Issue 
A&A
Volume 535, November 2011



Article Number  A88  
Number of page(s)  12  
Section  Stellar atmospheres  
DOI  https://doi.org/10.1051/00046361/201117491  
Published online  15 November 2011 
Spectral line polarization with angledependent partial frequency redistribution
IV. Scattering expansion method for the Hanle effect
Indian Institute of Astrophysics, Koramangala, 560 034 Bangalore, India
email: sampoorna@iiap.res.in
Received: 16 June 2011
Accepted: 9 September 2011
Context. The partial frequency redistribution (PRD) effects in line scattering are necessary ingredients for interpreting the linear polarization observed in strong resonance lines. It is a common practice to use angleaveraged PRD functions for simplicity (obtained by averaging over all scattering angles). It has been established that the use of angledependent PRD functions instead of angleaveraged functions is essential for weak fields.
Aims. Here we present an efficient iterative method to solve the polarized line radiative transfer equation in weak magnetic fields using angledependent PRD functions.
Methods. Based on the theory of Stokes vector decomposition for the Hanle effect combined with the Fourier azimuthal expansion of the angledependent PRD function, we try to formulate an efficient numerical method of solving the concerned transfer problem in onedimensional media. This iterative method (referred to as the scattering expansion method, SEM) is based on a series expansion of the polarized source vector in mean number of scatterings (Neumann series expansion). We apply the SEM approach to handle both the exact and various approximate forms of the Hanle scattering redistribution matrix.
Results. The SEM is shown to be an efficient method to solve angledependent PRD problems involving the Hanle effect. We show that compared to the earlier methods such as the perturbation methods, the SEM is stable and faster. We find that angledependent PRD significantly affects the Stokes U parameter.
Key words: methods: numerical / polarization / magnetic fields / Sun: atmosphere / line: formation / scattering
© ESO, 2011
1. Introduction
The resonance scattering is responsible for the generation of a linearly polarized solar spectrum (called the second solar spectrum). The magnetic field modifies this linear polarization through the wellknown Hanle effect. The shape of the linear polarization profiles of the spectral lines reveals a great deal of information about the anisotropy that prevails in the solar atmosphere. Equally important is the physics of line scattering – namely the details of the frequency redistribution during scattering. It is wellknown that for a finer analysis of the polarized spectrum, particularly of the strong resonance lines, the angledependent partial frequency redistribution (PRD) is necessary, as shown in the previous papers of this series (Frisch 2010; Sampoorna et al. 2011; Sampoorna 2011b).
The papers mentioned above used a decomposition technique to reduce the nonaxisymmetric Stokes transfer equation to a set of six irreducible components , where K = 0,2 and Q ∈ [−K, + K]. This is achieved through a irreducible spherical tensor expansion of the Hanle phase matrix (see Landi Degl’Innocenti & Landolfi 2004; Frisch 2007). When the PRD function used in the transfer equation is an “angleaveraged function”, are cylindrically symmetric. However, when the PRD function is explicitly angledependent, the are nonaxisymmetric. Frisch (2009) has shown that cylindrical symmetry can be retained by Fourierexpanding the angledependent PRD function over the azimuth angle difference (χ − χ′), where χ and χ′ are the azimuth angles of the outgoing and incoming rays in the atmospheric coordinate system (see Fig. 1). The Fourier azimuthal expansion of the angledependent PRD functions was originally introduced by Domke & Hubeny (1988). This expansion was cleverly used by Frisch (2009) for the Hanlescattering PRD transfer problem. The Fourier expansion of the angledependent PRD function was applied to the nonmagnetic (Rayleigh scattering) problem in Frisch (2010). In this nonmagnetic case there are only four cylindrically symmetric components. The relevant polarized transfer problem was solved in Sampoorna et al. (2011). Recently, Anusha & Nagendra (2011) have generalized to the case of multidimensional media, the Fourier decomposition technique of Frisch (2009) originally formulated for the onedimensional case.
An approximate solution (namely, single scattering approximation) to the Hanle transfer problem with angledependent PRD was presented in Sampoorna (2011b). Here we solve the full Hanle transfer problem in onedimensional media by applying the scattering expansion method (SEM). This method was originally formulated by Frisch et al. (2009) for solving the polarized line transfer equation with complete frequency redistribution (CRD). Subsequently it has been generalized by Sampoorna et al. (2011) to solve the polarized Rayleigh scattering transfer equation with angledependent PRD.
A detailed historical account of the work on angledependent PRD in polarized line transfer is given in Sampoorna et al. (2011). We refer to the same paper for references about early works on transforming the transfer equation from the Stokes vector (I,Q,U) basis to the cylindrically symmetric irreducible basis.
The organization of the paper is as follows. In Sect. 2 we recall the exact and various approximate forms of the Hanle scattering redistribution matrix. In Sect. 3 we briefly recall the decomposition technique of Frisch (2009), but suitably generalized here to accommodate the different forms of the Hanle scattering redistribution matrices discussed in Sect. 2. In Sect. 4 we present the equations of the SEM to solve the relevant transfer problems. The exact form of the Hanle scattering redistribution matrix discussed in Sect. 2 is included in the decomposition technique of Frisch (2009) in Sect. 3. It involves the azimuthal Fourier coefficients on the order of 0, 1, 2, 3, and 4 of the magnetic redistribution functions (see Sampoorna et al. 2007a,b). In Sect. 5 we discuss the properties of these functions. Section 6 is devoted to the results, and the conclusions are given in Sect. 7. An erratum is given in Sect. 8. In Appendix A we present the composite redistribution functions that enter the exact form of the Hanle scattering redistribution matrix. Appendix B contains a listing of the azimuthal Fourier coefficients.
2. Redistribution matrix for the weakfield Hanle scattering
In early works on scattering of radiation on atoms the problem of the frequency redistribution was ignored. For example, the Rayleigh phase matrix for resonance scattering in the absence of magnetic fields was derived by Hamilton (1947, see also Chandrasekhar 1950). In the presence of weak magnetic fields the expression for the Hanle phase matrix was derived by Stenflo (1978) and Landi Degl’Innocenti & Landi Degl’Innocenti (1988).
The problem of frequency redistribution during scattering in the presence of a weak magnetic field and collisions was originally addressed by Omont et al. (1973). However, they did not present the explicit form of the Hanle scattering redistribution matrix. But they remarked that the Hanle effect is operative only in the line core and not in the line wings. Owing to the very short lifetime of the excited level in the wing frequencies, the Hanle effect cannot effectively intervene during the scattering process. On the basis of these results, a heuristic (in the sense that we presume a decoupling of frequency redistribution function, and the angular phase matrix) form for the elements of the Hanle redistribution matrix in the presence of a weak magnetic field B can be written as (1)where i,j = 0,1,2. R(x,x′,Θ) stands for any of the type I, II, or III PRD functions of Hummer (1962), and Θ is the angle between the incoming (Ω′) and outgoing (Ω) rays (see Fig. 1). x and x′ are outgoing and incoming frequencies in Doppler width units. are the elements of the Hanle phase matrix (see Stenflo 1978; Landi Degl’Innocenti & Landi Degl’Innocenti 1988). Equation (1) is valid only in the line core, namely x ≤ x_{c}, where x_{c} denotes the transition frequency between line core and the wings. For x > x_{c}, redistribution matrix is given by Eq. (1) itself but with the Rayleigh phase matrix replacing the Hanle phase matrix. We refer to this division into Hanle and Rayleigh frequency domains as 1D cutoff approximation and x_{c} as 1D cutoff frequency – generally taken to be three Doppler widths. This approximation but with the angleaveraged redistribution function R(x,x′) in Eq. (1) instead of R(x,x′,Θ) was used in several previous works (see e.g., FaurobertScholl 1992; Nagendra et al. 1999).
Fig. 1
Geometry showing the scattering process in the atmospheric coordinate system (Zaxis along the atmospheric normal). The magnetic field makes an angle θ_{B} with respect to the polar Zaxis, and has an azimuth χ_{B}. (θ′,χ′) refer to the incident ray, and (θ,χ) to the scattered ray defined with respect to the polar Zaxis. Θ is the scattering angle. 

