All Figures

$\begin{figure} \par\includegraphics[width=10.5cm,clip]{0547fig1.ps} \end{figure}$ Figure 1: The pulsational radial velocity curves of HR 1217. The solid lines are the nightly synthetic multifrequency fits.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=16.2cm,clip]{0547fig2.ps} \end{figure}$ Figure 2: The discrete Fourier transform (central wavelength shown at the top) as a function of rotation phase ( top to bottom, rotation phase values shown at the far right) for the first 7 spectral orders (wavelength interval 5590-6300 Å). Each spectral order spans approximately 100 Å. The dashed lines show the location of the published photometric frequencies from Kurtz et al. (1989).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=16.4cm,clip]{0547fig3.ps} \end{figure}$ Figure 3: The same as in Fig. 2, but for the wavelength interval 5013-5590 Å (7 spectral orders).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.9cm]{0547fig4.ps} \end{figure}$ Figure 4: The rotational modulation of the amplitude of the $f_{\rm 2}=229.21$ c d^-1 (2653 $\mu$ Hz) mode for each of the spectral regions (orders).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.9cm]{0547fig5.ps} \end{figure}$ Figure 5: The rotational modulation of the phase of the $f_{\rm 2}=229.21$ c d^-1 (2653 $\mu$ Hz) mode for each of the spectral regions (orders). Symbols are the same as for Fig. 4. The pulsation phase is given in fractions of a pulsation cycle.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{0547fig6.ps} \end{figure}$ Figure 6: The amplitude spectra of consecutive steps of a DFT analysis for the entire RV data. The position of principal frequencies from Kurtz et al. (1989) are indicated by dashed lines. (Top) DFT of original RV data. (Middle) DFT of RV residuals after removing contribution from $f_{\rm 2}$ . (Bottom) DFT of residuals after removing the principal frequencies $f_{\rm 1}$ , $f_{\rm 2}$ , $f_{\rm 4}$ , $f_{\rm 3}$ and the rotationally split sidelobes $f_{\rm 2}^{+}$ , $f_{\rm 4}^{-}$ , $f_{\rm 2}$ , and $f_{\rm 2}^{-}$ . The $f_{\rm 6}$ mode (Kurtz et al. 2002) as well as a suspected new mode with amplitude of 14.3 m s^-1 and frequency of $219.9 \pm 1$ c d^-1 (2545.1 $\mu$ Hz) are shown by arrows in the bottom panel.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0547fig7.ps} \end{figure}$ Figure 7: The amplitude DFT spectra of merged nightly residuals after removing the contribution of $f_{\rm 2}$ , $f_{\rm 3}$ , and $f_{\rm 4}$ determined by least squares solutions for every night. The position of the principal frequencies from Kurtz et al. (1989) are indicated by dashed lines. The right arrow ( $f_{\rm 6}$ ) marks the location of the most recent photometric mode (Kurtz et al. 2002) and the $f_{\rm 7}$ mode is the dashed line to its immediate right. The new suspected mode is shown by the arrow to the left.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=11.5cm,clip]{0547fig8.ps} \end{figure}$ Figure 8: DFT of the "broad-band'' RVs of the order centered on 5825 Å from the individual nights ( left panels, from top to bottom) and after subtracting a two-frequency solution ( right panels, from top to bottom). Note the different RV scale for the upper four panels. The vertical dashed lines shows the position of the photometric frequencies from Kurtz et al. (2002). The Julian dates and the corresponding mean rotation phases are given for each panel.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0547fig9.ps} \end{figure}$ Figure 9: The phase curve of residuals after removal of a three frequency fit ( $f_{\rm 2}$ , $f_{\rm 4}$ and $f_{\rm 5}$ ) to data from the night JD 2 450 804. This is phased to the best fit frequency fit of 241.7 c d^-1 (exactly between $f_{\rm 6}$ and $f_{\rm 7}$ ). The semi-amplitude of remaining two mode pulsations is 56.2 m s^-1. Data points are repeated for the second cycle.