Hindawi Publishing Corporation International Journal of Spectroscopy Volume 2010, Article ID 983578, 7 pages doi:10.1155/2010/983578

Review Article

Pressure Broadening of Some He I Lines

Banaz Omar

Physics Department, Research Center OPTIMAS, Technical University ofKaiserslautern, Erwin Schroedinger Str. 46, 67663 Kaiserslautern, Germany

Correspondence should be addressed to Banaz Omar, omar@rhrk.uni-kl.de Received 29 April 2009; Accepted 12 July 2009 Academic Editor: Roland Stamm

Copyright © 2010 Banaz Omar. This is an open access article distributed under the Creative Commons Attribution License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.

Quantum statistical approach is adopted for calculating the spectral line shapes of neutral helium in dense plasmas. Stark broadening of isolated He I lines 5048 A (21P - 41S), 3889 A (23S - 33P), and 3188A (23S - 43P) is presented. Based on thermodynamic Green's function, the electronic contribution to the shift and width is considered. The participation of ions to the line broadening is treated in a quasistatic approximation, by taking both quadratic Stark effect and quadrupole interaction into account. The calculated shifts and widths are compared with existing data.

1. Introduction

Plasma spectroscopy deals with the characteristics of radiation emitted from a plasma. In dense plasmas, damping of the emitted radiation occurs by means of several mechanisms; the most effective one is pressure broadening (Stark broadening). The interaction between a radiating atom and surrounding perturbing particles leads to Stark broadening. High-speed electrons perturb the emitter by collisions, causing the interruption of the spontaneous emission and altering the emitter energy levels [ 1-4].

Line profile calculation is an interesting tool for both laboratory and astrophysical plasma diagnostics, for example, to determine the internal parameters, to understand the microscopic processes within the plasma, and to check the quality of the predicted experimental and theoretical parameters [1,2].

The emission spectra of helium and He-like ions with their simple atomic structures are interesting for plasma diagnostics such as in shock wave tube or pulsed arc plasmas [5, 6] and in the astrophysical context, for example, stellar atmospheres of hot stars and white dwarfs [7-9]. Helium is used as a carrier gas in many laboratories and is weekly interacting with materials and less harmful for plasma facing components than hydrogen and its isotopes [5]. The He-like ions may exist even at extremely high temperatures and densities. Even ITER is started with helium discharge, also He can be observed in discharge of JET. Spectroscopic

measurements of tokamak plasmas are not free from helium [10].

Various approaches have been investigated to calculate spectral line shapes in plasmas [9, 11-24]. In a semiclassical approach helium lines were calculated by Griem et al. [22, 23], using an impact approximation for electrons with a cutoff procedure, while almost stationary heavy ions are treated in a quasistatic ion approximation due to the static microfield. Also, molecular dynamics (MD) simulations have been performed by Calisti et al. [25] and Gigosos et al. [26] to include the influence of time-dependent microfield by introducing two kinds of simulations for calculating He I Stark line profiles.

Thermodynamic Green's function approach is a powerful tool to describe the Stark broadening [27-30]. In the last two decades, a quantum statistical approach has been developed, taking into account the medium effects by using Green's function [31-36]. In principle, this approach is able to describe dynamical screening and strong collisions by electrons, as well as the dynamic ion microfield, in a systematic way. This quantum statistical approach has been successfully applied to calculate the spectral line shapes of hydrogen, helium, H-, and He-like ions in dense plasmas [37-42].

In this paper thermodynamic Green's function approach is considered to calculate the pressure broadening of some selected neutral helium lines. In Section 2 the definitions and spectral properties of Green's function approach to spectral

line shapes of nonideal plasmas are presented. A review of the basic formalism is introduced and extended to helium lines. Section 3 provides the calculated shifts and full widths at half maximum (FWHM) for nonoverlapping, isolated (non-degenerate) He I lines 5048 A (21P - 4:S), 3889 A (23S- 33P), and 3188 A (23S - 43P) in dense plasmas. Finally, conclusions are given in Section 4.

