Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{2720fig1.ps}\hspace*{3mm} \includegraphics[width=7.4cm,clip]{2720fig2.ps} \end{figure}$ Figure 1: RF of Stokes I to $v_{\rm LOS}$ multiplied by $\Delta \tau _{\rm c}$ [10^-2 (km s ^-1)^-1] for Fe I 630.25 nm ( left) and Fe I 1564.85 nm ( right) in the HSRA quiet Sun model. The gray scale is the same in the two panels to facilitate comparisons.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{2720fig3.ps} \end{figure}$ Figure 2: Maximum value of the integrated RF to $v_{\rm LOS}$ for the lines of Table 1, as a function of the shape ratio multiplied by the central wavelength of the transition. Quiet Sun (crosses), penumbral (circles) and hot umbral (filled circles) atmospheres have been used. The most sensitive lines, Fe I 630.25 nm, and Fe I 1564.85 nm are marked with labels in the quiet Sun (dotted lines), penumbral (dashed lines), and umbral (dotted-dashed lines) models.
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In the text

$\begin{figure} \par\includegraphics[width=7.1cm,clip]{2720fig4.ps}\hspace*{4mm} \includegraphics[width=7.1cm,clip]{2720fig5.ps} \end{figure}$ Figure 3: Normalized RF of Stokes V to B multiplied by $\Delta \tau _{\rm c}$ [10^-5 G^-1] for Fe I 630.25 nm ( left) and Fe I 1564.85 nm ( right) in the HSRA model with a longitudinal magnetic field of B=2000 G. The same gray scale is used in the two panels.
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In the text

$\begin{figure} \par\includegraphics[width=7.1cm,clip]{2720fig6.ps} \end{figure}$ Figure 4: Maximum values of the integrated RF to B for the set of lines in Table 1 with $g_{\rm eff} \ne 0$ vs $(A^V_0/A^V_{1}) ~ g_{\rm eff} \lambda_0^{2}$ (strong field regime). The sensitivities have been evaluated in the quiet sun (crosses), penumbral (circles), and umbral (filled circles) models. Dotted, dashed, and dash-dotted lines mark the most sensitive lines, Fe I 630.25 nm, and Fe I 1564.85 nm in the quiet sun, penumbral, and umbral atmospheres, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=7.1cm,clip]{2720fig7.ps}\includegraphics[width=7.1cm,clip]{2720fig8.ps} \end{figure}$ Figure 5: Normalized RF of Stokes V to B multiplied by $\Delta \tau _{\rm c}$ [10^-5 G^-1] for Fe I 630.25 nm ( left) and Fe I 1564.85 nm ( right) in the HSRA model with a longitudinal magnetic field of B=200 G. This corresponds to the weak field regime.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{2720fig9.ps} \end{figure}$ Figure 6: Maximum values of the integrated RF to B for the lines of Table 1 with $g_{\rm eff} \ne 0$ vs the parameter $(A^{*}_{0}/A^{*}_{1}) \cos ~ \gamma g_{\rm eff} \lambda_0^{2}$ (weak field regime). The sensitivities have been evaluated in the quiet sun (crosses), penumbral (circles), and hot umbral (filled circles) models with a longitudinal magnetic field of 200 G. Dotted, dashed, and dash-dotted lines mark specific transitions in the quiet sun, penumbral, and umbral models, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{2720fig10.ps}\hspace*{2mm} \includegraphics[width=8cm,clip]{2720fig11.ps} \end{figure}$ Figure 7: Top: normalized RF of Stokes I to T multiplied by $\Delta \tau _{\rm c}$ [10^-5 K^-1] for Fe I 630.25 nm ( left) and Fe I 1564.85 nm ( right) in the HSRA quiet sun model. Bottom: the two subpanels below each line display the first ( left) and second ( right) signed terms on the rhs of Eq. (2) contributing to the RF. That is, the first and third subpanels show how Stokes I varies due to changes in the source function, while the second and fourth subpanels display how Stokes I reacts to the opacity variations induced by temperature changes. Note that the gray scale is inverted in this figure, with black representing positive values and white negative values.