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=12.2cm,clip]{0547fig10.ps} \end{figure}$ Figure 10: Pulsation amplitude and phase for the $f_{\rm 2}$ , $f_{\rm 3}$ and $f_{\rm 4}$ modes as a function of rotation phase. Note the different amplitude scales for different modes. Data points are repeated for the second cycle.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{0547fig11.ps} \end{figure}$ Figure 11: The pulsation RV variations of the Nd III 5294.1 Å spectral line obtained on JD 2 450 804.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0547fig12.ps} \end{figure}$ Figure 12: The frequency analysis of the RV measurements of the Nd III 5294.1 Å line obtained on JD 2 450 845. ( Top panel) The DFT of original RV data. ( Bottom panel) The DFT of the residual RV data after subtracting the contribution due to $f_{\rm 2}$ ( $K_{\rm 2}$ = 163.25 m s^-1), $f_{\rm 4}$ ( $K_{\rm 4}$ = 112.81 m s^-1), and $f_{\rm 7}$ ( $K_{\rm 7}$ = 64.04 m s^-1). The long vertical dashed lines show the position of all seven known photometric frequencies in the range of 226-242 c d^-1. The two short vertical lines show the expected equally spaced position of new p-modes at frequencies 223.3 c d^-1 and 220.4 c d^-1. Note the strong blended peak (K = 76 m s^-1) located approximately between these new frequencies.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0547fig13.ps} \end{figure}$ Figure 13: The phase curve of JD 2 450 845 RV residuals after removing the contribution due to $f_{\rm 2}$ , $f_{\rm 3}$ , $f_{\rm 4}$ , $f_{\rm 5}$ , and $f_{\rm 7}$ . The residual RV measurements are phased with a new, best fit frequency of 222.33 c d^-1 (K=66.3 m s^-1) which is located between frequencies $f_{\rm -1}$ and $f_{\rm0}$ and is likely the blend of these two modes. Phases are reckoned from the time of RV maximum. The data are binned into intervals 0.05 of pulsation period and are repeated for the second cycle.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0547fig14.ps} \end{figure}$ Figure 14: The amplitude spectra for two merged residual RV data of the Nd III 5294.1 Å line from the nights JD 2 450 843 and 2 450 845. This residual data results from two consecutive steps of pre-whitening the data by the contribution of $f_{\rm 2}$ and $f_{\rm 4}$ . The long vertical dashed lines show the positions of the seven known photometric frequencies. The two short dashed vertical lines at 223.3 c d^-1 (marked as $f_{\rm0}$ ) and 220.4 c d^-1 (marked as $f_{\rm -1}$ ) show the expected positions of the two modes extrapolated from the equidistant spacing of the $f_{\rm 1}$ - $f_{\rm 6}$ series. The well resolved peaks at frequencies of $220.58\pm 0.03$ c d^-1 ( K_-1 = 59.9 m s^-1) and $223.37 \pm 0.03$ c d^-1 ( K₀ = 50.3 m s^-1) correspond to new detected modes.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0547fig15.ps} \end{figure}$ Figure 15: DFT analysis of combined data for Nd III 5294.1 Å spanning JD 2 450 800-2 450 801. ( Top) DFT of the original data. ( Middle) DFT of the residuals after pre-whitening by the f₂ mode. ( Bottom) DFT of the RV residuals after prewhitening by the $f_{\rm 2}$ and $f_{\rm 4}$ ( $K_{\rm 4}=80.0$ m s^-1) modes. The remaining peaks correspond to $f_{\rm 1}$ ( $K_{\rm 1}= 30.0$ m s^-1), $f_{\rm 3}$ ( $K_{\rm 3}= 40.3$ m s^-1), and $f_{\rm 6}$ ( $K_{\rm 6}= 30.0$ m s^-1). The short vertical lines show the expected positions (at 223.3 c d^-1 and 220.4 c d^-1) of two modes extrapolated from the f₁- $f_{\rm 6}$ equidistant mode spacing. Note the missing signal of the $f_{\rm0}$ mode that is a indication of rotational modulation of this mode.