatures that can be archived. Here we setup a spectral analysis system for astrophysical and laboratory (SASAL) plasmas to make a bridge between them, and investigate the effects from non-thermal electrons, contribution from metastable level-population on level populations and charge stage distribution for coronal-like, photoionized, and geocoronal plasmas. Test applications to laboratory measurement (i.e. EBIT plasma) and astrophysical observation (i.e. Comet, Cygnus X-3) are presented. Time evolution of charge stage and level population are also explored for collisional and photoionized plasmas.

An International Astronomical Union Meeting, Ultraviolet and X-ray Spectroscopy of Astrophysical and Laboratory Plasmas, was held on the Belfield Campus of the Univ. of Dublin, Ireland, from 30 August through 1 September 1982. Over 80 scientists from 13 countries in the astronomical, plasma, and atomic physics communities participated in an exchange of both theoretical and experimental research. It is significant that such an exchange took place at this time because short-wavelength astrophysical satellite-borne experiments are producing data that can be directly compared with results from high-temperature plasma spectroscopy in the laboratory. The comparison provides a broad data base to check the validity of theoretical models, particularly in the case of highly ionized atoms. (Author)