2. Theoretical Calculations

Microscopic formation of the spectral line shapes in dense plasmas arises from perturbation of the radiative atom by collective and many-body effects [1,4]. Thus, the interaction with the surrounding particles must be taken into account. For example, screening is considered as an important collective effect in plasmas. The influence of electrons and ions may be treated separately due to the difference in mass and mobility. Green's function methods provide a perturbative approach to correlation functions and quantum effects of many-body systems. Two-particle Green's function is used to calculate the line shape and electron broadening from the self-energy and the vertex function. From statistical properties of the system, the current-current correlations determine the absorption spectrum, which is utilized by Ross [27]. Recently, further improvements of this approach have been made by Ropke et al. [32], Hitzschke et al. [33], Gunter et al. [34], and Omar et al. [41].

Optical properties of many-particle systems are specified by the dielectric function e(q, w) based on Green's function theory, which is the response of the medium to an external electromagnetic field. The longitudinal dielectric function is related to the polarization function n(q, w)

£l(q,a) = 1 - Vqn(q,a),

where V(q) = e2/(e0q2) is the Fourier transformed Coulomb potential. In terms of the absorption coefficient a(a) and the index of refraction n(a), the transverse dielectric function £t (q, a) in the long wavelength limit q — Oreads

lim £t(q, a)

n(a) +--a(a)

In the visible region where the wavelength X is large compared with the atomic dimension aB, the transverse and the longitudinal part of dielectric function coincide. The absorption coefficient is proportional to the imaginary part of the dielectric function

a(w) = —limlm e(q, w), cn(w) q- 0

n(w) = -^lim^Re e(q,w) + [(Re e(q,w))2 + »]1/2 j ,

where A denotes (Ime(q, w))2. In thermal equilibrium, the absorption coefficient is related to the emission coefficient by Kirchoff's law [43]. In optically thin plasma, the emission coefficient is proportional to the line emission. As mentioned

above, the dielectric function is related to the polarization function n(q, w). Then the medium modifications of spectral line shapes can be addressed to the bound-bound two-particle polarization function, which concerns to dipoledipole autocorrelation function [36].

The perturber-radiator interaction leads to pressure broadening, which contains electronic and ionic contributions. Describing the ionic contribution in the quasistatic approximation by averaging over the ionic microfield at radiating atom [31, 36, 44], we get

I pr(a)

X If'f (a) dßP(ß)

, ff, Jo

i i', ff

x Im < i

[ha-haif-Yif (a,ß)+irf-1 f'^

Here, the ionic microfield distribution function P(3) is taken according to the Hooper field distribution, and 3 = E/E0 is the normalized field strength [45]. So hwjf = Ej - Ef is the unperturbed transition energy between the initial i and the final f states; i' and f' are the corresponding intermediate states

f ' (a) = (i|r| f)(f '\r\i'}

-ha/ks T

where (i|r| f} is identified as a dipole matrix-element for the transition between i and f states. The line profile itself is determined by the vertex correction rf for the overlapping lines and by the self-energy corrections Z of the initial and final states

Zif (a,ß) = Re [Zi(a,ß) - Zf (a,ß)]

+ iIm [Zi(a, ß) + Z f (a, ß)].

Both electronic and ionic contributions occur in the self-energy Zn(a, ß), which is assumed to be diagonal in the atomic state n;

Z„(a, ß) = Zr ß + Zn1 (a, ß).

The electronic self-energy is obtained by performing a Born approximation with respect to the perturber-radiator interaction [36]

AS„E+irS„E = (n|Zel(£„, ß)|n)

V (q)X|M„„(q)

da Im e 1 (q, a + i0)

,7 [1+ ns(a)] En - Ea(ß) - h(a + iO).