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0547fig16.ps} \end{figure}$ Figure 16: The calculated rotational modulation of the relative RV amplitudes (modulus of the spatial response function) of pure l=1, 2 and 3 zonal (m=0) modes in a standard OPM for HR 1217. The pulsation phase is positive around the magnetic maximum ( $\phi =1.0$ ) and switches sign after every pass of the response function through zero. The l = 1, m = 0 mode does not change its pulsation phase over the rotation period reflecting the non-reversive variations of magnetic field in HR 1217.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=14.4cm,clip]{0547fig17.ps} \end{figure}$ Figure 17: Left panel: p-mode echelle-spectrum of HR 1217. The $f_{\rm -1}, f_{\rm 1}, f_{\rm 3}$ , $f_{\rm 5}$ and $f_{\rm0}, f_{\rm 2}, f_{\rm 4}, f_{\rm 6}$ modes which are likely related respectively to odd and even l-degrees are spaced on $\approx$ 34 $\mu$ Hz. The $f_{\rm 7}$ mode is shown by open circle. Right panel: the theoretical l=1-4 p-mode echelle-spectrum model "L'' from Gautschy et al. (1998). The modes with n=33 to n=37 and different l-degrees form vertical columns (different symbols). The column representing the l=4 modes between the l=1, 3 and l=2 columns is similar to spacing that is observed for $f_{\rm 7}$ mode in HR 1217.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=10.5cm,clip]{0547fig1.ps} \end{figure}$	Figure 1: The pulsational radial velocity curves of HR 1217. The solid lines are the nightly synthetic multifrequency fits.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=16.2cm,clip]{0547fig2.ps} \end{figure}$	Figure 2: The discrete Fourier transform (central wavelength shown at the top) as a function of rotation phase ( top to bottom, rotation phase values shown at the far right) for the first 7 spectral orders (wavelength interval 5590-6300 Å). Each spectral order spans approximately 100 Å. The dashed lines show the location of the published photometric frequencies from Kurtz et al. (1989).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=16.4cm,clip]{0547fig3.ps} \end{figure}$	Figure 3: The same as in Fig. 2, but for the wavelength interval 5013-5590 Å (7 spectral orders).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.9cm]{0547fig4.ps} \end{figure}$	Figure 4: The rotational modulation of the amplitude of the $f_{\rm 2}=229.21$ c d^-1 (2653 $\mu$ Hz) mode for each of the spectral regions (orders).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.9cm]{0547fig5.ps} \end{figure}$	Figure 5: The rotational modulation of the phase of the $f_{\rm 2}=229.21$ c d^-1 (2653 $\mu$ Hz) mode for each of the spectral regions (orders). Symbols are the same as for Fig. 4. The pulsation phase is given in fractions of a pulsation cycle.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0547fig9.ps} \end{figure}$	Figure 9: The phase curve of residuals after removal of a three frequency fit ( $f_{\rm 2}$ , $f_{\rm 4}$ and $f_{\rm 5}$ ) to data from the night JD 2 450 804. This is phased to the best fit frequency fit of 241.7 c d^-1 (exactly between $f_{\rm 6}$ and $f_{\rm 7}$ ). The semi-amplitude of remaining two mode pulsations is 56.2 m s^-1. Data points are repeated for the second cycle.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=12.2cm,clip]{0547fig10.ps} \end{figure}$	Figure 10: Pulsation amplitude and phase for the $f_{\rm 2}$ , $f_{\rm 3}$ and $f_{\rm 4}$ modes as a function of rotation phase. Note the different amplitude scales for different modes. Data points are repeated for the second cycle.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=17cm,clip]{0547fig11.ps} \end{figure}$	Figure 11: The pulsation RV variations of the Nd III 5294.1 Å spectral line obtained on JD 2 450 804.
Open with DEXTER