Ion dynamics effect on stark-broadened line shapes: A cross-comparison of various models

Atoms 2014,2, 299-318; doi:10.3390/atoms2030299 OPEN ACCESS atoms ISSN 2218-2004 www.mdpi.com/journal/atoms Article Ion Dynamics Effect on Stark-Broadened Line Shapes: A Cross-Comparison of Various Models Sandrine Ferri 1,*, Annette Calisti 1, Caroline Mossé 1, Joël Rosato 1, Bernard Talin 1, Spiros Alexiou 2, Marco A. Gigosos 3, Manuel A. González 3, Diego González-Herrero 3, Natividad Lara 3, Thomas Gomez 4, Carlos Iglesias 5, Sonja Lorenzen 6, Roberto C. Mancini 7 and Evgeny Stambulchik 8 1Aix-Marseille Université, CNRS, PIIM UMR7345, 13397 Marseille, France; E-Mails: [email protected] (A.C.); [email protected] (C.M.); [email protected] (J.R.); [email protected] (B.T.) 2TETY, University of Crete, 71409 Heraklion, TK 2208, Greece; E-Mail: [email protected] (S.A.) 3Department de Óptica y Física Applicada, Universidad de Valladolid, Valladolid 47071, Spain; E-Mails: [email protected]a.es (M.A.G.); [email protected]a.es (M.A.G.); die[email protected] (D.G.-H.); [email protected]a.es (N.L.) 4Department of Astronomy, University of Texas, Austin, TX 78731, USA; E-Mail: [email protected]xas.edu (T.G.) 5LLNL, Livermore, CA 94550, USA; E-Mail: [email protected]v (C.I.) 6Institut für Physik, Universität Rostock, D-18051 Rostock, Germany; E-Mail: [email protected] (S.L.) 7Physics Dept., University of Nevada, Reno, NV 89557, USA; E-Mail: [email protected] (R.C.M.) 8Faculty of Physics, Weizmann Institute of Science, Rehovot 7610001, Israel; E-Mail: Evgeny[email protected] (E.S.) *Author to whom correspondence should be addressed; E-Mail: [email protected]; Tel.: +33-49128-8623. Received: 30 April 2014; in revised form: 10 June 2014 / Accepted: 16 June 2014 / Published: 4 July 2014 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 2014,2300 Lyman-αand -βlines in neutral hydrogen. Also discussed are results from the Helium-α and -βlines of Ar XVII. Keywords: Stark broadening; line shapes; plasmas; numerical simulations; models 1. Introduction 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. With the increasing number of applications in different areas of plasma physics, the modeling of line broadening from neutral or charged emitters has been in perpetual development and remains a keystone in plasma spectroscopy [1]. In the formation of a line shape, Stark broadening is the most computationally challenging contribution, since the main difficulty is to properly characterize the emitter environment. It involves a complex combination of atomic physics, statistical mechanics and detailed plasma physics [2]. In particular, it is well known that the quasi-static ion approximation can lead to discrepancies with experimental data near the line center. This happens whenever the electric microfields produced at the emitter by the surrounding ions fluctuate during the inverse half-width at half-maximum (HWHM) time scale. The first attempts to account for ion dynamics in theoretical models were done in the 1970s, followed by experimental proof (see the historic introduction in [3] and the references therein). Since then, several models based on stochastic or collisional approaches have been developed, together with numerical simulations ([4] and the references therein). Necessarily, their limit of applicability, accuracy and, thus, results differ from one another, and up to now, no systematic comparison have existed [5]. The purpose here is to present cross-comparisons of different models that account for the ion dynamics effect. The line shape formalism is briefly recalled in Section 2, which serves to introduce notation. The specifics of the various models and numerical simulations are also presented in this section. We review the simulations Euler–Rodrigues (ER)-simulation [6], HSTRK [7], HSTRK_frequency separation technique (FST) [8], SimU [9,10], Xenomorph [11] and the models QuantST.MMM (MMM—model microfield method) [12], quasicontiguous (QC)-frequency fluctuation model (FFM) [13], multi-electron line-shape (MELS) [14], multi-electron radiator line-shape (MERL) [15,16], PPP [17], ST-PST [18] and UTPP [19] that have been used for the present purpose. The ion dynamics effect on the hydrogen Lyman-αand -βlines is discussed in Section 3.1, demonstrating the difficulty of such modeling even for these well-known lines. In Section 3.2, results on helium-α and -βlines of Ar XVII produced by the two stochastic models (Boerker–Iglesias–Dufty (BID) [20] and FFM [4,21]) are discussed with the help of the numerical simulation (SimU). The reliability of such calculations is of interest in the diagnostics of inertial confinement fusion core plasma conditions. Conclusions