Open with DEXTER 
A general PRD matrix that takes into account the effects of elastic collisions in the presence of arbitrary magnetic fields was derived by Bommier (1997). In the weakfield limit (Zeeman splitting of the upper level much smaller than the Doppler width of the line), the coupling of circular polarization to the linear polarization and also to the intensity is weak and can be neglected. The resulting Hanle scattering redistribution matrix is exact in the sense that it does not make use of the frequency domains to represent the transition from Hanle scattering in the line core to the Rayleigh scattering in the line wings. Bommier (1997) refers to it as approximation I, because it is derived only under the “weakfield limit”. Indeed, in approximation I the coupling of frequency redistribution to the linear polarization is kept intact. The angleaveraged version of this approximation I was used in polarized line transfer computations by Sampoorna et al. (2008).
In the present paper we confine our attention only to pure typeII scattering. Thus in the absence of elastic collisions, the angledependent redistribution matrix under approximation I may be written as (see Bommier 1997)(2) Here are irreducible spherical tensors introduced by Landi Degl’Innocenti (1984). The magnetic kernel is of the form (3)Here θ_{B} and χ_{B} represent the orientation of the magnetic field in the atmospheric coordinate system (see Fig. 1). Explicit expressions for the reduced rotation matrices can be found in Landi Degl’Innocenti & Landolfi (2004, Table 2.1, p. 57). For a twolevel atom with an unpolarized lower level and a J → J′ → J scattering transition (where J and J′ are the total angular momentum quantum numbers of lower and upper levels, respectively), takes the form (4)where Γ_{R} is the radiative deexcitation rate, Γ_{I} is the inelastic collisional deexcitation rate, ω_{L} is the Larmor frequency, and g_{J′} is the Landé factor of the upper level. The quantities are defined in Eq. (10.11) of Landi Degl’Innocenti & Landolfi (2004). The composite redistribution functions of typeII () are linear combinations of angledependent magnetic redistribution functions of typeII (see Sampoorna et al. 2007a,b, also Sampoorna 2011a). The explicit form of these functions for a J = 0 → 1 → 0 scattering transition can be found in Appendix A of Sampoorna et al. (2007b). For an arbitrary J → J′ → J scattering transition the are given in Appendix A of the present paper.
For practical applications, Bommier (1997) also derived the socalled approximations II and III, where the 2D frequency space (x,x′) is decomposed into several domains, in each of which the frequency redistribution is “decoupled” from the polarization. Approximation II uses the angledependent PRD functions, and approximation III the corresponding angleaveraged functions of Hummer (1962). The approximations II and III for the Hanle redistribution matrix have been considered in Nagendra et al. (2002, see also Nagendra et al. 2003), where a perturbation method is used to solve the concerned polarized transfer equation. For approximation III a polarized accelerated lambda iteration (ALI) method based on the corewing approach was later developed by Fluri et al. (2003).
Under approximation II and in the absence of elastic collisions, the redistribution matrix is given by Eq. (2), but with the replacement (5)Here the index m ( = 1,2) stands for different (x, x′) frequency domains. Under approximation III the redistribution matrix is given by Eqs. (2) and (5), but with the angledependent redistribution function replaced by the angleaveraged one. The analytic form of the magnetic kernels in different angledependent (approximation II) and angleaveraged (approximation III) frequency domains can be found in Bommier (1997, see also Nagendra et al. 2002; Anusha et al. 2011). It is useful to note that in approximations II and III there is a factorization of frequency redistribution and polarization, so that within a given domain depends only on B, unlike in approximation I which is a nondomainbased theory.
In the 1D cutoff approximation, takes the form (6)where W_{K} is the polarizability factor depending on the Jquantum numbers of the upper and lower levels, and ϵ is the thermalization parameter.
3. A decomposition method for Hanle effect with angledependent PRD
Here we describe the Stokes vector decomposition method, which enables us to write the original “Stokes vector transfer equation” in a simplified form. The simplification takes place because the “decomposed (irreducible) transfer equation” becomes azimuthangleindependent. In fact, this irreducible transfer equation for the cylindrically symmetric Fourier components of the radiation field allows us to formulate an iterative method of solution. Here we present only the essential steps of this decomposition technique. The full details are given in Frisch (2009).
The polarized transfer equation for the Stokes vector can be written in the component form as (7)where Ω (θ,χ) is the ray direction with respect to the atmospheric normal (see Fig. 1) and μ = cosθ. The line optical depth is denoted by τ and ϕ(x) is the normalized Voigt function. The ratio of continuum to line absorption coefficient is denoted by r. The total source vector is given by (8)where S_{c,i} are the components of the unpolarized continuum source vector. We assume that S_{c,0} = B_{ν0}, where B_{ν0} is the Planck function at the line center, and S_{c,1} = S_{c,2} = 0. The line source vector can be written as(9) where Ω′ (θ′,χ′) is the direction of the incoming ray defined with respect to the atmospheric normal, and dΩ′ = sinθ′dθ′dχ′. The primary source is assumed to be unpolarized, so that G_{0}(τ) = ϵB_{ν0} and G_{1}(τ) = G_{2}(τ) = 0.
Frisch (2009) has shown that the Stokes vector and the source vector can be decomposed into six irreducible components and . However, these components continue to be nonaxisymmetric because of the presence of an angledependent PRD function. The problem can be simplified only through the introduction of an azimuthal Fourier expansion of the angledependent PRD function. Using this approach the can also be expanded over the azimuth χ as (10)with similar expansions for and (see Frisch 2009, for details). The Fourier coefficients satisfy a nonLTE transfer equation similar to Eq. (7), with the source term given by Eq. (8), but with and instead of S_{l,i} and S_{c,i}. Because the continuum is assumed to be unpolarized, . The Fourier coefficients of the line source vector are given by (11) where the primary source term , and k and k′ together satisfy the condition k′ = k + Q′ − Q′′. From this condition, it follows that for a given value of k, the values of k′ get restricted to k − 4 ≤ k′ ≤ k + 4. The nonzero azimuthal Fourier coefficients are of the form (12)with K and K′ both even or both odd. are a combination of trigonometric functions, and are given by . The analytic form of the magnetic kernel in the Fourier basis depends on the level of approximation used to represent the Hanle redistribution matrix (see Sect. 2 for details). Below we present the form of for different choices of approximation levels (1D cutoff, approximations II and I of Bommier 1997).
In the 1D cutoff approximation(13) The Fourier coefficients of the angledependent PRD function are given by Eq. (14) of Frisch (2009, see also Eq. (8) of Sampoorna 2011b).
The difficulty in implementing the approximation II in the decomposition method given above was discussed in Sampoorna (2011b). Basically the domains of approximation II depend on both the frequencies (x,x′) and the scattering angle Θ, while we work in the Fourier basis which is inherently azimuthangle independent. To handle this difficulty, Sampoorna (2011b) used the angleaveraged frequency domains of approximation III, but continued to use the angledependent PRD functions of Hummer (1962). With this simplification for approximation II is given by (14)For approximation I (nondomainbased PRD theory) the is given by Eqs. (3) and (4), but with replaced by . In this case, the Fourier azimuthal expansion is applied to the ‘magnetic redistribution functions’ instead of the Hummer’s PRD functions.
Notice that the range of k values extend a priori from − ∞ to + ∞, which produces an infinite set of integral equations for . A numerical solution is possible only if we truncate this infinite set. In practice the number of Fourier coefficients required is determined by the number of terms needed to accurately represent the angledependent PRD function. For the typeII PRD function of Hummer (1962), Domke & Hubeny (1988) have shown that at least five terms are needed to represent the exact value of the function to a sufficient accuracy. Thus for k = 0, ± 1, ± 2, ± 3, ± 4, we obtain a set of 54 coupled integral equations. In the following section we present an iterative method called the SEM to solve Eq. (11) efficiently (see Frisch et al. 2009; Sampoorna et al. 2011).
4. Scattering expansion method for Hanle effect with angledependent PRD
Here we present an iterative method based on a Neumann series expansion of the components of the source vector contributing to the polarization. This iterative method was referred to as SEM by Sampoorna et al. (2011), who applied it to the nonmagnetic polarized line transfer problem with angledependent PRD. Indeed, these authors showed that this method is faster than the corewingbased polarized ALI method.
The Neumann series amounts to an expansion in terms of the mean number of scattering events (see Frisch et al. 2009). Its first term yields the socalled “single scattered solution”. For Rayleigh scattering with angledependent PRD the single scattering approximation to the polarized source vector components was presented by Frisch (2010). For the Hanle effect with angledependent PRD the corresponding approximation was presented recently by Sampoorna (2011b). The inclusion of higherorder terms in the Neumann series allows us to include multiple scattering effects in the expression for the polarized source vector components.
We first neglect polarization in the calculation of Stokes I, i.e., we assume that Stokes I is cylindrically symmetric and is given by the component itself to an excellent approximation. This component is the solution of a nonLTE unpolarized radiative transfer equation with the line source vector given by(15)where , , and . Equation (15) can be solved using a scalar ALI method based on a corewing approach. Keeping only the contribution of on the RHS of Eq. (11) to the K = 2 Fourier coefficients, we can show that values of k are limited to k = 0, ± 1, and ± 2 (see Sampoorna 2011b). Thus the single scattering approximation for each component can be written as (16)The superscript 1 stands for the single scattering approximation to the polarized component of the source vector. The corresponding radiation field for k = 0, ± 1, ± 2 is calculated with a formal solver and it serves as a starting solution for calculating the higherorder terms.
Fig. 2
Azimuthal Fourier coefficients of typeII plotted as a function of the outgoing frequency x for different choices of μ and μ′. Left panels show and right panels show . The damping parameter a = 0.001. Thin lines correspond to x′ = 1 and thick lines to x′ = 4. Solid, dotted, dashed, dotdashed, and dashtripledotted lines correspond to k = 0,1,2,3, and 4, respectively. For notational brevity we simply dropped the M dependence on the ytitle of the plotted functions. 

