| Issue |
A&A
Volume 417, Number 1, April I 2004
|
|
|---|---|---|
| Page(s) | 375 - 380 | |
| Section | Atomic, molecular, and nuclear data | |
| DOI | https://doi.org/10.1051/0004-6361:20034162 | |
| Published online | 16 March 2004 | |
Importance of collisions with charged particles for stellar UV line shapes: 
1
Astronomical Observatory, Volgina 7, 11160 Belgrade, Serbia and Montenegro
2
Isaac Newton Institute of Chile, Yugoslavia Branch
Corresponding author: N. Milovanović, nmilovanovic@aob.bg.ac.yu
Received:
6
August
2003
Accepted:
10
November
2003
Stark broadening parameters, widths and shifts, for 84 spectral
lines of doubly-ionized cadmium () have been calculated
using the modified semi-empirical approach (MSE). Calculated spectral lines belong
to the transitions 4d95s–4d95p and 4d95p–4d95d. Widths and
shifts of the spectral lines are given for temperature range of
5000 K–60 000 K and an electron density of 1023 m-3. The influence of
collisions with charged particles on UV stellar lines along the HR
diagram is discussed. Compared to the Doppler broadening, the influence of
the Stark broadening mechanism is more important for deeper atmospheric layers
and for larger values of 
. Stark broadening does not depend on
turbulent velocity for the considered stellar model of a standard main sequence
hot star of A0 spectral type. The influence of the Stark widths for standard
models of DA and DB white dwarfs is also discussed.
Key words: atomic processes / line: formation / stars: atmospheres / stars: early-type / stars: white dwarfs
© ESO, 2004
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