All Figures

$\begin{figure} \par\includegraphics[width=9cm,height=14cm]{7398fig1.eps}\end{figure}$ Figure 1: RXTE PCA (2-60 keV) pulse profiles consecutive in time during outburst. Two cycles are plotted for clarity. The evolution of intensity of the first part of the outburst is plotted on the left column increasing from bottom to top. The fall is plotted on the right, with intensity decreasing from top to bottom.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,height=4.5cm]{7398fig2.eps}\end{figure}$ Figure 2: PCA (2-60 keV) pulse profiles at the same orbital phase ( $0.73\pm 0.02$ cycles) and at the same luminosity state ( $5.62\pm 0.04\times 10^{+36}$ erg s^-1).
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In the text

$\begin{figure} \par\includegraphics[width=18.8cm,height=3cm]{7398fig3.eps}\end{figure}$ Figure 3: RXTE PCA 2-60 keV pulse profiles at the same luminosity state ( $L \simeq 2\pm 0.6\times 10^{+36}$ erg s^-1; see Fig. 4 bottom).
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,height=7.5cm]{7398fig4.eps}\end{figure}$ Figure 4: Top. Sample of PCA observations selected for the pulse profile intensity analysis. An extra circle indicates the existence in addition of an INTEGRAL IBIS/ISGRI observation. Bottom. RXTE PCA flux in the 2-30 keV energy range. The horizontal dotted line denotes the luminosity level of ${\simeq }4\times 10 ^{+36}$ erg s^-1.
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In the text

$\begin{figure} \par\includegraphics[width=7.75cm,height=5.3cm]{7398fig5top.eps} ... ....eps}\includegraphics[width=7.75cm,height=5.3cm]{7398fig5bottom.eps}\end{figure}$ Figure 5: We have obtained 2-60 keV RXTE PCA pulse shapes varying from only single sinusoidal-like peak (phases 0.9-1), to profiles with two peaks (phases 0.7-0.9), and even occasionally with three (phases 0.5-0.7) and four peaks (0.2-0.5). From top to bottom, the four peaks strength is plotted vs. time, luminosity (2-60 keV rms flux) and orbital phase.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,height=7cm]{7398fig6.eps}\end{figure}$ Figure 6: From top to bottom, the ratio of the main to the second, the third and the fourth peak plotted vs. luminosity (2-60 keV rms flux). We have rejected few observations with large uncertainties for clarity.
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In the text

$\begin{figure} \par\includegraphics[width=18.5cm,height=8.2cm,clip]{7398fig7.eps} \end{figure}$ Figure 7: Evolution of SAX J2103.5+4545 PCA pulse profile with intensity in 4 energy bands ( from top to bottom). They are sorted consecutive in time during the brightest period (MJD 52 650-52 800) of the source.
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In the text

$\begin{figure} \par\includegraphics[width=8.9cm,height=8cm,clip]{7398fig8.eps} \end{figure}$ Figure 8: Some examples of SAX J2103.5+4545 PCA pulse profiles showing a more complex structure, in the same 4 energy bands.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,height=5.5cm,clip]{7398fig9.eps} \end{figure}$ Figure 9: ISGRI (20-60 keV) mean pulse profiles of SAX J2103.5+4545 generated by combining profiles from individual INTEGRAL ScWs.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,height=7.6cm,clip]{7398fig10.eps}\end{figure}$ Figure 10: Averaged peaks strength evolution with energy. The behaviour displayed here follows the one proposed from points 1 to 5 in the text.
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In the text

$\begin{figure} \par\includegraphics[width=8.7cm,height=11cm,clip]{7398fig11.eps} \end{figure}$ Figure 11: Top. Long-term hardness ratios history. From middle to bottom: HR-intensity diagram and spectral parameters evolution vs. intensity.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,height=6cm,clip]{7398fig12.eps}\end{figure}$ Figure 12: Top: long-term frequency history. Middle: averaged spin-up rates history. Bottom: 40-60 keV RXTE HEXTE averaged fluxes. A spin-up rate and X-ray flux correlation was found, confirming that an accretion disk during periastron passage is present.
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In the text