Open with DEXTER 
The higherorder terms can be obtained by substituting for appearing in the RHS of Eq. (11), from . Clearly, as in the single scattering approximation, we continue to set k′ = 0, but include the coupling of (K = 2,Q) components with other polarization components (K′ = 2,Q′′) that were neglected in the single scattering approximation. However, we neglect the coupling of the Fourier components k with other k′0 Fourier components, eventhough k′ = ± 1 and ± 2 Fourier components are available from the single scattered solution. The advantage of retaining only the k′ = 0 term in the RHS of Eq. (11) is that the value of k, which is now decided by the condition k = Q′′ − Q′, is now limited to 0, ± 1, ± 2, ± 3, and ± 4. In other words, only four more values of k are needed to account for higherorder terms compared to the single scattering approximation. Consequently, the inclusion of higherorder terms increases the number of the K = 2 Fourier coefficients that contribute to the source vector from 25 for single scattering to 45 for higher orders of scattering. We have verified that retaining the coupling of k with, say, k′ = ± 1 Fourier components does not lead to significant changes in the converged solution that was obtained when we kept only k′ = 0 components. This clearly shows that the coupling of k to k′ = 0 is the dominant one, while the coupling to other k′0 Fourier components is negligible, and if retained, it only increases the dimensionality of the problem (without any increase in accuracy) because of the condition k′ = k + Q′ − Q′′. The at order n are given by (17) with k = Q′′ − Q′. Notice that are zero for k = ± 3 and ± 4. The explicit forms of are given in Appendix B.
5. Azimuthal Fourier coefficients of magnetic redistribution functions
Extension of the decomposition technique of Frisch (2009) to the Hanle redistribution matrix given by approximation I (see Sect. 2), involves the application of the Fourier azimuthal expansion to the magnetic redistribution functions (see Sect. 3 and Appendix A). For a J = 0 → 1 → 0 scattering transition there are six components of typeII magnetic redistribution functions. They are denoted by , where X stands for H (Voigt type) or F (FaradayVoigt type), and M = 0, ± 1. We denote the corresponding azimuthal Fourier coefficients by . We note that and are normalized to the corresponding magnetically shifted Voigt and FaradayVoigt profile functions. All k0 components are normalized to zero.
The method of computation of azimuthal Fourier coefficients of Hummer’s redistribution functions are discussed in detail in Sect. 4 of Sampoorna et al. (2011). The same method has been appropriately extended to compute the azimuthal Fourier coefficients of magnetic redistribution functions. Hence we do not again repeat those details here.
For a weak magnetic field (Hanle Γ = 1), different M components of typeII function differ very little (graphically indistinguishable). These differences are relevant when the difference of two such components is formed in the composite redistribution functions (see Eq. (A.2)). These difference quantities are responsible for a smooth switchover from Hanle scattering in the line core to the Rayleigh scattering in the wings. Therefore we show only the azimuthal Fourier coefficients for k = 0,1,2,3, and 4 in Fig. 2.
From the left panels of Fig. 2 we see that the behavior of for k = 0,1, and 2 are identical to those presented in Fig. 2 of Sampoorna et al. (2011). As expected, the k = 3 and k = 4 components are much smaller than the k = 0 component, except for forward and backward scattering (see Figs. 2b and 2c). The function takes both positive and negative values not only for k0 but also for k = 0, because it involves FaradayVoigttype functions. For forward and backward scattering, exhibits sharp peaks at  x  = 1 when x′ = 1. On the other hand, for forward scattering the function exhibits a zero crossover at  x  = 1 when x′ = 1 (see Fig. 2e), which is typical of the behavior of FaradayVoigt functions. However, for backward scattering, shown in Fig. 2f does not show a crossaver at  x  = 1. For x′ = 4, behave similar to the corresponding (namely dominance of the frequency coherent nature of typeII function).
6. Results and discussions
We considered isothermal, selfemitting planeparallel atmospheres with no incident radiation at the boundaries. These slab models are characterized by (T,a,ϵ,r), where T is the optical thickness of the slab. The Planck function at the line center B_{ν0} is taken as unity. A logarithmic depth grid with five points per decade is used, with the first depth point at τ_{1} = 10^{4}. For the frequency grid we used equally spaced points in the line core and logarithmically spaced ones in the wings. Furthermore, the maximum frequency x_{max} was chosen such that the condition ϕ(x_{max})T ≪ 1 is satisfied. We have typically 70 points in the interval [0,x_{max}] . We used a sevenpoint Gaussian quadrature in [0 < μ ≤ 1].
6.1. Comparison with the perturbation method
In this section we compare the emergent solutions obtained from the SEM approach for angledependent PRD Hanle transfer problem presented in Sect. 4 and the corresponding solution computed from an independent method, namely the perturbation method of Nagendra et al. (2002). We present this comparison for 1D cutoff approximation (Sect. 6.1.1), approximation II (Sect. 6.1.2), and approximation I (Sect. 6.1.3).
We recall that the method presented in Nagendra et al. (2002) solves the polarized transfer equation with angledependent PRD and Hanle effect perturbatively in the Stokes vector basis. In this method it is necessary to discretize the azimuth χ of the radiation field apart from the frequency x and orientation θ. As a result, the CPU and memory requirements for this method are pretty high compared to the SEM approach described in the present paper (because in the SEM we do not have to discretize the azimuth χ).
For all figures presented in this section, a = 10^{3}, ϵ = 10^{3}, r = 0 (pure line case), and the line of sight is defined by μ = 0.11 and χ = 0°. The magnetic field parameters are taken as Γ = 1, θ_{B} = 30°, and χ_{B} = 0°. For the perturbation method we used a 16 point trapezoidal grid for χ ∈ [0,2π].
Fig. 3
Comparison of the multiple scattered solution from the SEM (solid lines) and of that from the perturbation method (dashed lines). Dotted lines represent the single scattered solution. The 1D cutoff approximation is used with x_{c} = 3. The model parameters are (a,ϵ,r) = (10^{3},10^{3},0) and the magnetic field parameters are (Γ,θ_{B},χ_{B}) = (1,30°,0°). The line of sight is represented by μ = 0.11 and χ = 0°. Panel a) corresponds to T = 1 and panel b) to T = 10^{4}. The positive Q direction corresponds to the linear polarization perpendicular to the solar limb. 

