Abstract
Modeling the Stark broadening of spectral lines in plasmas is a complex problem. The problem has a long history, since it plays a crucial role in the interpretation of the observed spectral lines in laboratories and astrophysical plasmas. One difficulty is the characterization of the emitter’s environment. Although several models have been proposed over the years, there have been no systematic studies of the results, until now. Here, calculations from stochastic models and numerical simulations are compared for the Atoms 2014, 2 300 Lyman-α and -β lines in neutral hydrogen. Also discussed are results from the Helium-α and -β lines of Ar XVII.
Highlights
Line shape analysis is one of the most important tools for plasma diagnostics, as it provides information on the underlying physical processes involved in the line formation
We recall that the line shape is given by: I(ω) = Re π dt eiωt C(t) where C(t) is the autocorrelation function of the radiator dipole operator d, which can be expressed in Liouville space as: C(t) =≪ d† |U(t)|dρ0 ≫
Ρ0 is the density operator for the emitter only at the thermodynamical equilibrium and U(t) = {Ul (t)}l∈F is the bath averaged evolution operator of the emitter. l belongs to a measurable functional space, {F }, which provides a statistical method for the calculation of average quantities
Summary
Sandrine Ferri 1, *, Annette Calisti 1 , Caroline Mossé 1 , Joël Rosato 1 , Bernard Talin 1 , Spiros Alexiou 2 , Marco A. González 3 , Diego González-Herrero 3 , Natividad Lara 3 , Thomas Gomez 4 , Carlos Iglesias 5 , Sonja Lorenzen 6 , Roberto C. Received: 30 April 2014; in revised form: 10 June 2014 / Accepted: 16 June 2014 /
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