are given in Section 4. Atoms 2014,2301 2. Theory, Models and Simulations We recall that the line shape is given by: I(ω) = 1 πRe ∫∞ 0 dt eiωtC(t)(1) 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≫(2) where the double bra and ket vectors are defined as usual in Liouville space. Here, ρ0is the density operator for the emitter only at the thermodynamical equilibrium and U(t) = {Ul(t)}l∈Fis the bath averaged evolution operator of the emitter. lbelongs to a measurable functional space, {F}, which provides a statistical method for the calculation of average quantities. The main problem is to determine U(t). One has thus: •to find the time evolution of Ul(t)for a given microfield configuration, which means solving the following equation: dUl(t) dt =−i[L0−d·Fl(t)] Ul(t), Ul(0) = 1 (3) where L0represents the Liouvillian of the unperturbed radiator and d·Fl(t)represents the Stark effect that connects the dipole operator dto the microfield created by surrounding charged particles Fl(including ions and electrons), •and to average it over a statistical ensemble of the microfields { }l∈F. In its general form, the problem cannot be treated analytically. Nevertheless, U(t)can be obtained by numerical simulation integrating Equation (3) on simulated sampling of microfield histories. Usually, such a calculation is split into two independent steps [3]. First, the plasma particle trajectories are obtained by a numerical solution of Newton’s equations of motion or an alternative method. Knowing the trajectory of each particle, the electric fields at the emitter are evaluated and stored to be used in the second step. Then, the line shape simulation follows: a step-by-step integration of Equation (3) is performed using these field histories. The evolution operator of the emitter is calculated, and the whole procedure is repeated several times in order to average over a representative sample set of independent perturbing field histories {f1, f2...fN}. As a result, C(t)is given by: C(t) = 1 N N ∑ i=1 Ci(t)(4) and the line shape is obtained by a Fourier transform of C(t). Although all line shape simulations are based on the same scheme, we will see in the next section that they can differ slightly depending on the details of the models. Alternatively, efficient analytical models based on fundamental assumptions and approximations have been developed [1]. In the standard theory (ST), the line shape calculation is based on the separation between the ions and the electrons due to the radically different dynamical properties of the microfields Atoms 2014,2302 they create. Indeed, the typical fluctuation rate of the electric field created by perturber species pwith a velocity relative to the center of mass vpand a density npis defined by: νp=vp/dp(5) where dp= (3/4πnp)1/3is a typical interparticle distance. Assuming equal temperature for ions and electrons and plasma neutrality, one has [3]: νe νi ∼(µi µe)1/2 Z1/3 i.(6) Thus, the perturbation due to the electrons (with reduced mass µe) is nearly two orders of magnitude faster than that of ions (with reduced mass µiand charge Zi). This allows for treating the electrons and the ions in a different way. The fast electrons are assumed to perturb the emitter by means of collisions, treated in the impact approximation, and the slow ions are assumed to be quasi-static. This results in a quantum-emitter system perturbation operator l=−d·Fi,l +iϕe, containing a non-Hermitian homogeneous electron-impact broadening contribution ϕeand the ion microfield interaction −d·Fi,l, which has to be numerically averaged with a static-field probability distribution Q(Fi), or because of isotropy, with dW(Fi)=4πF2 iQ(Fi)dFi. The later can be calculated numerically in the ideal gas limit for perturbing ions [22] or using more sophisticated models that account for ion correlations [23]. Using the set of above assumptions, the quasi-static line shape is written as: Is(ω) = −1 πIm ≪d†|∫dFiQ(Fi)Gs(ω, Fi)|dρ0≫(7) in which the resolvent operator is given by: Gs(ω, Fi) = (ω−L0+d·Fi−iϕe)−1.(8) Although the electrons are often well described within the impact approximation, a quasi-static treatment of the ions can lead to large errors for plasma conditions, such as the ion microfields fluctuate during the inverse HWHM time scale. In the next section, we briefly review the simulations and the models that have been developed to account for the ion dynamics effect and that have been used for the present cross-comparisons. 