Open with DEXTER 
6.1.1. 1D frequency cutoff approximation
Here we present the emergent solution computed with a 1D cutoff approximation for the Hanle redistribution matrix (see Sect. 2 for more details). A 1D cutoff frequency with x_{c} = 3 Doppler widths was used.
Figure 3 shows the log I, Q/I, and U/I for T = 1 (panel (a)), and T = 10^{4} (panel (b)). The solid line shows the multiple scattered solution from the SEM approach, and the dashed line shows the corresponding multiple scattered solution from the perturbation method. The single scattered solution is shown as a dotted line for comparison. Spikes or dents observed around x = 3 are caused by the abrupt cutoff used. Clearly, the multiple scattered solution from the SEM approach compares fairly well with the corresponding solution from the perturbation method. The slight differences noticed around the line center are caused by the finite resolution of the azimuth angle grid used in the perturbation method (with 16 points). We have verified that these differences decrease when we increase the number of azimuth points from 16 to 36, but at the cost of huge memory and CPU time. In the SEM approach the transfer problem is solved on a basis of azimuthindependent (reduced) Fourier coefficients. The azimuth dependence is finally recovered when transforming into the Stokes vector basis (see our Eq. (10), and Eqs. (B.1)–(B.3) of Frisch 2007).
6.1.2. 2D frequency domains
Here we present the solutions computed using the domainbased Hanle scattering redistribution matrix (approximation II) discussed in Sect. 2. Figure 4 shows the emergent solutions for T = 1 (panel (a)), and T = 10^{4} (panel (b)). The solid lines again represent the multiple scattered solution from SEM approach, and the dashed lines represent the corresponding solution from the perturbation method. We recall that angleaveraged frequency domains of approximation III with angledependent PRD functions are used in the SEM approach, while the actual approximation II (angledependent frequency domains) of Bommier (1997) is used in the perturbation method.
CPU time requirements for the SEM approach proposed in this paper and the perturbation method of Nagendra et al. (2002) for different values of optical thickness T.
Fig. 4
Same as Fig. 3, but with 2D frequency domains of Bommier (1997) in the Hanle PRD matrix. 

