$\begin{figure} \par\includegraphics[width=10cm,clip]{6979-01.ps} \end{figure}$ Figure 1: An example of the geometry of an accretion disk with a circular cross-section. Here, R₀ and a are the major radius of the geometric axis and the radius of the last closed flux surface, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{6979-02.ps} \end{figure}$ Figure 2: The two-dimensional pressure (gray-scale) and plasma beta $\beta = 2p/B^{2}$ (contours) profile for an accretion disk with constant density. The cross-section is circular and the inverse aspect ratio $\epsilon =0.1$ . The central object is to the left of the figure.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{6979-03a.ps}\includegraphics... ...=6cm,clip]{6979-03b.ps}\includegraphics[width=6cm,clip]{6979-03c.ps}\end{figure}$ Figure 3: a) Real, and b) imaginary parts of the sub-spectrum of the MHD continua as functions of the radial flux coordinate $s \equiv \sqrt {\psi }$ and c) represented in the complex plane for toroidal mode number n=-1 and poloidal mode numbers m=[-3,5]. The corresponding disk equilibrium shown in Fig. 2 has a constant density distribution.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{6979-04.ps} \end{figure}$ Figure 4: The growth rate of the most unstable continuum mode as a function of the value of gravitational potential on the magnetic axis $R_{{\rm M}}$ . The gravitational potential is scaled with respect to the Alfvén speed on the magnetic axis.
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In the text

$\begin{figure} \par\includegraphics[width=6.4cm,clip]{6979-06.ps} \end{figure}$ Figure 6: The pressure (gray-scale) and plasma beta $\beta = 2p/B^{2}$ (contours) distribution in a poloidal cross-section for an accretion disk with density $\rho \propto (1-0.4\psi )$ and an inverse aspect ratio $\epsilon =0.1$ .
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{6979-07a.ps}\includegraphics[width=6cm,clip]{6979-07b.ps}\end{figure}$ Figure 7: For the accretion disk equilibrium shown in Fig. 6, a) the real parts of the sub-spectrum of MHD continua as function of the radial flux coordinate $s \equiv \sqrt {\psi }$ and b) sub-spectrum of the MHD continua in the complex plane are shown for toroidal mode number n=-1 and poloidal mode numbers m=[-3,5]. For these mode numbers, no unstable or overstable modes are found.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{6979-08.ps} \end{figure}$ Figure 8: The pressure (gray-scale) and plasma beta $\beta = 2p/B^{2}$ (contours) for a thick accretion disk with density $\rho \propto (1-0.4\psi )$ and an inverse aspect ratio $\epsilon =0.5$ .
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In the text

$\begin{figure} \par\begin{tabular}{l} \includegraphics[height=0.2\textheight,cl... ...ludegraphics[height=0.2\textheight,clip]{6979-09c.ps} \end{tabular} \end{figure}$ Figure 9: For the thick disk equilibrium shown in Fig. 8, a) the real and b) imaginary parts of the sub-spectrum of the MHD continua as a function of the radial flux coordinate $s \equiv \sqrt {\psi }$ and c) sub-spectrum of the MHD continua in the complex plane are shown for toroidal mode number n=-1 and poloidal mode numbers m=[-3,5].
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{6979-10.ps} \end{figure}$ Figure 10: Growth rate of the most overstable continuum mode as a function of the inverse aspect ratio $\epsilon = a / R_{0}$ .
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In the text

$\begin{figure} \par\includegraphics[width=10cm,clip]{6979-01.ps} \end{figure}$	Figure 1: An example of the geometry of an accretion disk with a circular cross-section. Here, R₀ and a are the major radius of the geometric axis and the radius of the last closed flux surface, respectively.
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$\begin{figure} \par\includegraphics[width=6cm,clip]{6979-02.ps} \end{figure}$	Figure 2: The two-dimensional pressure (gray-scale) and plasma beta $\beta = 2p/B^{2}$ (contours) profile for an accretion disk with constant density. The cross-section is circular and the inverse aspect ratio $\epsilon =0.1$ . The central object is to the left of the figure.
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$\begin{figure} \par\includegraphics[width=6cm,clip]{6979-03a.ps}\includegraphics... ...=6cm,clip]{6979-03b.ps}\includegraphics[width=6cm,clip]{6979-03c.ps}\end{figure}$	Figure 3: a) Real, and b) imaginary parts of the sub-spectrum of the MHD continua as functions of the radial flux coordinate $s \equiv \sqrt {\psi }$ and c) represented in the complex plane for toroidal mode number n=-1 and poloidal mode numbers m=[-3,5]. The corresponding disk equilibrium shown in Fig. 2 has a constant density distribution.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{6979-04.ps} \end{figure}$	Figure 4: The growth rate of the most unstable continuum mode as a function of the value of gravitational potential on the magnetic axis $R_{{\rm M}}$ . The gravitational potential is scaled with respect to the Alfvén speed on the magnetic axis.
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$\begin{figure} \par\begin{tabular}{ll} \includegraphics[width=5.5cm,clip]{6979-... ... \includegraphics[width=5.5cm,clip]{6979-05c.ps} & \end{tabular} \end{figure}$	Figure 5: The Brunt-Väisälä frequency projected on a flux surface for the points a), b), and c) shown in Fig. 4 shown as a contour plot in a poloidal cross-section.
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$\begin{figure} \par\includegraphics[width=6.4cm,clip]{6979-06.ps} \end{figure}$	Figure 6: The pressure (gray-scale) and plasma beta $\beta = 2p/B^{2}$ (contours) distribution in a poloidal cross-section for an accretion disk with density $\rho \propto (1-0.4\psi )$ and an inverse aspect ratio $\epsilon =0.1$ .
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$\begin{figure} \par\includegraphics[width=6cm,clip]{6979-07a.ps}\includegraphics[width=6cm,clip]{6979-07b.ps}\end{figure}$	Figure 7: For the accretion disk equilibrium shown in Fig. 6, a) the real parts of the sub-spectrum of MHD continua as function of the radial flux coordinate $s \equiv \sqrt {\psi }$ and b) sub-spectrum of the MHD continua in the complex plane are shown for toroidal mode number n=-1 and poloidal mode numbers m=[-3,5]. For these mode numbers, no unstable or overstable modes are found.
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$\begin{figure} \par\includegraphics[width=6cm,clip]{6979-08.ps} \end{figure}$	Figure 8: The pressure (gray-scale) and plasma beta $\beta = 2p/B^{2}$ (contours) for a thick accretion disk with density $\rho \propto (1-0.4\psi )$ and an inverse aspect ratio $\epsilon =0.5$ .
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$\begin{figure} \par\begin{tabular}{l} \includegraphics[height=0.2\textheight,cl... ...ludegraphics[height=0.2\textheight,clip]{6979-09c.ps} \end{tabular} \end{figure}$	Figure 9: For the thick disk equilibrium shown in Fig. 8, a) the real and b) imaginary parts of the sub-spectrum of the MHD continua as a function of the radial flux coordinate $s \equiv \sqrt {\psi }$ and c) sub-spectrum of the MHD continua in the complex plane are shown for toroidal mode number n=-1 and poloidal mode numbers m=[-3,5].
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$\begin{figure} \par\includegraphics[width=9cm,clip]{6979-10.ps} \end{figure}$	Figure 10: Growth rate of the most overstable continuum mode as a function of the inverse aspect ratio $\epsilon = a / R_{0}$ .
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