2.1. The Numerical Simulations The results from four numerical simulation codes based on different models have been submitted. They differ either in the way they model the motions of the plasma particles or in the procedure for the integration of the Schrödinger equation. In the ER-simulation, the simulated plasma is an electrically neutral ensemble of statistically independent charged particles made of Niions and Neelectrons moving along straight line trajectories within a spherical volume. An emitter is assumed to be placed at the center of such a box. The temporal evolution of the whole system is measured along a discrete time axis from zero to a definite number of times of a fixed increment. Every temporal state is given by the set of values of the positions and velocities of the particles in the system. At every time step, the electric field produced by ions and Atoms 2014,2303 electrons is calculated using Coulomb’s law or a Debye-screened field. This electric field is an input to the Schrödinger equation that computes the emitter time evolution operator. For hydrogen and when the no-quenching approximation is considered, the atom state is described with the Euler–Rodrigues parameters [24]. The HSTRK and HSTRK_FST codes also use the Gigosos–Cardeñoso approach [25]. Both codes rely on the Hegerfeld–Kesting–Seidel method of collision-time statistics [26] and compute C(t). Depending on the appropriate option, HSTRK can do an electron only, ion only or joint simulation, but one can also do combinations, e.g., electron simulation and quasi-static ions or impact electrons and ion simulation. For the Fourier transform, if a long-time exponential behavior is detected for times t > τ, then the contribution to the Fourier transform of the (τ, ∞) region is computed analytically using the detected exponential decay and added to ∫τ 0dtC(t)eıωt.τis determined via start-up runs, e.g., a run with a small number of configurations is done to obtain a rough idea of the HWHM and τis adjusted to cover at least a number of inverse HWHMs. The integral is done by Filon’s rule [27]. HSTRK_FST implements the frequency separation technique, which first identifies the “impact” phase space of ion perturbers (e.g., impact parameters and velocities), which produce a width much less (in these runs, “much less” was 10-times less) than the field fluctuation frequency. This meant: HWHM(Ω) = 0.1 Ω (9) where the HWHM is computed by including all ion perturbers with impact parameter ρand velocity v > Ωρ. Hence, the calculation is essentially the same, except that only slow ions v < Ωρare included in the simulation. The C(t)obtained from the simulation of these slow ions is then multiplied by e−HW HM(Ω)t, and the Fourier transform is taken as in HSTRK. The use of a pure exponential form for the rapidly fluctuating (impact) part is a consequence of using the complete collision assumption for solving the impact part [28,29] and results in a C(t)that is not correct for very short times. This is manifested in the (far) wing behavior of the HSTRK_FST profiles and can be remedied by using the incomplete collision formulas of the above-cited analytical solutions. SimU is a combination of two codes: a molecular dynamics (MD) simulation of variable complexity and a solver for the evolution of an atomic system with the MD field history used as a (time-dependent) perturbation. A technical difference from other numerical simulation methods is the way the spectrum is calculated. Instead of employing the dipole autocorrelation function via Equation (1), SimU calculates the Fourier transform of the dipole matrix:  d(ω) = ∫∞ 0 dt e−iωt  d(t)(10) and then uses it directly instead of C(t): Iλ(ω)∝1 2π∑ i ρi∑ f ω4 fi|eλ· ⟨ dfi(ω)⟩|2(11) where eλis the light polarization direction and each initial state iis assigned a population factor ρi. Similarly to other methods, this procedure is repeated many times and averaged (cf. Equation (4)). The recently developed code, Xenomorph, is based on the models of Gigosos and González [30], where a straight line assumption is made. A general Schrödinger solver described in [31] is used to Atoms 2014,2304 obtain the eigenvalues En(t)and eigenvectors |n(t)⟩at every time step of the simulation. The emitter time evolution operator is then evaluated: Ul(t+ ∆t) = {∑ n e−iEn(t)∆t/¯hn(t)⟩⟨n(t)|}Ul(t)(12) and is used to obtain the dipole matrix. The Fourier transform of the latter is computed to obtain the line shape function, as is done in SimU (cf. Equations (10) and (11)). 