Open with DEXTER 
As for the 1D cutoff approximation, the differences observed near the line center between the multiple scattered solution from the SEM approach and the perturbation method are caused by the finite resolution of the χ grid in the perturbation method. However, considerable differences are observed between the two solutions in the transition region 3 ≤ x ≤ 4. These differences are not caused by the finite resolution of the χ grid in the perturbation method. But they are caused by the use of angleaveraged frequency domains to solve the angledependent PRD transfer problem in the SEM approach. However, there seems to be no way to include selfconsistently the angledependent frequency domains explicitly in the SEM approach. Our attempts to derive azimuthaveraged frequency domains were not successful, and still remain an open theoretical problem. Nevertheless, the SEM approach is shown to be numerically superior to the perturbation method, as can be seen from Table 1.
In Table 1 we compare the CPU time requirements for SEM and perturbation method for T = 1,10,100,10^{3}, and 10^{4}. From Table 1 we see that the SEM approach is faster than the perturbation approach, particularly for slabs of larger optical thickness T. This is because as T increases, the perturbation method converges slowly, because it is basically a classical lambda iteration on Stokes source vector components S_{Q} and S_{U}, and actually fails to converge for higher values of T, whereas the SEM approach works for any value of T and for any choice of the model parameters. Because the starting solution, namely the single scattered solution, is already a good approximation to the full solution (compare solid and dotted lines in Figs. 3–5), the SEM converges faster and thereby requires less CPU time. Moreover, the SEM approach requires about 1 GB of main memory, while the perturbation method requires about 11 GB for the same line transfer problem.
Fig. 5
Comparison of the multiple scattered solution from the SEM (solid lines) and that from the perturbation method (dashed lines). Dotted lines represent the single scattered solution. Approximation I (nondomainbased PRD) is used for the SEM approach, while approximation II (2D angledependent frequency domains) is used in the perturbation method. Other model parameters are the same as in Fig. 3. 

Open with DEXTER 
Fig. 6
The emergent I, Q/I, and U/I profiles at μ = 0.11 and χ = 0° computed for the angleaveraged (dashed lines) and the angledependent (solid lines) nondomainbased PRD. Panel a): thin lines T = 20, medium thick lines T = 200, and thick lines T = 2 × 10^{3}. Panel b): thin lines T = 2 × 10^{4}, medium thick lines T = 2 × 10^{6}, and thick lines T = 2 × 10^{8}. Other model parameters are (a,ϵ,r) = (10^{3},10^{4},0). The absolute differences Δ(Q/I) and Δ(U/I) in percentage are also shown. 

Open with DEXTER 
6.1.3. Nondomainbased PRD theory
Figure 5 shows a comparison between the emergent solutions computed using approximation I (nondomainbased PRD) in the SEM approach (solid lines) and the approximation II (domainbased PRD) in the perturbation method (dashed lines). For thin slabs (panel (a)) both solutions match at all the frequencies, except near the line center, which as before is caused by the finite resolution of the χ grid in the perturbation method. For thicker slabs (panel (b)) we note that Q/I is nearly insensitive to the frequency space decomposition, while U/I shows some difference particularly at the transition region 3 ≤ x < 4. The nondomainbased PRD theory produces smoother U/I profiles at all frequencies, while the domainbased PRD theory produces sharp peaks at the transition region between the line core and line wings owing to abrupt cutoffs.
6.2. Hanle Stokes profiles computed with angledependent and angleaveraged nondomainbased PRD matrix
Following Sampoorna et al. (2011, see however Sect. 8, here we present a comparison of emergent Hanle Stokes profiles computed with angledependent and angleaveraged PRD functions for several atmospheric parameters. For this purpose we consider the nondomainbased PRD matrix (approximation I) of Bommier (1997). The angleaveraged version of this PRD matrix has been implemented in a polarized ALI code in Sampoorna et al. (2008). We used this code to compute the angleaveraged solutions, while the corresponding angledependent solutions were computed using the SEM approach presented in this paper.
For a study of the differences between angledependent and angleaveraged emergent solutions, we consider a standard atmospheric model (T,a,ϵ,r) = (2 × 10^{3},10^{3},10^{4},0) around which we vary the various atmospheric parameters one at a time, keeping other parameters fixed. For all figures presented in this section the magnetic field parameters are (Γ,θ_{B},χ_{B}) = (1,30°,0°). Furthermore, in all figures of this section the solid lines represent the angledependent solutions and the dashed lines represent the corresponding angleaveraged solutions.
6.2.1. Effect of optical thickness T
In Fig. 6 we compare the emergent I, Q/I, and U/I profiles computed with angleaveraged (dashed lines) and the angledependent (solid lines) nondomainbased PRD matrix for different values of optical thickness T. We cover a range of optical thickness from thin slabs (T = 20) to very thick slabs (T = 2 × 10^{8}). Below each of the Q/I and U/I panels we also plot the absolute difference Δ(X/I) =  (X/I)_{AD} − (X/I)_{AA}  in percentage, where X stands for Q or U and the acronyms AD for angledependent and AA for angleaveraged.
As the optical thickness T increases, the amplitude of the near wing peak in Q/I initially increases until T = 2 × 10^{4}. For T > 2 × 10^{4} the near wing peak amplitude decreases. This trend is also followed by the absolute difference Δ(Q/I). The biggest differences are noted for T = 2 × 10^{3}, however. The U/I profiles on the other hand show considerable differences in their shapes themselves for all values of T. Only for T = 20 the angledependent and angleaveraged solutions match near the line center. For other values of T differences are observed for all frequencies in the range 0 ≤ x ≤ 5. The absolute difference Δ(U/I) is most pronounced for T = 20. Consequently, angledependent PRD effects are more important for U/I profiles than for Q/I profiles.
It is interesting to note that the U/I profiles for T ≥ 2 × 10^{4} are all identical. Moreover, the intensity I and Q/I in the line core are nearly the same for these optical thicknesses. This behavior can perhaps be explained with the concept of thermalization depths and thermalization frequencies (Frisch 1980). The thermalization depth τ_{th} defines the depth below which the source function for Stokes I departs from the Planck function, and above which the source function is equal to the Planck function. The thermalization frequency x_{th} defines the frequency below which the source function equals the Planck function for τ > τ_{th}, and above which the source function departs from the Planck function at all depths. In the case of angleaveraged typeII redistribution function of Hummer (1962), Frisch (1980) and Hubený (1985) show that the thermalization depth and thermalization frequency in the line core are and , while in the line wings they are and , respectively. For a = 10^{3} and ϵ = 10^{4} we have , , , and . Clearly, all photons with frequencies are thermalized for T ≥ 2 × 10^{4}, which explains the observed behavior of I, Q/I, and U/I at these frequencies.
Fig. 7
The emergent I, Q/I, and U/I profiles at μ = 0.11 and χ = 0° computed for the angleaveraged (dashed lines) and the angledependent (solid lines) nondomainbased PRD. Panel a): thin lines ϵ = 10^{2}, medium thick lines ϵ = 10^{6}, and thick lines ϵ = 0. Panel b): thin lines r = 10^{8}, medium thick lines r = 10^{6}, and thick lines r = 10^{4}. Other model parameters are (T,a) = (2 × 10^{3},10^{3}). For panel a) r = 0, and for panel b) ϵ = 10^{4}. The absolute differences Δ(Q/I) and Δ(U/I) in percentage are also shown. 