Here, the sum over a runs from n - 2 to n + 2 discrete bound states for virtual transitions, and the level splitting due to the

ion microfield Ea(ft) has been neglected [35]. So nB(w) = [exp(hu>/kBT) - 1]-1 is the Bose distribution function, and Mna(q) are the transition matrix-elements, given below. The inverse dielectric function £-1(q, w) contains many particle effects which account for the dynamical screening of the interaction in the plasma:

Im £ 1 (q, a)

Im £(q, a)

[Re £(q, a)]2 + [Im£(q,a)]2

The random phase approximation (RPA) for the dielectric function is used:

l(q, a) = 1 - 2 V(q) J"

d3p fe (Ep) - fe (Ep+q)

(2n)3 Ep - Ep+q - ñ(a + i0) '

where Ep = h2p2/2me is the kinetic energy of electrons, and fe (Ep) is the Fermi distribution function of the electrons, approximated to the Boltzmann distribution function in the degenerate limit

fe (Ep) S 2 6XP(

h2 p2 2mekBT

The full expression of the inverse dielectric function has to be used if the transition frequency ana becomes comparable to the electron plasma frequency apl = (nee2/e0me)1/2. However, in the high-frequency limit ana » apl, the inverse dielectric function can be approximated by

w \ —Im e( q, a) , ,

Im e—1 (q, a) = . , './ Im £ (q, a). (12)

Inq,a) I

This binary collision approximation leads to a linear behavior of the electronic shift contribution with respect to the electron density, whereas a nonlinear dependence of the electronic shift with increasing electron density is expected if the full expression of the inverse dielectric function is used [33,35].

The vertex function for the coupling between the upper and the lower state is given by

r ; f —

2n f d3q d3p

e2 J (2n)3 (2n)3

fe{Ep) V2

X (q)Mjj(q)Mff (-q) S

h2p ■ q

The transition matrix-elements Mna(q) describe the coupling between free charges and bound states. In lowest order, they are determined by the atomic eigenfunctions fn(p) of the radiating electron and depend on the momentum transfer fiq [34, 46]

Mna (q) :

fn (p)

Zefa p

m¡+me

q-ef4 p+

m¡ + me

assuming that the ion with charge Z is much heavier than the electron m, » me:

Mna (q)

(2n )3

fï (p) [Ze fa (p) - efa (p + q)]

= ie^ZSna -J d3rf„*(r) exp (iq ■ r)fa(r.

(9) Expanding the plane wave into spherical harmonics

exp (iq ■ r) = 4^ X ilji(qr)Y,*m(nq)Ym,(nr), (16)

l=0 m = -l

where ji(qr) is the Bessel function, a multipole expansion can be derived; for example, l = 0, 1, 2 gives the monopole, dipole, and quadrupole contribution of the radiator-electron interaction, respectively. The radial part of helium wave function is calculated based on Coulomb approximation method of Bates and Damgaard [47-49]. For more detail see [41].

By using the Born approximation, the electronic self-energy is overestimated. To avoid this we apply a cutoff procedure and add the strong collision term in contrast to partial summation of the three-particle T-matrix, which is quite suitable for treating short-range interactions between particles [50], where the result might be slightly modified. According to Griem, the cutoff parameter for the q-integration is the inverse of the minimum limiting impact parameter (qmax = 1/pmin) [22, 36, 49, 51].

To determine the ionic self-energy, we approximate the time-dependent microfield fluctuation by its static value. In general, dynamic ionic microfield is important for overlapping lines and at low electron density in the line center [52, 53]. Due to the slow movement of heavy ions, the ion microfield is assumed to be constant during the time of interest for the radiation process. The static ionic contribution to the ionic self-energy is treated by means of the microfield concept including both quadratic Stark effect and quadrupole effects. The first-order perturbation term vanishes for nonhydrogenic like atoms because of nondegeneracy with respect to the orbital quantum number l. According to second-order perturbation theory, the quadratic Stark effect is proportional to the square of the microfield [54]

Y?nlm(E) = e2\E\2 X

|{n, l, m\z\n', l', m')\

n' ,l',m'

