Stark broadening of heavy ion spectral lines in spectra of hot stars.

Details Stark broadening of heavy ion spectral lines in spectra of hot stars. Stark broadening of heavy ion spectral lines in spectra of hot stars.

Sep 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994pobeo..46....1p&link_type=abstract

Publications de l'Observatoire Astronomique de Beograd, No. 46, p. 1 - 131

Astronomy and Astrophysics

Astronomy

1

Spectral Lines: Stark Broadening, Hot Stars: Spectra

Scientific paper

A large number of heavy ion spectral lines are present in spectra of hot stars. Stark broadening is the dominant pressure broadening mechanism for stars with Teff ⪆10000K. Due to the lack of reliable atomic data for Stark broadening calculation of heavy ion lines with complex spectra it is not always possible to apply a semiclassical approach. In this case one can provide Stark broadening data using approximative methods. One of such method is the modified semi-empirical approach (MSE). In this work the author investigates the applicability of this modified semi-empirical approach for Stark broadening parameter calculation of ions with complex spectra. To test the MSE approach he has selected seven singly ionized emitters (Z ≥ 30): Zn II, As II, Sb II Cd II, I II, Br II and Bi II.

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