Open with DEXTER 
6.2.2. Effects of the thermalization parameter ϵ and the continuum strength parameter r
Figure 7a shows the effect of ϵ on the difference between the angledependent and angleaveraged emergent solutions. As expected, the intensity I increases with an increase in ϵ, while the degree of polarization (both Q/I and U/I) decreases. The differences between Q/I profiles computed with the angledependent and angleaveraged PRD essentially decrease at all frequencies as ϵ increases from 10^{6} to 10^{2}. But for the U/I profiles the differences decrease for  x  ≤ 3, beyond which the differences are the same for both ϵ = 10^{6} and 10^{2}. In the same figure we also show the case of conservative scattering (ϵ = 0). Here an unpolarized incident radiation is given as the lower boundary condition, namely, , because there is no primary source of photons. The emergent Q/I and U/I are confined to the line core (  x  ≤ 3), where we observe some differences between the angledependent and angleaveraged cases.
The effect of the continuum strength parameter r on the differences between angledependent and angleaveraged profiles is shown in Fig. 7b. As in the nonmagnetic case (see Fig. 11 of Sampoorna et al. 2011), there is a gradual decrease of the differences between angledependent and angleaveraged Q/I profiles with an increase in r, particularly at the near wing maxima. The U/I profiles on the other hand show only a small sensitivity to r in the frequency range 2 < x < 5, where the differences also decrease with an increase in r.
Fig. 8
The emergent I, Q/I, and U/I profiles for different values of the heliocentric angle computed for the angleaveraged (dashed lines) and the angledependent (solid lines) nondomainbased PRD. The atmospheric model used is (T,a,ϵ,r) = (2 × 10^{3},10^{3},10^{4},0). The absolute differences Δ(Q/I) and Δ(U/I) in percentage are also shown. 