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{2720fig12.ps} \end{figure}$ Figure 8: Maximum value of the integrated RF of Stokes I to T for the lines of Table 1 vs. the wavelength of each transition. The sensitivities have been evaluated in the quiet Sun (crosses), penumbral (circles), and umbral (filled circles) models. Solid, dashed, and dotted curves represent the partial derivatives of the continuum intensity with respect to temperature ( $\partial A_{2}/\partial T$ ) in the quiet Sun, penumbral, and umbral models.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{2720fig13.ps} \end{figure}$ Figure 9: Maximum value of the integrated RF of Stokes I to T for the lines of Table 1 vs. the parameter $P_{\rm T}$ (see text for details). Quiet Sun (crosses), penumbral (circles), and umbral (filled circles) atmospheres have been used. The most sensitive lines, Fe I 630.25 nm, and Fe I 1564.85 nm in these models are marked with dotted, dashed, and dot-dashed lines, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{2720fig14.ps} \end{figure}$ Figure 10: Response function of the equivalent width to temperature perturbations for Fe I 630.25 (solid line), Fe I 1564.85 nm (dotted line), and Fe II 614.93 nm (dash-dotted line) in the quiet Sun model.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{2720fig15.ps} \end{figure}$ Figure 11: Integrated RF of equivalent width to temperature perturbations vs. $P_{\rm W}$ for HSRA (crosses), penumbral (circles) and umbral (filled circles) model atmospheres.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{2720fig1.ps}\hspace*{3mm} \includegraphics[width=7.4cm,clip]{2720fig2.ps} \end{figure}$	Figure 1: RF of Stokes I to $v_{\rm LOS}$ multiplied by $\Delta \tau _{\rm c}$ [10^-2 (km s ^-1)^-1] for Fe I 630.25 nm ( left) and Fe I 1564.85 nm ( right) in the HSRA quiet Sun model. The gray scale is the same in the two panels to facilitate comparisons.
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$\begin{figure} \par\includegraphics[width=7.1cm,clip]{2720fig4.ps}\hspace*{4mm} \includegraphics[width=7.1cm,clip]{2720fig5.ps} \end{figure}$	Figure 3: Normalized RF of Stokes V to B multiplied by $\Delta \tau _{\rm c}$ [10^-5 G^-1] for Fe I 630.25 nm ( left) and Fe I 1564.85 nm ( right) in the HSRA model with a longitudinal magnetic field of B=2000 G. The same gray scale is used in the two panels.
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$\begin{figure} \par\includegraphics[width=7.1cm,clip]{2720fig7.ps}\includegraphics[width=7.1cm,clip]{2720fig8.ps} \end{figure}$	Figure 5: Normalized RF of Stokes V to B multiplied by $\Delta \tau _{\rm c}$ [10^-5 G^-1] for Fe I 630.25 nm ( left) and Fe I 1564.85 nm ( right) in the HSRA model with a longitudinal magnetic field of B=200 G. This corresponds to the weak field regime.
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$\begin{figure} \par\includegraphics[width=7.2cm,clip]{2720fig13.ps} \end{figure}$	Figure 9: Maximum value of the integrated RF of Stokes I to T for the lines of Table 1 vs. the parameter $P_{\rm T}$ (see text for details). Quiet Sun (crosses), penumbral (circles), and umbral (filled circles) atmospheres have been used. The most sensitive lines, Fe I 630.25 nm, and Fe I 1564.85 nm in these models are marked with dotted, dashed, and dot-dashed lines, respectively.
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$\begin{figure} \par\includegraphics[width=7.4cm,clip]{2720fig14.ps} \end{figure}$	Figure 10: Response function of the equivalent width to temperature perturbations for Fe I 630.25 (solid line), Fe I 1564.85 nm (dotted line), and Fe II 614.93 nm (dash-dotted line) in the quiet Sun model.
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$\begin{figure} \par\includegraphics[width=7.4cm,clip]{2720fig15.ps} \end{figure}$	Figure 11: Integrated RF of equivalent width to temperature perturbations vs. $P_{\rm W}$ for HSRA (crosses), penumbral (circles) and umbral (filled circles) model atmospheres.
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