Stark-broadening parameters of ionized mercury spectral lines of astrophysical interest

Details Stark-broadening parameters of ionized mercury spectral lines of astrophysical interest Stark-broadening parameters of ionized mercury spectral lines of astrophysical interest

May 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992jqsrt..47..315d&link_type=abstract

Journal of Quantitative Spectroscopy and Radiative Transfer (ISSN 0022-4073), vol. 47, no. 5, May 1992, p. 315-318.

Astronomy and Astrophysics

Astrophysics

2

Line Spectra, Magnetic Stars, Mercury (Metal), Spectral Line Width, Stark Effect, Stellar Spectrophotometry, Abundance, Atomic Energy Levels, Fine Structure, Stellar Atmospheres, Stellar Composition

Scientific paper

The semiclassical perturbation formalism is presently used to calculate electron-, proton-, and ionized-He-impact linewidths and line shifts for seven Hg II lines observed in the spectra of Mn and magnetic stars, as well as in laboratory plasmas. In the case of the astrophysically important 3983.9 A line, the results obtained underestimate the real Stark line width. Accuracy is improved for this line by multiplying the semiclassical line widths by an averaged ratio of measured to calculated values.

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