Open with DEXTER 
6.2.3. Centertolimb variations
As in Sampoorna et al. (2011), we show in Fig. 8 the centertolimb variation of the emergent I, Q/I, and U/I profiles and also of the difference between angledependent and angleaveraged polarization profiles. Clearly as μ → 1 the absolute differences in both Q/I and U/I tend to zero. However, there are significant differences in the shapes of the U/I profiles computed with angledependent and angleaveraged PRD. Also the magnitude of Q/I profiles computed with angledependent PRD is smaller than those computed with angleaveraged PRD, while the opposite is the case for U/I profiles. It is interesting to note that the amplitude of the minima in angledependent U/I at x = 3 seems to increase as μ changes from 0.7 to 0.97.
7. Conclusions
We have developed an iterative method based on the Neumann series expansion of the polarized source vector components to solve the complex transfer problem with angledependent PRD and Hanle effect. This method, originally developed by Frisch et al. (2009) for CRD problems, was generalized to the angledependent PRD nonmagnetic transfer problems by Sampoorna et al. (2011), who referred to it as the scattering expansion method (SEM). Thanks to the decomposition method developed by Frisch (2009), we were able to formulate here an efficient iterative method to solve this complex problem. In this method, the polarized radiation field is first decomposed into six irreducible components, which remain nonaxisymmetric because of the use of angledependent PRD function, however. These nonaxisymmetric components are then reduced to 6 × (2n_{k} − 1) Fourier components using a Fourier azimuthal expansion of the angledependent PRD function (where n_{k} is the number of positive k values including zero). Clearly, one obtains an infinite set of integral equations for the Fourier components of the irreducible source vector because k in general takes values from − ∞ to + ∞. Sampoorna (2011b) showed that the number of Fourier components can be limited to 26 when one applies the single scattering approximation (see e.g., Frisch et al. 2009). This is because the value of k is limited to k = 0, ± 1, ± 2 in this case. The single scattering approximation gives a reasonable approximation to the full solution. We showed how to include higherorder terms to develop the SEM approach as a solution technique. Including higherorder terms increases the number of Fourier components to 46 because k now takes values 0, ± 1, ± 2, ± 3, and ± 4. For the Hanle scattering redistribution matrix, we have considered both the exact (approximation I of Bommier 1997) and approximate (approximation II of Bommier 1997, 1D cutoff approximation) forms. We confined our attention only to pure typeII scattering.
We have shown that the SEM approach is computationally more efficient (see Table 1) than the perturbation method of Nagendra et al. (2002). When a 1D cutoff approximation is used for the Hanle redistribution matrix, both the SEM approach and the perturbation method give nearly the same solutions. However, the differences between the solutions obtained from both the methods occur near the transition region 3 ≤ x ≤ 4, when the approximation II of Bommier (1997) is used. The reason is that in the SEM approach angleaveraged frequency domains are used for handling the angledependent transfer problem, while actual angledependent frequency domains are used in the perturbation method. Because the SEM approach is devised based on azimuthally symmetric Fourier components, the actual angledependent frequency domains cannot be implemented in this approach. It needs the derivation of azimuthaveraged frequency domains, which is beyond the scope of the present paper. In spite of this difficulty, we have shown that SEM approach is still able to handle angledependent transfer using angleaveraged frequency domains to a sufficient accuracy. Furthermore, the SEM approach can handle slabs of any optical thickness, while the older perturbation method suffers from convergence problems for thick slabs because it essentially is a method based on classical lambda iteration on the linear polarization components of the source vector.
We have carried out a detailed numerical study to analyze the role of angledependent PRD effects. For this purpose we have used the angledependent and angleaveraged versions of the nondomainbased PRD matrices (approximation I) of Bommier (1997). In the presence of a weak magnetic field the Q/I profiles computed with angledependent and angleaveraged PRD show significant differences both around the line core and near wing maxima for T ≤ 2 × 10^{3}. For T ≥ 2 × 10^{4} the differences are small and appear mainly near the line core. The U/I profiles on the other hand show significant differences in the shape itself at all optical depths and almost at all frequencies. Therefore we reconfirm the conclusions of Nagendra et al. (2002) that the U/I profiles are highly sensitive to the angledependence of the PRD function, and should be taken into account for magnetic field determination based on Hanle effect.
8. Erratum
Figures 6–8 and Figs. 10–12 of Sampoorna et al. (2011) are slightly erratic, and consequently the conclusions drawn based on them. These figures show the comparison of the nonmagnetic Stokes Q and Q/I profiles computed with angledependent (solid lines) and angleaveraged (dashed lines) PRD functions. The error lies in the fact that these comparisons were not made on the same footing. The angleaveraged functions in Sampoorna et al. (2011) were computed using the method described in Gouttebroze (1986) combined with the frequency grid refinement discussed in Sect. 4 of Sampoorna et al. (2011). In the present paper we calculated the angleaveraged PRD functions by explicitly angleaveraging the corresponding angledependent PRD functions (see Eqs. (103) and (104) of Bommier 1997), using a 31point GaussLegendre quadrature. This method of computing the angleaveraged PRD function is also combined with the frequency grid refinement discussed in Sect. 4 of Sampoorna et al. (2011). We found that these two different methods of computing the same angleaveraged function give slightly different emergent Stokes Q profiles. This in turn affects the difference between the Q/I profiles computed with the angledependent and angleaveraged PRD functions. We note that Stokes I is not much affected by any of the two methods used for computing angleaveraged PRD function.
We think that computing the angleaveraged functions by explicit angleaveraging is on par with the computation of corresponding angledependent functions because the error made (if any) in the computation will be on a similar order. Consequently, only one conclusion of Sampoorna et al. (2011, see last two sentences in their abstract and first two sentences of last but one paragraph of their conclusions section) is incorrect. Instead that conclusion should read as follows: the relative difference in the emergent polarization rate Q/I computed with angledependent and angleaveraged PRD functions is between 10% and 30% for slabs with optical thickness 20 ≤ T ≤ 2 × 10^{3}, the largest differences occurring in the near wing peaks. For slabs of optical thickness T ≥ 2 × 10^{4} the differences are comparatively smaller (and occur only around the line core) and therefore angleaveraged PRD functions can safely be used. These conclusions now agree with the conclusions of the present paper and those of Nagendra et al. (2002) and Faurobert (1987, 1988).
References
 Anusha, L. S., & Nagendra, K. N. 2011, ApJ, 739, 40 [NASA ADS] [CrossRef] [Google Scholar]
 Anusha, L. S., Nagendra, K. N., Bianda, M., et al. 2011, ApJ, 737, 95 [NASA ADS] [CrossRef] [Google Scholar]
 Bommier, V. 1997, A&A, 328, 726 [NASA ADS] [Google Scholar]
 Chandrasekhar, S. 1950, Radiative transfer (Oxford: Clarendon Press) [Google Scholar]
 Domke, H., & Hubeny, I. 1988, ApJ, 334, 527 [NASA ADS] [CrossRef] [Google Scholar]
 Faurobert, M. 1987, A&A, 178, 269 [NASA ADS] [Google Scholar]
 Faurobert, M. 1988, A&A, 194, 268 [NASA ADS] [Google Scholar]
 FaurobertScholl, M. 1992, A&A, 258, 521 [NASA ADS] [Google Scholar]
 Fluri, D. M., Nagendra, K. N., & Frisch, H. 2003, A&A, 400, 303 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Frisch, H. 1980, A&A, 83, 166 [NASA ADS] [Google Scholar]
 Frisch, H. 2007, A&A, 476, 665 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Frisch, H. 2009, in Solar Polarization 5, ed. S. V. Berdyugina, K. N. Nagendra, & R. Ramelli (San Francisco: ASP), ASP Conf. Ser., 405, 87 [Google Scholar]
 Frisch, H. 2010, A&A, 522, A41 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Frisch, H., Anusha, L. S., Sampoorna, M., & Nagendra, K. N. 2009, A&A, 501, 335 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Gouttebroze, P. 1986, A&A, 160, 195 [NASA ADS] [Google Scholar]
 Hamilton, D. R. 1947, ApJ, 106, 457 [NASA ADS] [CrossRef] [Google Scholar]
 Hubený, I. 1985, A&A, 145, 461 [NASA ADS] [Google Scholar]
 Hummer, D. G. 1962, MNRAS, 125, 21 [NASA ADS] [CrossRef] [Google Scholar]
 Landi Degl’Innocenti, E. 1984, Sol. Phys., 91, 1 [NASA ADS] [CrossRef] [Google Scholar]
 Landi Degl’Innocenti, M., & Landi Degl’Innocenti, E. 1988, A&A, 192, 374 [NASA ADS] [Google Scholar]
 Landi Degl’Innocenti, E., & Landolfi, M. 2004, Polarization in Spectral Lines (Dordrecht: Kluwer) [Google Scholar]
 Landi Degl’Innocenti, E., Bommier, V., & SahalBréchot, S. 1991, A&A, 244, 391 [NASA ADS] [Google Scholar]
 Nagendra, K. N., Paletou, F., Frisch, H., & FaurobertScholl, M. 1999, in Solar Polarization, ed. K. N. Nagendra, & J. O. Stenflo (Boston: Kluwer), 127 [Google Scholar]
 Nagendra, K. N., Frisch, H., & Faurobert, M. 2002, A&A, 395, 305 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Nagendra, K. N., Frisch, H., & Fluri, D. M. 2003, in Solar Polarization, ed. J. Trujillo Bueno, & J. Sanchez Almeida (San Francisco: ASP), ASP Conf. Ser., 307, 227 [Google Scholar]
 Omont, A., Smith, E. W., & Cooper, J. 1973, ApJ, 182, 283 [NASA ADS] [CrossRef] [Google Scholar]
 Sampoorna, M. 2011a, ApJ, 731, 114 [NASA ADS] [CrossRef] [Google Scholar]
 Sampoorna, M. 2011b, A&A, 532, A52 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Sampoorna, M., Nagendra, K. N., & Stenflo, J. O. 2007a, ApJ, 663, 625 [NASA ADS] [CrossRef] [Google Scholar]
 Sampoorna, M., Nagendra, K. N., & Stenflo, J. O. 2007b, ApJ, 670, 1485 [NASA ADS] [CrossRef] [Google Scholar]
 Sampoorna, M., Nagendra, K. N., & Frisch, H. 2008, J. Quant. Spec. Radiat. Transf., 109, 2349 [NASA ADS] [CrossRef] [Google Scholar]
 Sampoorna, M., Nagendra, K. N., & Frisch, H. 2011, A&A, 527, A89 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Stenflo, J. O. 1978, A&A, 66, 241 [NASA ADS] [Google Scholar]
Appendix A: Composite redistribution functions of typeII
The composite redistribution function of typeII, are obtained after applying the Doppler broadening to the rest frame quantity of Bommier (1997, see her Eq. (81)), where are generalized profile functions (see Landi Degl’Innocenti et al. 1991). For a J → J′ → J scattering transition, it takes the form(A.1)where M,M′ and N denote the magnetic substates of the upper level J′ and the lower level J, respectively. The magnetic redistribution functions and are defined in Eqs. (24)–(26) of Sampoorna (2011a), but with the energy conservation term x_{NN′′} set to zero because it is neglected in approximation I (see Sect. 4.1 of Bommier 1997). Here “H” stands for Voigt type and “F” for FaradayVoigt type functions.
In the present paper we considered only a J = 0 → 1 → 0 scattering transition. In this case the explicit form of are listed in Appendix A of Sampoorna et al. (2007b), where it is denoted by the symbol . For easy reference we list them here in a slightly different form (namely, M,M′ here corresponds to − q and − q′ of Sampoorna et al. 2007b). (A.2)
Appendix B: The azimuthal Fourier coefficients
The azimuthal Fourier coefficients are defined in Eq. (12). It is easy to verify that they satisfy the following properties (B.1)(B.2)Owing to the abovementioned symmetry relations, there are only 13 independent coefficients. For i = 0,1 and the reference angle γ = 0 (see Landi Degl’Innocenti & Landolfi 2004), the form of are given in Eq. (A.6) of Frisch (2010). For i = 2 and the reference angle γ = 0, are given by (B.3)Using Eq. (A.6) of Frisch (2010) and our Eq. (B.3) in Eq. (12), we obtain the following explicit form for these coefficients : (B.4)
All Tables
CPU time requirements for the SEM approach proposed in this paper and the perturbation method of Nagendra et al. (2002) for different values of optical thickness T.
All Figures
Fig. 1
Geometry showing the scattering process in the atmospheric coordinate system (Zaxis along the atmospheric normal). The magnetic field makes an angle θ_{B} with respect to the polar Zaxis, and has an azimuth χ_{B}. (θ′,χ′) refer to the incident ray, and (θ,χ) to the scattered ray defined with respect to the polar Zaxis. Θ is the scattering angle. 

