All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{6030fig1.eps} \end{figure}$ Figure 1: The Paschen-Back effect in the doublet level with N=5 for the $B^2 \Sigma$ v = 0 state of CN.
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In the text

$\begin{figure} \par\includegraphics[width=14.7cm,clip]{6030fig2.eps} \end{figure}$ Figure 2: Dependence of the H $\ddot{ \rm o}$ nl-London factors on magnetic field strength for the CN violet system. Upper panels: calculations for transitions corresponding to the different rotational branches, which are strictly defined only for weak magnetic fields. Lower panels: the grouping is done for transitions between states with fixed spin projection on the magnetic field direction, a definition which is representative of the physics in the complete PBR.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{6030fig3.eps} \end{figure}$ Figure 3: Scattering profiles for a whole doublet, in the (0, 0) band of the CN violet system. Solid and dashed curves represent the PBR and ZR cases respectively. Left panels: P(2), $N = 2 \! \to \! 1 \! \to \! 2$ , for 200 G field. Right panels: P(3), $N = 3 \to \! 2 \! \to \! 3$ , for 0, 1 and 200 G fields. Note that the PBE and ZE curves for 0 G and 1 G superimpose, so they are undistinguishable, while the curves for 200 G can be easily seen separately. The magnetic field is perpendicular to the line of sight and is in the plane of the solar surface. The Doppler width $\Delta \lambda _{\rm D}=25$ mÅ, the Voigt parameter a=0.0001. Unpolarized incident radiation field and single scattering at angle $90^{\circ }$ are assumed. Collisional depolarization and continuum opacity are neglected.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{6030fig4.eps} \end{figure}$ Figure 4: Same as Fig. 3 but for a magnetic field direction perpendicular to the solar surface and the line of sight. There is no Hanle effect in the usual sense in this case. In both panels only the curves for 200 G are shown.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{6030fig5.eps} \end{figure}$ Figure 5: Scattering profiles for the R(1), $N = 1 \! \to \! 2 \! \to \! 1$ transition. Left panels: Realistic Doppler width $\Delta \lambda _{\rm D}=25$ mÅ and a=0.0001, curves for 0, 1, 200 G fields. Note that like in Fig. 3 the PBE and ZE curves for 0 G and 1 G superimpose, while the curves for 200 G might be seen separately (but the difference between them is much smaller than in Fig. 3). Right panels: very small Doppler width $\Delta \lambda _{\rm D}=2.5$ mÅ and a=0.001, curves only for a field of 200 G. In the top and right panel the different components of the doublet are marked: "1'' for ^R S₁₂ (0.5), "2'' for R₁ (1.5), "3'' for R₂ (0.5), "4'' for ^R Q₂₁ (1.5).
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{6030fig6.eps} \end{figure}$ Figure 6: Scattering profiles for transitions in the (0, 7) band of the MgH $B'~ {}^{2} \Sigma - X ~ {}^{2} \Sigma$ system, assuming a horizontal field. Left panel: R(10), $N = 10 \! \to \! 11 \! \to \! 10$ transition. Right panel: R(25), $N = 25 \! \to \! 26 \! \to \! 25$ transition. Solid and dashed lines represent the PBR and ZR calculations, respectively. Doppler width $\Delta \lambda _{\rm D}=25$ mÅ field strength 200 G, and spin-rotational constant $\gamma_{\rm SR}=10^{-4} ~ {\rm cm}^{-1}$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{6030fig7.eps} \end{figure}$ Figure 7: The dependence of saturated depolarization on magnetic field strength. The N numbers of the transitions are indicated in the plot. The magnetic field is perpendicular to the solar surface. The solid curves represent the PBR case, the dashed lines the ZR case.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{6030fig8.eps} \end{figure}$ Figure 8: The same as Fig. 7, but for a magnetic field vector perpendicular to the line of sight and in the plane of the solar surface.
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In the text

$\begin{figure} \par\includegraphics[width=15.5cm,clip]{6030fig9.eps} \end{figure}$ Figure 9: Dependence of saturated depolarization on field direction. Left panel: dependence on declination (angle with the plane which is perpendicular to the solar surface), when the azimuth (angle with the plane that is perpendicular to the direction on the observer and contains the normal to the solar surface) equals zero. Right panel: dependence on azimuth (when the declination equals zero). Curves for a P(2), $N = 2 \! \to \! 1 \! \to \! 2$ transition in a 200 G field and for a R(1), $N = 1 \! \to \! 2 \! \to \! 1$ in a 400 G field. We have changed the sign of the depolarization for the $1 \! \to \! 2 \! \to \! 1$ curves to make plots more clear. The solid curves represent the PBR case, the dashed curves the ZR case.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{6030fig10.eps} \end{figure}$ Figure 10: Dependence of depolarization on the magnetic field strength for the (0, 7) band of the MgH $B'~ {}^{2} \Sigma - X ~ {}^{2} \Sigma$ system for different values of the spin-rotational constant $\gamma _{\rm SR}$ , for the transitions R(1), $N = 1 \! \to \! 2 \! \to \! 1$ . Continuous lines represent $\gamma_{\rm SR}=10^{-4} ~ {\rm cm}^{-1}$ , dashed lines $\gamma_{\rm SR}=5 \times 10^{-4}~{\rm cm}^{-1}$ , dashed-dotted lines for $\gamma_{\rm SR}=10^{-3}~{\rm cm}^{-1}$ . Thick curves represent the PBR case, thin the ZR case.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{6030fig1.eps} \end{figure}$	Figure 1: The Paschen-Back effect in the doublet level with N=5 for the $B^2 \Sigma$ v = 0 state of CN.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{6030fig4.eps} \end{figure}$	Figure 4: Same as Fig. 3 but for a magnetic field direction perpendicular to the solar surface and the line of sight. There is no Hanle effect in the usual sense in this case. In both panels only the curves for 200 G are shown.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{6030fig7.eps} \end{figure}$	Figure 7: The dependence of saturated depolarization on magnetic field strength. The N numbers of the transitions are indicated in the plot. The magnetic field is perpendicular to the solar surface. The solid curves represent the PBR case, the dashed lines the ZR case.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{6030fig8.eps} \end{figure}$	Figure 8: The same as Fig. 7, but for a magnetic field vector perpendicular to the line of sight and in the plane of the solar surface.
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