Enlm En'Vi

where E is the microfield strength; n, l, and m are the well-known principal, orbital, and magnetic atomic quantum numbers, respectively. The quadrupole Stark effect is due to the inhomogeneity of the ionic microfield. We use the expression derived by Halenka [55]:

Z3nn' (E) = -

2V32n r0 p

eEoBp(ß)(n\3z2 - r2\n'). (18)

Here, Bp(ft) is the mean field gradient at a given field strength, and the screening parameter p = r0/rD is taken as the ratio between the mean particles distance r0 and the Debye radius rD.

ne (1022i

Gigosos et al., independent particles Gigosos et al., interacting paricles Griem

Berg et al. [62] Soltwisch and Kusch [64] Pérez et al. [6]

Milosavljevic and DjeniZe [7] Kelleher [57] Kobilarov et al. [61] Gao et al. [59] Binary approximation

Dynamical screening \ This work

Nonquenching approximation

Figure 1: Stark FWHM for the He I line 3889 A as a function of electron density. A comparison is made with the measured [6, 5661] and other theoretical data [22, 62].

r i $ CP

r A * i

: J ° f # 235 - 33P

........ ...........

1 10 100 1000

ne (1022m-3)

o Gigosos et al., independent particles c Gigosos et al., interacting particles • Berg et al. [62]

Griem x Pérez et al. [6] □ Morris and Cooper [60] ¿ Kelleher [57] + Kobilarov et al. [67]

Binary approximation > Dynamical screening f This work

Nonquenching approximation

Figure 2: Stark shift for the He I line 3889 A as a function of electron density. A comparison is made with the measured [6, 5658, 63] and other theoretical data [22, 62].

3. Results and Discussions

The Stark broadening parameters for the transition (21P -4XS) 5048 A are given in Table 1. Our width wth and shift dth results are compared to calculated values of Bassalo et al. (BCW) [66], measurements of Kelleher [56], and measurements of Diatta [67]. Our calculations agree better with the measured value by Kelleher [56] in contrast to the results given by Bassalo et al. [66]. The measured shift by Diatta [67] is obviously smaller than the calculated shifts given in Table 1.

The Stark width and shift of the line (23 S - 33P) 3889 A are measured by Perez et al. [6]. The measured values were in the plasma density range of (1 - 6) X 1022 m-3 and temperature interval of (0.8 - 3) X 104 K with a mean value of 2 X 104 K. The error bar in the case of ne was ±10%, and the uncertainty in the temperature evaluation was about 20%. Recently, the FWHM of this line is measured by Gao et al. [61] for a helium arc for density range (0.5 - 4) X 1022m-3. Figures 1 and 2 include other available experimental [5660, 63] and theoretical results [22, 62]. The MD simulation results of Gigosos et al. [62] have been performed for independent as well as interacting particles in nonquenching approximation. Our calculations are also presented, the width shows a good agreement especially with the MD simulations data of Gigosos et al. [62], where no Doppler

broadening is included. Nonlinearity can be seen at very high electron density. The discrepancy between the measured and calculated line broadening may be related to self absorption [61]. However, our results for the shift are overestimated, on the other hand better agreement can be seen by comparing our results in non-quenching approximation with the results of Gigosos et al. [62], which give lower values of shift at high electron density.

The Stark parameters of the line (23S - 43P) 3188 A are measured by PeMez et al. [64]. They made a spectroscopic and interferometric analysis of a pulsed plasma. The electron temperature (from 1900 K to 2300 K) was obtained from the intensity ratio of He II lines. Electron density was determined by interferometry, ranging from 1.25 X 1022 m-3 to 6.22 X 1022m-3. From these experimental results an empirical calibration for the Stark parameters was obtained in a broad range of electron densities [64]. The experimental and various theoretical Stark parameters are reported by Pelaez et al. [64], and our results are included in Figures 3 and 4 for Stark width and shift as a function of electron density, respectively, at the given plasma temperatures. Theoretical predictions of Bassalo et al. (BCW) [24] can also be seen in Figures 3 and 4. Further experimental results are presented, carried out by Kelleher [56], Mijatovic' et al. [65], Berg et al. [58], and Soltwisch and Kusch [60]. The measured value of Berg et al. [58] was compared with Griem's theory [58]

