All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{rrly-landcompare.eps} \end{figure}$ Figure 1: Distribution of Landé factors of all lines used to construct the LSD profile of RR Lyrae (top) and $\alpha ^2$ CVn (bottom).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{cvnnew.eps} \end{figure}$ Figure 2: Longitudinal magnetic field variation of the prototypical magnetic Ap star $\alpha ^2$ CVn. The open and solid circles show respectively the observations reported by Wade et al. (2000b) and the longitudinal magnetic field measurements obtained within the context of this programme. The solid curve is a least-squares fit.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{pulyr.eps} \end{figure}$ Figure 3: Comparison of our longitudinal magnetic field measurements (solid circles) of RR Lyrae as a function of pulsation phase with the magnetic field variation reported by Romanov et al. 1987 in 25-28 September 1982 (open circles).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{blalyr.eps} \end{figure}$ Figure 4: Comparison of our longitudinal magnetic field measurements (solid circles) of RR Lyrae as a function of Blazhko phase with the mean magnetic field variation reported by Romanov et al. (1994) (open circles).
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In the text

$\begin{figure} \par\includegraphics[width=15.1cm,clip]{lsd.eps}\end{figure}$ Figure 5: a) and b) show respectively the representative LSD unpolarized Stokes I (lower curves) and circularly polarized Stokes V (upper curves) profiles of RR Lyrae. a) LSD V and I profiles obtained on 31 July 2002 corresponding to maximum pulsation phase ( $\phi \sim 0.00$ ) and maximum Blazhko phase ( $\psi \sim 0.00$ ), the heliocentric radial velocity value is -99.24 km s^-1 and the line broadening phenomenon associated with the shock wave passage is clearly visible (Chadid & Gillet 1996b). b) LSD V and I profiles obtained on 9 July 2000 corresponding to minimum pulsation phase ( $\phi \sim 0.50$ ) and minimum Blazhko phase ( $\psi \sim 0.50$ ), the heliocentric radial velocity value is -55.40 km s^-1. Significant Zeeman signature is not detected in either a) or b).
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In the text

$\begin{figure} \par\includegraphics[width=12.4cm,clip]{cyclebis.eps} \end{figure}$ Figure 6: Longitudinal magnetic field measurements of RR Lyrae from 1999 through 2002. No clear magnetic field variability is visible with the period of about 4 years.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{rrly-landcompare.eps} \end{figure}$	Figure 1: Distribution of Landé factors of all lines used to construct the LSD profile of RR Lyrae (top) and $\alpha ^2$ CVn (bottom).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{cvnnew.eps} \end{figure}$	Figure 2: Longitudinal magnetic field variation of the prototypical magnetic Ap star $\alpha ^2$ CVn. The open and solid circles show respectively the observations reported by Wade et al. (2000b) and the longitudinal magnetic field measurements obtained within the context of this programme. The solid curve is a least-squares fit.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{pulyr.eps} \end{figure}$	Figure 3: Comparison of our longitudinal magnetic field measurements (solid circles) of RR Lyrae as a function of pulsation phase with the magnetic field variation reported by Romanov et al. 1987 in 25-28 September 1982 (open circles).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{blalyr.eps} \end{figure}$	Figure 4: Comparison of our longitudinal magnetic field measurements (solid circles) of RR Lyrae as a function of Blazhko phase with the mean magnetic field variation reported by Romanov et al. (1994) (open circles).
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$\begin{figure} \par\includegraphics[width=12.4cm,clip]{cyclebis.eps} \end{figure}$	Figure 6: Longitudinal magnetic field measurements of RR Lyrae from 1999 through 2002. No clear magnetic field variability is visible with the period of about 4 years.
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