2.2. The Models The main difficulty in introducing the ion dynamics in the Stark line shape calculations is to develop a model that provides a sufficiently accurate solution of the evolution Equation (2) assuming an idealized stochastic process that conserves the statistical properties of the “real” interaction between the microfields and the radiating atom. A successful model developed for neutral emitters—the model microfield method (MMM), due to Brissaud and Frisch [32,33]—involves stochastic fields that are constant in a given time interval and suddenly jump from one value to the next one at random times. The amplitudes of the field sequences are determined in order to be consistent with the static properties of the microfield, i.e., the static-field probability distribution Q(F). The jumping frequency ν(F)has to be chosen properly in order to reproduce the dynamics properties of the microfields represented by their autocorrelation function <F(t)·F(0) >. In QuantSt.MMM, MMM (for ions) is combined with a quantum-statistical approach to calculate pressure broadening due to plasma electrons. The perturbation by electrons is considered to second order in the potential [34,35]. MELS and MERL are based upon the BID model. The latter derives from the MMM, but its formulation is based on statistical mechanics [36] and provides a unified description of radiative and transport properties for charged emitters [20]. The stochastic line shape is written as: Id(ω) = −1 πIm ≪d†|∫dFQ(Fi)GBID(ω, Fi) 1 + iν(ω)∫dFQ(Fi)GBID(ω, Fi)|dρ0≫(13) in which the resolvent is given by: GBID(ω, Fi) = (ω−L0+d·Fi−iν(ω))−1(14) The jumping frequency ν(ω)is chosen as: ν(ω) = ν0 1 + iωτ .(15) where the two parameters ν0and τare defined in this model by the lowand high-frequency limits of the momentum autocorrelation function. Here, τis assumed to be null. Another approach is the frequency fluctuation model (FFM), on which the PPP code and, recently, the QC-FFM code rely. The latter is a hybrid model using the quasi-contiguous approximation [37] for H-like transitions and the FFM for modeling the microfield dynamics effect. The FFM relies on a different idealization of the stochastic process than MMM and BID. Here, the quantum system perturbed Atoms 2014,2305 by a time-dependent microfield behaves like a set of field-dressed two-level transitions (SDT) subject to a collision-type mixing process. More precisely, the fluctuation mechanism of these SDT obeys a stationary Markov process defined by the instantaneous probability of states pj=aj/∑kak(ajbeing the intensity of the SDT, j) and the transition rates between these states Wk,j =−Γjδk,j +Wk,j, where Γk,j =νδi,j and Wk,j =νpj. The typical fluctuation rate νFFM of the electric field, given by Equation (5), is used. Working in the Liouville space of the dressed two-level radiators, the line shape is written as [38]: Id(ω) = 1 πRe ∑ j,k i≪Dk|GFFM(ω)|Djpj≫(16) with the resolvent: GFFM(ω) = (ω−Lω+iW)−1(17) where Lωis the Liouville operator involving the transition energies of the SDT (ωi) and Diare the matrix elements of the dipole moment for the SDT. Due to the particular form of the matrix of transition rates W, the dynamic line shape is written as [4]: Id(ω) = ∑kak πRe ∑k pk ν+i(ω−ωk) 1−ν∑k pk ν+i(ω−ωk) (18) Despite the fact that the two stochastic models lead to different functional forms, it follows that both BID and FFM recover the static limit for νBID = 0 in Equation (14) and for νFF M = 0 in Equation (18). In the opposite limit, both models recover the fast fluctuation limit (ν→ ∞) that should approximate the “no ions” profile. However, BID recovers the impact limit in the line center whenever νis large, while the FFM does not (see [39] for a more detailed discussion). We note that QC-FFM uses the FFM approximation for ions and electrons alike. For the latter, correctly approaching the impact approximation in the fast fluctuation limit becomes especially important. To this end, a modification to the effective fluctuation rate was introduced: ˜ν=ν+ν2 ν0 (19) where ν0is an empirically obtained constant (for details, see [13]). Two other models based on the collisional approach have been used, too. The ST-PST model is based on the standard theory with a number of options. Specifically, apart from the pure ST results, ST-PST can (and by default does) also compute the results of ST with penetrating collisions correctly accounted for analytically [18]. In addition, an FST-FFM calculation is also done [8]: first, an Ωis determined, exactly as described above for HSTRK_FST. Next, the FFM is applied to the field that excludes the fast, impact part. Last, the two profiles are convolved. As a result, the impact limit is correctly built in and recovered, hence extending the FFM validity without sacrificing its speed. Note, however, that with the current FST implementation, which uses the completed collision assumption for the impact phase space, the far wings are not accurate, as already discussed. The UTPP code is devoted to the calculation of hydrogen line shapes in regimes where the impact approximation for ions is reasonably