Astronomy & Astrophysics

$\begin{figure} \par\epsfig{file=2591-02.eps, width=8cm} \end{figure}$ Figure 2: Complete MHD spectrum of a weakly magnetized thin disk for wavenumbers m=0 and k=200.
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In the text

$\begin{figure} \par\epsfig{file=2591-03.eps, width=8cm} \end{figure}$ Figure 3: The eigenfunction $\chi$ of the mode with the largest growth rate. The growth rate is $0.728\Omega$ .
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In the text

$\begin{figure} \par\begin{tabular}{cc} \epsfig{file=2591-04a.eps, width=7cm}\hspace*{2mm}& \epsfig{file=2591-04b.eps, width=7.2cm} \end{tabular} \end{figure}$ Figure 4: The growth rate and the oscillation frequency of the most unstable axisymmetric MRI mode as a function of the scaled Alfvén frequency for disk model A, where $\beta = 1000$ . In this purely axial magnetic field configuration, the axisymmetric modes are purely exponentially growing in time.
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In the text

$\begin{figure} \par\begin{tabular}{cc} \epsfig{file=2591-05a.eps, width=7cm}\hspace*{2mm}& \epsfig{file=2591-05b.eps, width=7.2cm} \end{tabular} \end{figure}$ Figure 5: The growth rate and the oscillation frequency of the most unstable axisymmetric MRI mode as a function of the scaled Alfvén frequency for disk model B, where $\beta = 500$ .
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In the text

$\begin{figure} \par\begin{tabular}{cc} \epsfig{file=2591-06a.eps, width=7.2cm} & \epsfig{file=2591-06b.eps, width=7.4cm} \end{tabular} \end{figure}$ Figure 6: The growth rate and the oscillation frequency of the most unstable axisymmetric MRI mode as a function of the scaled Alfvén frequency for disk model C, where $\beta = 9.901$ .
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In the text

$\begin{figure} \par\begin{tabular}{cc} \epsfig{file=2591-07a.eps, width=7.2cm} & \epsfig{file=2591-07b.eps, width=7.4cm} \end{tabular} \end{figure}$ Figure 7: The growth rate and the oscillation frequency of the most unstable axisymmetric MRI mode for a disk close to equipartition with a dominant toroidal magnetic field component (disk model D).
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In the text

$\begin{figure} \par\epsfig{file=2591-11.eps, width=7cm,clip} \end{figure}$ Figure A.1: The radial "wavenumber'' q of the eigenfunction $\chi$ shown in Fig. 3. The growth rate is $0.728\Omega$ .

In the text

$\begin{figure} \par\begin{picture} (0,0)(95,15) \includegraphics{2591-01.ps}\en... ...{\mddefault}{\updefault}{$\Omega_{{\rm A}}^{-}$ }}}}} \end{picture} \end{figure}$	Figure 1: Continuous parts of the MHD spectrum for a weakly inhomogeneous equilibrium.
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$\begin{figure} \par\epsfig{file=2591-02.eps, width=8cm} \end{figure}$	Figure 2: Complete MHD spectrum of a weakly magnetized thin disk for wavenumbers m=0 and k=200.
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$\begin{figure} \par\epsfig{file=2591-03.eps, width=8cm} \end{figure}$	Figure 3: The eigenfunction $\chi$ of the mode with the largest growth rate. The growth rate is $0.728\Omega$ .
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$\begin{figure} \par\begin{tabular}{cc} \epsfig{file=2591-04a.eps, width=7cm}\hspace*{2mm}& \epsfig{file=2591-04b.eps, width=7.2cm} \end{tabular} \end{figure}$	Figure 4: The growth rate and the oscillation frequency of the most unstable axisymmetric MRI mode as a function of the scaled Alfvén frequency for disk model A, where $\beta = 1000$ . In this purely axial magnetic field configuration, the axisymmetric modes are purely exponentially growing in time.
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$\begin{figure} \par\begin{tabular}{cc} \epsfig{file=2591-05a.eps, width=7cm}\hspace*{2mm}& \epsfig{file=2591-05b.eps, width=7.2cm} \end{tabular} \end{figure}$	Figure 5: The growth rate and the oscillation frequency of the most unstable axisymmetric MRI mode as a function of the scaled Alfvén frequency for disk model B, where $\beta = 500$ .
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$\begin{figure} \par\begin{tabular}{cc} \epsfig{file=2591-06a.eps, width=7.2cm} & \epsfig{file=2591-06b.eps, width=7.4cm} \end{tabular} \end{figure}$	Figure 6: The growth rate and the oscillation frequency of the most unstable axisymmetric MRI mode as a function of the scaled Alfvén frequency for disk model C, where $\beta = 9.901$ .
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$\begin{figure} \par\begin{tabular}{cc} \epsfig{file=2591-07a.eps, width=7.2cm} & \epsfig{file=2591-07b.eps, width=7.4cm} \end{tabular} \end{figure}$	Figure 7: The growth rate and the oscillation frequency of the most unstable axisymmetric MRI mode for a disk close to equipartition with a dominant toroidal magnetic field component (disk model D).
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$\begin{figure} \par\begin{tabular}{cc} \epsfig{file=2591-08a.eps, width=7.2cm} & \epsfig{file=2591-08b.eps, width=7.4cm} \end{tabular} \end{figure}$	Figure 8: The growth rate and the oscillation frequency of the most unstable mode for disk model E, where the disk rotation is Keplerian.
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$\begin{figure} \par\begin{tabular}{cc} \epsfig{file=2591-09a.eps, width=7.2cm} & \epsfig{file=2591-09b.eps, width=7.4cm} \end{tabular} \end{figure}$	Figure 9: The growth rate and the oscillation frequency of the most unstable mode for disk model F, where the disk rotation is weaklysub-Keplerian.
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$\begin{figure} \par\begin{tabular}{cc} \epsfig{file=2591-10a.eps, width=7.2cm} & \epsfig{file=2591-10b.eps, width=7.4cm} \end{tabular} \end{figure}$	Figure 10: The growth rate and the oscillation frequency of the most unstable mode for disk model G, where the disk rotation is strongsub-Keplerian.
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