Sylvie Sahal-Brechot, Milan S. Dimitrijevic, Nebil Ben Nessib
Stark broadening theory is currently operated for calculating widths and
shifts of spectral lines that are needed for spectroscopic diagnostics and
modelling in astrophysics, laboratory and technological plasmas. We have
calculated a great number of data, obtained through the impact semi- classical
perturbation theory: tables have been published for neutral atom and ion
emitters, and typical temperatures, electron and ion densities. They are
currently implemented in the STARK-B database which participates to the
European effort within the VAMDC (Virtual Atomic and Molecular data Centre).
Despite of that, a great number of data are still missing and their orders of
magnitude would at least be welcome. In the present paper, we will revisit and
compare the orders of magnitudes and trends of the impact Stark widths and
shifts, by considering their semiclassical perturbation expressions. We will
also provide fitting formulae which are essential for the modelling codes of
stellar atmospheres and envelope
View original:
http://arxiv.org/abs/1201.2022
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