accurate. Such a regime is attained for lines with a low principal Atoms 2014,2306 quantum number in magnetic fusion experiments in the absence of Doppler broadening (Doppler-free line shape models were required for radiation transport simulations, e.g., [40]). In UTPP, a line shape is calculated using the following formula: I(ω) = 1 πRe ≪d†|1 s+iL0+K(s)|dρ0≫(20) where s=−iω and K(s)is a collision operator calculated in a framework similar to that used in the Voslamber unified theory (Bogoliubov-Born-Green-Kirkwood-Yvon (BBGKY) hierarchy), but here adapted to ions [19]. The main advance with respect to the unified theory is that the collision operator accounts for the finite lifetime of the atom during each collision; this lifetime yields an effective range for the action of the microfield of the order of v/¯γ, where ¯γis a typical matrix element of the collision operator (see the discussion in [41]). This model (and its adaptation to electrons) does not lead to a divergent collision operator if the Debye length is assumed infinite, which is in contrast to standard hydrogen models (see [42]); this makes it suitable for the presented cases, provided the perturbing species under consideration is strongly dynamic. 3. Comparisons and Discussion To test the accuracy of the different numerical codes based either on stochastic and collisional models or numerical simulations, calculations for standardized case problems were carried out and analyzed [5]. A preselected set of transitions on a grid of electron densities (ne) and temperatures (T=Te=Ti) have been proposed, and for each case, the atomic and plasma models have been specified. In this way, various contributions that can affect the Stark broadened line shape, such as the influence of particle correlations on electric microfields, the effects of external fields, the high-n merging with continuum or the satellite broadening, have been investigated. For the present purpose, we will only focus on cases where the ion dynamics effect was studied. 3.1. Hydrogen Lyman-αand Lyman-βLines The following examples consider the hydrogen Lyman-αand Lyman-βlines in an ideal plasma consisting of protons for electron densities ne= 1017 −1019 cm−3and temperatures T= 1 −100 eV. These cases are not necessarily practical, but permit basic comparisons to assess the influence of ion dynamics on the line profiles. Here, only pure ionic linear Stark effect is considered (∆n= 0 interactions are ignored) and the fine structure is not taken into account. The concept of ideal plasma means that unscreened particles moving along straight path trajectories are considered in the numerical simulations, and the Holtsmark static-field distribution function [22] is used in the models. An overall comparison of the results is presented in Figure 1. For each subcase (determined by a combination of (ne, T)) and for each code, ratios between the full-width at half-maximum (FWHM) and an average of FWHM of all submitted results have been evaluated [5]: Ri=FWHM <FWHM >.(21) Atoms 2014,2307 The graph is divided in two regions: the left side corresponds to results for the Lyman-αline and the right side to the Lyman-βline. Each region is divided into three sub-regions that correspond to the three densities chosen. Finally, in each sub-region, each set of results corresponds to the temperatures, T= 1,10,100 eV, respectively. For the Lyman-αcase, the results present a large dispersion, deviating from the average by more than a factor of five in each direction. In contrast, the scatter for the Lyman-β shows a rather good agreement between the codes. In fact, these two lines present a completely different behavior concerning the ion dynamics effect. Figure 1. Overall comparison of the workshop results of the ion dynamics effect on Lyman-αand -βhydrogen lines. For each subcase, i.e., different pairs of (ne, T), the scatter of ratios between the different results and an average value is plotted. The different symbols correspond to: (black dot) SimU; (red square) UTPP; (blue triangle) PPP; (blue asterisk) Xenomorph; (cyan open triangle) HSTRK; (cyan triangle) HSTRK_FST; (red diamond) ER-simulation; (green circle) QuantST.MMM; (black cross) QC-FFM. 5 6 7 8 0.1 2 3 4 5 6 7 8 1 2 3 4 5 6 7 8 10 FWHM/<FWHM> n e (cm -3 ) 10 17 cm -3 H Lymanβ H Lymanα 10 19 cm -3 10 18 cm -3 10 17 cm -3 10 18 cm -3 10 19 cm -3 T=1eV T=10eV T=100eV 3.1.1. The Lyman-αLine The static Stark effect of the Lyman-αline (as all the ∆n=n−n′= 1 lines, where nand n′are the principal quantum number of the upper and lower states, respectively) features a strong unshifted component that is highly sensitive to the ion dynamics effect. Thus, even though the Lyman-αline is the simplest