Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=4.3cm,clip]{Gf231_f1a.eps}\includegrap... ...lip]{Gf231_f1c.eps}\includegraphics[width=4.3cm,clip]{Gf231_f1d.eps}\end{figure}$ Figure 1: a) H $\alpha$ solar image taken at 7:04 UT on 6 September 1999 (©Observatoire de Paris - BASS2000). b) EIT 195 Å full-disk solar image taken at 6:36 UT on the same day. c) The corresponding heliographic projection of the solar disk; the overlaid square (S5-N85, L=60-150) shows a pair of dark long filaments. d) The corresponding snapshot; a rectangular ROI (centred at N37, L=115) is overlaid in dark.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{Gf231_f2.eps}\end{figure}$ Figure 2: a) Averaged intensity I in the ROI southern end (thick line) and 14-h-boxcar running average I₀ (thin line). b) Intensity time series I/I₀-1. c) Corresponding Morlet wavelet power spectrum: increasing grey level is used to represent increasing power; significant power is within the 95% confidence level contour (including red noise) and outside the hatched cones of influence.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{Gf231_f3.eps}\end{figure}$ Figure 3: Lomb-Scargle periodogram (thin solid), normalised Fourier power spectrum (histogram mode) and normalised global wavelet spectrum (thick solid). The horizontal dashed line is the 95% confidence level for the periodogram.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{Gf231_f4.eps}\end{figure}$ Figure 4: a) Time-space plot of relative intensity along the ROI long axis. b) Distribution of scale-averaged wavelet transforms over the waveband $12.8 \pm 2$ h along the ROI long axis. Significant power is within the 95% level contour (including red noise) and outside the hatched cones of influence.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{Gf231_f5.eps}\end{figure}$ Figure 5: a) Distribution of the relative Lomb-Scargle periodogram along the ROI long axis. Increasing grey level is used to represent increasing relative power; significant power is within the 95% level contour. b) Average of the relative spectral powers over distance; the ratio level of 1 is shown as a horizontal dashed line.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{Gf231_f2.eps}\end{figure}$	Figure 2: a) Averaged intensity I in the ROI southern end (thick line) and 14-h-boxcar running average I₀ (thin line). b) Intensity time series I/I₀-1. c) Corresponding Morlet wavelet power spectrum: increasing grey level is used to represent increasing power; significant power is within the 95% confidence level contour (including red noise) and outside the hatched cones of influence.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{Gf231_f3.eps}\end{figure}$	Figure 3: Lomb-Scargle periodogram (thin solid), normalised Fourier power spectrum (histogram mode) and normalised global wavelet spectrum (thick solid). The horizontal dashed line is the 95% confidence level for the periodogram.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{Gf231_f4.eps}\end{figure}$	Figure 4: a) Time-space plot of relative intensity along the ROI long axis. b) Distribution of scale-averaged wavelet transforms over the waveband $12.8 \pm 2$ h along the ROI long axis. Significant power is within the 95% level contour (including red noise) and outside the hatched cones of influence.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{Gf231_f5.eps}\end{figure}$	Figure 5: a) Distribution of the relative Lomb-Scargle periodogram along the ROI long axis. Increasing grey level is used to represent increasing relative power; significant power is within the 95% level contour. b) Average of the relative spectral powers over distance; the ratio level of 1 is shown as a horizontal dashed line.
Open with DEXTER