Open with DEXTER  
In the text 
Fig. 2
Azimuthal Fourier coefficients of typeII plotted as a function of the outgoing frequency x for different choices of μ and μ′. Left panels show and right panels show . The damping parameter a = 0.001. Thin lines correspond to x′ = 1 and thick lines to x′ = 4. Solid, dotted, dashed, dotdashed, and dashtripledotted lines correspond to k = 0,1,2,3, and 4, respectively. For notational brevity we simply dropped the M dependence on the ytitle of the plotted functions. 

Open with DEXTER  
In the text 
Fig. 3
Comparison of the multiple scattered solution from the SEM (solid lines) and of that from the perturbation method (dashed lines). Dotted lines represent the single scattered solution. The 1D cutoff approximation is used with x_{c} = 3. The model parameters are (a,ϵ,r) = (10^{3},10^{3},0) and the magnetic field parameters are (Γ,θ_{B},χ_{B}) = (1,30°,0°). The line of sight is represented by μ = 0.11 and χ = 0°. Panel a) corresponds to T = 1 and panel b) to T = 10^{4}. The positive Q direction corresponds to the linear polarization perpendicular to the solar limb. 

Open with DEXTER  
In the text 
Fig. 4
Same as Fig. 3, but with 2D frequency domains of Bommier (1997) in the Hanle PRD matrix. 

Open with DEXTER  
In the text 
Fig. 5
Comparison of the multiple scattered solution from the SEM (solid lines) and that from the perturbation method (dashed lines). Dotted lines represent the single scattered solution. Approximation I (nondomainbased PRD) is used for the SEM approach, while approximation II (2D angledependent frequency domains) is used in the perturbation method. Other model parameters are the same as in Fig. 3. 

Open with DEXTER  
In the text 
Fig. 6
The emergent I, Q/I, and U/I profiles at μ = 0.11 and χ = 0° computed for the angleaveraged (dashed lines) and the angledependent (solid lines) nondomainbased PRD. Panel a): thin lines T = 20, medium thick lines T = 200, and thick lines T = 2 × 10^{3}. Panel b): thin lines T = 2 × 10^{4}, medium thick lines T = 2 × 10^{6}, and thick lines T = 2 × 10^{8}. Other model parameters are (a,ϵ,r) = (10^{3},10^{4},0). The absolute differences Δ(Q/I) and Δ(U/I) in percentage are also shown. 

Open with DEXTER  
In the text 
Fig. 7
The emergent I, Q/I, and U/I profiles at μ = 0.11 and χ = 0° computed for the angleaveraged (dashed lines) and the angledependent (solid lines) nondomainbased PRD. Panel a): thin lines ϵ = 10^{2}, medium thick lines ϵ = 10^{6}, and thick lines ϵ = 0. Panel b): thin lines r = 10^{8}, medium thick lines r = 10^{6}, and thick lines r = 10^{4}. Other model parameters are (T,a) = (2 × 10^{3},10^{3}). For panel a) r = 0, and for panel b) ϵ = 10^{4}. The absolute differences Δ(Q/I) and Δ(U/I) in percentage are also shown. 

Open with DEXTER  
In the text 
Fig. 8
The emergent I, Q/I, and U/I profiles for different values of the heliocentric angle computed for the angleaveraged (dashed lines) and the angledependent (solid lines) nondomainbased PRD. The atmospheric model used is (T,a,ϵ,r) = (2 × 10^{3},10^{3},10^{4},0). The absolute differences Δ(Q/I) and Δ(U/I) in percentage are also shown. 

Open with DEXTER  
In the text 
Current usage metrics show cumulative count of Article Views (fulltext article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 4896 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.