Table 1: The calculated FWHM and shift (without/with screening) for the line 5048 A are given; wth and dth this work; wB and dB Bassalo et al. [66]. The experimental wexp and dexp are included [56, 67].

ne Te Wb Wth Wexp dB dth dexp

(1022 m-3)_(103 K)_(A)_(A)_(A)_(A)_(A)_(A)

3.2 30.0 5.22/5.22 5.385/5.378 — 2.19/2.05 2.56/2.397

2.0 18.0 3.10/3.10 3.183/3.179 3.4 1.43/1.35 1.783/1.677 0.9 [67]

1.03±12% 20.9±20% 1.58/1.58 1.623/1.622 1.68 0.75/0.68 0.862/0.82 0.89 [56]

X Pelaez et al. [66]

--Pelaez et al., calibration line

O Mijatovic et al. [67]

A Kelleher [57]

□ Berg et al. [62]

□ Soltwisch and Kusch [64] * Griem

o BCW, Debye screening O BCW, no Debye screening a Binary approximation ") > Dynamical screening I This work ---Nonquenching approximation J

Figure 3: The measured Stark FWHM and calculated values for He I 3188 A line versus electron density. The calculated Stark widths are included from different approaches [22, 24, 56, 58, 60, 64, 65].

at electron density (1.5 ± 0.08) X 1023 m-3 and temperature (2.9 ± 0.2) X 104K.

4. Conclusions

The quantum statistical approach has been developed to calculate spectral line shapes in dense plasmas. By using thermodynamic Green's function, a systematic perturbative treatment of the polarization function has been performed [33, 34, 46]. In contrast to the molecular dynamics (MD) simulations, consistent quantum description is applied here to calculate the Stark parameters by using the formalism presented above. The calculated Stark shift and full width at half maximum (FWHM) of He I lines 5048 A (2*P -4*S), 3889A (23S - 33P), and 3188A (23S - 43P) have been calculated in the density range (1021 - 1024)m-3 and for temperatures between (0.5 - 6) X 104K. In dense plasmas the binary (few-particle) collision approximation

Pelaez et al. [66] Pelaez et al., calibration line O Mijatovic et al. [67]

Kelleher [57] □ Berg et al. [62]

---Griem

* Griem

° BCW, Debye screening ° BCW, no Debye screening Binary approximation

> Dynamical screening I This work

Nonquenching approximation

Figure 4: The measured Stark shift and calculated values for He I 3188 A line versus electron density. The calculated Stark shifts are included from different theoretical approaches [22, 24, 56, 58, 64, 65].

is not appropriate to describe the collective interactions; therefore at high densities the dynamical screening effect will be more important seen (12), which reduces the linearity of Stark parameters with increasing electron density. This affects mostly the shift than the width, and it can be seen in Figures 2 and 4. The Hooper microfield distribution function is applicable for plasmas in the regime r < 1, in which the correlations between plasma particles are considered as small perturbations. This distribution is not applicable in strongly coupling regime, where the correlation effect is important at high density, and therefore a new distribution function should be adopted. Generally, our calculated line widths show good agreement by comparing with other results, while the shift is slightly overestimated for the lines 3889 A and 3188 A. However, by performing nonquenching approximation better agreement can be seen.

Moreover, our quantum statistical approaches can be applied not only to investigate the line shapes of two-electron atom but also to complex atoms. Furthermore, the deformation of spectral line profiles can be investigated in a strong magnetic field for stellar diagnostic.

Acknowledgments

This project is supported by Emmy Noether-Program of the Deutsche Forschungsgemeinschaft, RE1141/11-1. The author would like to thank A. Wierling, G. Ropke, and M. A. Gonzalez for helpful discussions.

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