case from the atomic structure point of view, it presents a non-trivial Stark-broadening behavior. In Figure 2, only results from the numerical simulations are plotted for the sake of clarity. One sees that in the range of 1 to 100 eV, the simulations either predict that the width increases when the plasma temperature increases (for the fixed density ne= 1019 cm−3, they present a temperature dependency as ∼T1/3) or predict that the width is mostly insensitive to the temperature’s rise (for the fixed density ne= 1017 cm−3). Concerning the dependence on the plasma density, the width, which is mainly due to the width of the central component for T= 1 eV, increases as n1/3 e. For T= 100 eV, the results show a n2/3 edependence, corresponding to the quasi-static behavior of the lateral components [2]. We mention, however, that the cutoff of the Coulomb interaction at a finite box size may not accurately reproduce an ideal plasma [42]. Atoms 2014,2314 Figure 10. The He-αline, the strong component for T= 1 keV and ne= 5 ×1023 cm−3: SimU (black circles); FFM with ν= 3 eV (solid blue); ν= 5.62 eV (solid red); and ν= 8 eV (solid black). 0.001 0.01 0.1 normalized intensity 3160315031403130312031103100 energy (eV) Finally, the He-βline is presented in Figure 11. At the chosen plasma conditions, as the Stark splitting of the He-βquasi-static line shape is greater than the fluctuation rate and the electron width is larger, the ion dynamics effect is less pronounced than on the He-α. Figure 11 shows SimU, BID and FFM in rather good agreement relative to the discrepancies of their quasi-static profiles. The measure of the dynamics-to-static relative depth is defined by: Dd−s=Idyn(ω0)−Istat(ω0) Idyn(ω0)(23) There is a fairly good agreement between the BID and the FFM (see Table 2). Figure 11. The He-βline for T= 1 keV and (a)ne= 5×1023 cm−3; (b)ne= 2×1024 cm−3. Static ions: MERL (red dot), PPP (blue dot); SimU (black dot); BID (solid red); FFM (solid blue). 50x10 -3 40 30 20 10 0 normalized intensity 37203700368036603640 energy(eV) MERL QS BID PPP QS FFM SimU a) 20x10 -3 15 10 5 0 normalized intensity 376037403720370036803660364036203600 energy(eV) MERL QS BID PPP QS FFM SimU b) Atoms 2014,2315 Table 2. Dynamics-to-static relative dip (%) measured on the argon He-βline for T= 1 keV. Models BID FFM Ne= 5 ×1023 cm−358 57 Ne= 1 ×1024 cm−350 51 Ne= 2 ×1024 cm−347 48 4. Conclusions Line shape calculations from different numerical codes that account for the ion dynamics effect were presented. To test the accuracy of the different codes, standardized case problems have been chosen and a systematic cross-comparison has been done. Results from four numerical simulations based on different algorithms and seven models relying on either stochastic or collisional processes, have been then submitted. Surprisingly, the results obtained on the hydrogen Lyman-αline in an ideal OCP plasma consisting of protons presents a large dispersion. While the numerical simulations show a relatively good agreement between each other, the FFM and MMM models systematically display a weaker width than the averaged results. This can be explained by an incomplete description of the ion dynamics effect on the central component of this line. The detailed study on the influence of the microfields directionality in the line shape presented in this volume, [44] or other methods discussed here can help improve the modeling of lines with unshifted components. The overestimate of the UTPP code based on a collisional approach is explained by an incomplete description of ion static effects. The results obtained on the H Lyman-βline present a better agreement between all codes. Concerning the ion dynamics effect on the argon He-αand -βlines, BID and FFM show a different behavior that has been attributed, up to now, to numerical inaccuracies, due to the very weak value of the line intensities. The recently developed numerical simulation code, SimU, could not help discriminate between the two models, but highlighted another problem: it seems that different values of fluctuation rates have to be used to reproduce different portions of the simulated profile. As both the linear and quadratic Stark effect, which are linked to the weak and strong values of microfields, respectively, are involved in producing the shape of this line, one can wonder if a frequency- (or field-) dependent fluctuation rate is needed to give a better description of ion dynamics on this line. Acknowledgments The authors would like to acknowledge the International Atomic Energy Agency B.J. Braams and H.-K. Chung for the organizational and financial support of this workshop. 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