All Figures

$\begin{figure} \par\includegraphics[width=9cm,clip]{7958f1} \end{figure}$ Figure 1: ( $\alpha$ , $\lambda$ ) parameter space for the simulations carried out. Each simulation is represented by a circlet, and corresponds to a pair of values of the viscosity parameter and angular momentum ( $\alpha$ , $\lambda$ ). Empty circlets refer to the four boundary disc models showing single shocks and pulsed outflows. The boundary line is the limit for ( $\alpha$ , $\lambda$ ) pairs to produce an oscillating shock and an outflow. Inside the shaded domain both outflows and shocks are periodical. Outflows are supported by higher $\alpha$ viscosity parameters when adopting lower initial $\lambda$ at the disc outer edge as a boundary condition.
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In the text

$\begin{figure} \par\includegraphics[width=11.4cm,clip]{aa7958f2a.eps} \end{figure}$ Figure 2: Plots of the outflow rate d $n_{\rm jet}/{\rm d}t$ , the accretion rate d $n_{\rm acc}/{\rm d}t$ , and the number of particles in the disc $N_{\rm disk}$ versus time. Quantities in the plots are expressed in simulation units. At the top of each panel, the adopted ( $\lambda$ , $\alpha$ ) parameters and the model ID are also reported.
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In the text

$\begin{figure} \par\includegraphics[width=11.4cm,clip]{aa7958f2b.eps} \end{figure}$ Figure 2: continued.
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In the text

$\begin{figure} \par\includegraphics[width=11.5cm,clip]{aa7958f2c.eps} \end{figure}$ Figure 2: continued.
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In the text

$\begin{figure} \par\includegraphics[width=4.1cm,clip]{7958f2j.eps}\includegraphics[width=4.1cm,clip]{7958f2k.eps} \end{figure}$ Figure 2: continued.
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In the text

$\begin{figure} \par\includegraphics[width=12cm, height=16cm]{7958f3} \end{figure}$ Figure 3: Twelve XY-plots concerning different phases $\phi$ of the periodical accretion disc time evolution with $\alpha = 2 \times 10^{-3}$ , and initial outer edge boundary conditions v_X = 0.1 and $\lambda = 1.6$ . In such plots, density isocontours are shown. Distances are expressed in units of the Schwartzschild radius. For $\phi$ in the range $0 \div 016$ , the RH conditions are satisfied. Instead, for $\phi$ in the range $\sim$ $0.16 \div 0.90$ , the RH conditions are not satisfied and the shock front decays and then forms again. From $\phi \sim 0.90$ and afterward, the RH conditions are satisfied again and the shock front remains at $X \simeq 10$ .
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In the text

$\begin{figure} \par\includegraphics[height=8.cm, width=8cm]{7958f4} \end{figure}$ Figure 4: Fourier spectrum of the flux time variation of 0440-003 (solid line) with superimposed Fourier spectrum of model L (dashed line). L is the model whose simulated Fourier spectrum better fits the source power spectrum. Frequencies are expressed in Hz and power is normalized to its maximum.
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In the text

$\begin{figure} \par\includegraphics[height=8 cm, width=8.5 cm,clip]{7958f5} \end{figure}$ Figure 5: Fourier spectrum of the flux time variation of 1730-130 (solid line) with superimposed Fourier spectrum of model A (dashed line). Scales are as in Fig. 4.
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In the text

$\begin{figure} \par\includegraphics[height=8.5 cm, width=8.5 cm,clip]{7958f6} \end{figure}$ Figure 6: Fourier spectrum of the flux time variation of 1101+384 (solid line) with superimposed Fourier spectrum of model N (dashed line). Scales are as in Fig. 4.
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In the text

$\begin{figure} \par\includegraphics[height=8 cm, width=8.5 cm,clip]{7958f7} \end{figure}$ Figure 7: Fourier spectrum of the time flux variation of 3C 279 (solid line) with superimposed Fourier spectrum of model K (dashed line). In this case, the model whose simulated Fourier spectrum best fits the source is model K. Scales are as in Fig. 4.
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In the text

$\begin{figure} \par\includegraphics[width=8.5 cm,clip]{7958f8} \end{figure}$ Figure 8: The rotation periods of the disc inner edge, the outer edge and the annular rings where radial shocks occur in comparison with the outflow periods (as well as the radial shock periods) for five pairs of ( $\gamma$ , $\alpha$ ). Shaded bars refer to the rotation periods of the annular rings where periodical radial shocks form and degrade in their cyclical evolution. Both outflows and radial shocks can be single or double.
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In the text

$\begin{figure} \par\includegraphics[width=11.4cm,clip]{aa7958f2a.eps} \end{figure}$	Figure 2: Plots of the outflow rate d $n_{\rm jet}/{\rm d}t$ , the accretion rate d $n_{\rm acc}/{\rm d}t$ , and the number of particles in the disc $N_{\rm disk}$ versus time. Quantities in the plots are expressed in simulation units. At the top of each panel, the adopted ( $\lambda$ , $\alpha$ ) parameters and the model ID are also reported.
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$\begin{figure} \par\includegraphics[width=11.4cm,clip]{aa7958f2b.eps} \end{figure}$	Figure 2: continued.
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$\begin{figure} \par\includegraphics[height=8.cm, width=8cm]{7958f4} \end{figure}$	Figure 4: Fourier spectrum of the flux time variation of 0440-003 (solid line) with superimposed Fourier spectrum of model L (dashed line). L is the model whose simulated Fourier spectrum better fits the source power spectrum. Frequencies are expressed in Hz and power is normalized to its maximum.
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$\begin{figure} \par\includegraphics[height=8 cm, width=8.5 cm,clip]{7958f5} \end{figure}$	Figure 5: Fourier spectrum of the flux time variation of 1730-130 (solid line) with superimposed Fourier spectrum of model A (dashed line). Scales are as in Fig. 4.
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$\begin{figure} \par\includegraphics[height=8.5 cm, width=8.5 cm,clip]{7958f6} \end{figure}$	Figure 6: Fourier spectrum of the flux time variation of 1101+384 (solid line) with superimposed Fourier spectrum of model N (dashed line). Scales are as in Fig. 4.
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$\begin{figure} \par\includegraphics[height=8 cm, width=8.5 cm,clip]{7958f7} \end{figure}$	Figure 7: Fourier spectrum of the time flux variation of 3C 279 (solid line) with superimposed Fourier spectrum of model K (dashed line). In this case, the model whose simulated Fourier spectrum best fits the source is model K. Scales are as in Fig. 4.
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