$\begin{figure} \par\includegraphics[width=6.3cm,height=6.3cm,clip]{7398fig13.eps} \end{figure}$ Figure 13: Spin-up rates vs. RXTE 2-100 keV non absorbed averaged flux every 1.5 and 2.5 orbits. A linear fit was found the best one.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,height=3cm]{7398fig14.eps} \end{figure}$ Figure 14: RXTE ASM orbital light curve of SAX J2103.5+4545 from MJD 52 200-52 500.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,height=14cm]{7398fig1.eps}\end{figure}$	Figure 1: RXTE PCA (2-60 keV) pulse profiles consecutive in time during outburst. Two cycles are plotted for clarity. The evolution of intensity of the first part of the outburst is plotted on the left column increasing from bottom to top. The fall is plotted on the right, with intensity decreasing from top to bottom.
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$\begin{figure} \par\includegraphics[width=9cm,height=4.5cm]{7398fig2.eps}\end{figure}$	Figure 2: PCA (2-60 keV) pulse profiles at the same orbital phase ( $0.73\pm 0.02$ cycles) and at the same luminosity state ( $5.62\pm 0.04\times 10^{+36}$ erg s^-1).
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$\begin{figure} \par\includegraphics[width=18.8cm,height=3cm]{7398fig3.eps}\end{figure}$	Figure 3: RXTE PCA 2-60 keV pulse profiles at the same luminosity state ( $L \simeq 2\pm 0.6\times 10^{+36}$ erg s^-1; see Fig. 4 bottom).
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$\begin{figure} \par\includegraphics[width=8.6cm,height=7.5cm]{7398fig4.eps}\end{figure}$	Figure 4: Top. Sample of PCA observations selected for the pulse profile intensity analysis. An extra circle indicates the existence in addition of an INTEGRAL IBIS/ISGRI observation. Bottom. RXTE PCA flux in the 2-30 keV energy range. The horizontal dotted line denotes the luminosity level of ${\simeq }4\times 10 ^{+36}$ erg s^-1.
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$\begin{figure} \par\includegraphics[width=7.75cm,height=5.3cm]{7398fig5top.eps} ... ....eps}\includegraphics[width=7.75cm,height=5.3cm]{7398fig5bottom.eps}\end{figure}$	Figure 5: We have obtained 2-60 keV RXTE PCA pulse shapes varying from only single sinusoidal-like peak (phases 0.9-1), to profiles with two peaks (phases 0.7-0.9), and even occasionally with three (phases 0.5-0.7) and four peaks (0.2-0.5). From top to bottom, the four peaks strength is plotted vs. time, luminosity (2-60 keV rms flux) and orbital phase.
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$\begin{figure} \par\includegraphics[width=8.5cm,height=7cm]{7398fig6.eps}\end{figure}$	Figure 6: From top to bottom, the ratio of the main to the second, the third and the fourth peak plotted vs. luminosity (2-60 keV rms flux). We have rejected few observations with large uncertainties for clarity.
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$\begin{figure} \par\includegraphics[width=18.5cm,height=8.2cm,clip]{7398fig7.eps} \end{figure}$	Figure 7: Evolution of SAX J2103.5+4545 PCA pulse profile with intensity in 4 energy bands ( from top to bottom). They are sorted consecutive in time during the brightest period (MJD 52 650-52 800) of the source.
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$\begin{figure} \par\includegraphics[width=8.9cm,height=8cm,clip]{7398fig8.eps} \end{figure}$	Figure 8: Some examples of SAX J2103.5+4545 PCA pulse profiles showing a more complex structure, in the same 4 energy bands.
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$\begin{figure} \par\includegraphics[width=8.6cm,height=5.5cm,clip]{7398fig9.eps} \end{figure}$	Figure 9: ISGRI (20-60 keV) mean pulse profiles of SAX J2103.5+4545 generated by combining profiles from individual INTEGRAL ScWs.
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$\begin{figure} \par\includegraphics[width=8cm,height=7.6cm,clip]{7398fig10.eps}\end{figure}$	Figure 10: Averaged peaks strength evolution with energy. The behaviour displayed here follows the one proposed from points 1 to 5 in the text.
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$\begin{figure} \par\includegraphics[width=8.7cm,height=11cm,clip]{7398fig11.eps} \end{figure}$	Figure 11: Top. Long-term hardness ratios history. From middle to bottom: HR-intensity diagram and spectral parameters evolution vs. intensity.
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$\begin{figure} \par\includegraphics[width=8cm,height=6cm,clip]{7398fig12.eps}\end{figure}$	Figure 12: Top: long-term frequency history. Middle: averaged spin-up rates history. Bottom: 40-60 keV RXTE HEXTE averaged fluxes. A spin-up rate and X-ray flux correlation was found, confirming that an accretion disk during periastron passage is present.
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$\begin{figure} \par\includegraphics[width=6.3cm,height=6.3cm,clip]{7398fig13.eps} \end{figure}$	Figure 13: Spin-up rates vs. RXTE 2-100 keV non absorbed averaged flux every 1.5 and 2.5 orbits. A linear fit was found the best one.
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$\begin{figure} \par\includegraphics[width=8.4cm,height=3cm]{7398fig14.eps} \end{figure}$	Figure 14: RXTE ASM orbital light curve of SAX J2103.5+4545 from MJD 52 200-52 500.
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