1. STARK BROADENING PARAMETERS OF S II SPECTRAL LINES FOR STELLAR PLASMA CONDITIONS
MILAN S. DIMITRIJEVIĆ1, NENAD MILOVANOVIĆ1,
ZORAN SIMIĆ1, SYLVIE SAHAL-BRÉCHOT2
1Astronomical Observatory, Volgina 7, Belgrade, Serbia
2LERMA, Observatoire de Paris, Meudon, France

2. Spectral lines of ionized sulfur have been observed in stellar spectra(see e.g. Adelman and Pintaldo (2000), Adelman et al. (2001)), so that their Stark broadening parameters are needed for sulfur abundance determination, radiative transfer calculations as well as for stellar spectra analysis and synthesis.
Stark broadening is particularly significant for white dwarfs, post AGB stars, pre- white dwarfs and for A type stars.

3. PART OF TABLE: 3 of 12 calculated SC method: PERTURBER DENSITY = 1
PART OF TABLE: 3 of 12 calculated SC method: PERTURBER DENSITY = 1.E+17cm-3
PERTURBERS ARE: ELECTRONS PROTONS NIZED HELIUM
TRANSITION T(K) WIDTH(A) SHIFT(A) WIDTH(A) SHIFT(A) WIDTH(A) SHIFT(A)
S II 3d 4p E E E E E-02
A E E E E E-02
C= 0.63E E E E E E-02
E E E E E-02
E E E E E-02
E E E E E-02
S II 3d 4p E E E E E-03
A E E E E E-03
C= 0.84E E E E E E-02
E E E E E-02
E E E E E-02
E E E E E-02
S II 4s 4p E E E E-02
A E E E E-01
C= 0.77E E E E E-01
E E E E E-01
E E E E E-01
E E E E E-01

4. THANK YOU!